Silicon-Germanium Voltage-Controlled Oscillator at 105 GHz

NASA Technical Reports Server (NTRS)

Wong, Alden; Larocca, Tim; Chang, M. Frank; Samoska, Lorene A.

2011-01-01

A group at UCLA, in collaboration with the Jet Propulsion Laboratory, has designed a voltage-controlled oscillator (VCO) created specifically for a compact, integrated, electronically tunable frequency generator useable for submillimeter- wave science instruments operating in extreme cold environments.

78 FR 42587 - Deepwater Port License: Amendment of the Neptune LNG LLC Deepwater Port License and Temporary...

Federal Register 2010, 2011, 2012, 2013, 2014

2013-07-16

... Neptune LNG LLC Deepwater Port License and Temporary Suspension of Operations at the Neptune LNG Deepwater... decision to approve the request of Neptune LNG LLC (Neptune) for a temporary five-year suspension of port operations at the Neptune Deepwater Port by amending the Neptune Deepwater Port License. ADDRESSES: The...

UCLA High Speed, High Volume Laboratory Network for Infectious Diseases. Addendum

DTIC Science & Technology

2009-08-01

s) and should not be construed as an official Department of the Army position, policy or decision unless so designated by other documentation... Design : Because of current public health and national security threats, influenza surveillance and analysis will be the initial focus. In the upcoming...throughput and automated systems will enable processing of tens of thousands of samples and provide critical laboratory capacity. Its overall design and

Hubble Finds New Dark Spot on Neptune

NASA Technical Reports Server (NTRS)

1995-01-01

NASA's Hubble Space Telescope has discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet's northern hemisphere is now tilted away from Earth, the new feature appears near the limb of the planet.

The spot is a near mirror-image to a similar southern hemisphere dark spot that was discovered in 1989 by the Voyager 2 probe. In 1994, Hubble showed that the southern dark spot had disappeared.

Like its predecessor, the new spot has high altitude clouds along its edge, caused by gasses that have been pushed to higher altitudes where they cool to form methane ice crystal clouds. The dark spot may be a zone of clear gas that is a window to a cloud deck lower in the atmosphere.

Planetary scientists don t know how long lived this new feature might be. Hubble's high resolution will allow astronomers to follow the spot's evolution and other unexpected changes in Neptune's dynamic atmosphere.

The image was taken on November 2, 1994 with Hubble's Wide Field Planetary Camera 2, when Neptune was 2.8 billion miles (4.5 billion kilometers) from Earth. Hubble can resolve features as small as 625 miles (1,000 kilometers) across in Neptune's cloud tops.

The Wide Field/Planetary Camera 2 was developed by the Jet Propulsion Laboratory and managed by the Goddard Spaced Flight Center for NASA's Office of Space Science.

This image and other images and data received from the Hubble Space Telescope are posted on the World Wide Web on the Space Telescope Science Institute home page at URL http://oposite.stsci.edu/pubinfo/

Self-instructional "virtual pathology" laboratories using web-based technology enhance medical school teaching of pathology.

PubMed

Marchevsky, Alberto M; Relan, Anju; Baillie, Susan

2003-05-01

Second-year medical students have traditionally been taught pulmonary pathophysiology at the University of California-Los Angeles (UCLA) School of Medicine using lectures, discussion groups, and laboratory sessions. Since 1998, the laboratory sessions have been replaced by 4 interactive, self-instructional sessions using web-based technology and case-based instruction. This article addresses nature of transformation that occurred from within the course in response to the infusion of new technologies. The vast majority of the course content has been digitized and incorporated into the website of the Pathophysiology of Disease course. The teaching histological slides have been photographed digitally and organized into "cases" with clinical information, digital images and text, and audio descriptions. The students study the materials from these cases at their own pace in 2 "virtual pathology" laboratory, with a few instructors supervising the on-site sessions. The students discuss additional cases available on the website in 2 other laboratory sessions supervised by a pulmonologist and a pathologist. Marked improvement in student participation and satisfaction was seen with the use of web-based instruction. Attendance at laboratory sessions, where the students had previously been required to bring their own microscopes to study histological slides at their own pace, increased from approximately 30% to 40% of the class in previous years to almost 100%. Satisfaction surveys showed progressive improvement over the past 4 years, as various suggestions were implemented. The value of web-based instruction of pathology at the UCLA School of Medicine is discussed.

CONTRIBUTIONS OF 20TH CENTURY WOMEN TO PHYSICS

Science.gov Websites

Annotated Photo Gallery In Her Own Words Some Physics History 500+ Books and Articles Field Editors Physical Society, the University of California, UCLA Physics and Astronomy Department, the Laboratories of Astrophysics Burbidge, E. M. Burnell, Jocelyn Faber, Sandra Leavitt, Henrietta Payne-Gaposchkin,Cecilia Rubin

Instructional Objectives for a Junior College Course in Introduction to Mathematical Thinking.

ERIC Educational Resources Information Center

Starkweather, Ann, Comp.

These instructional objectives have been selected from materials submitted to the Curriculum Laboratory of the Graduate School of Education at UCLA. Arranged by major course goals, these objectives are offered simply as samples that may be used where they correspond to the skills, abilities, and attitudes instructors want their students to…

Instructional Objectives for a Junior College Course in College Mathematics.

ERIC Educational Resources Information Center

Starkweather, Ann, Comp.

These instructional objectives have been selected from materials submitted to the Curriculum Laboratory of the Graduate School of Education at UCLA. Arranged by major course goals, these objectives are offered simply as samples that may be used where they correspond to the skills, abilities, and attitudes instructors want their students to…

Instructional Objectives for a Junior College Course in Intermediate Algebra.

ERIC Educational Resources Information Center

Starkweather, Ann, Comp.

These instructional objectives have been selected from materials submitted to the Curriculum Laboratory of the Graduate School of Education at UCLA. Arranged by major course goals, these objectives are offered simply as samples that may be used where they correspond to the skills, abilities, and attitudes instructors want their students to…

Strategies for Using Peer-Assisted Learning Effectively in an Undergraduate Bioinformatics Course

ERIC Educational Resources Information Center

Shapiro, Casey; Ayon, Carlos; Moberg-Parker, Jordan; Levis-Fitzgerald, Marc; Sanders, Erin R.

2013-01-01

This study used a mixed methods approach to evaluate hybrid peer-assisted learning approaches incorporated into a bioinformatics tutorial for a genome annotation research project. Quantitative and qualitative data were collected from undergraduates who enrolled in a research-based laboratory course during two different academic terms at UCLA.…

The Parkes front-end controller and noise-adding radiometer

NASA Technical Reports Server (NTRS)

Brunzie, T. J.

1990-01-01

A new front-end controller (FEC) was installed on the 64-m antenna in Parkes, Australia, to support the 1989 Voyager 2 Neptune encounter. The FEC was added to automate operation of the front-end microwave hardware as part of the Deep Space Network's Parkes-Canberra Telemetry Array. Much of the front-end hardware was refurbished and reimplemented from a front-end system installed in 1985 by the European Space Agency for the Uranus encounter; however, the FEC and its associated noise-adding radiometer (NAR) were new Jet Propulsion Laboratory (JPL) designs. Project requirements and other factors led to the development of capabilities not found in standard Deep Space Network (DSN) controllers and radiometers. The Parkes FEC/NAR performed satisfactorily throughout the Neptune encounter and was removed in October 1989.

Detection of C2H4 Neptune from ISO/PHT-S Observations

NASA Technical Reports Server (NTRS)

Schulz, B.; Encrenaz, Th.; Bezard, B.; Romani, P. N.; Lellouch, E.; Atreya, S. K.

1999-01-01

The 6-12 micrometer spectrum of Neptune has been recorded with the PHT-S instrument of the Infrared Space Observatory (ISO) at a resolution of 0.095 micrometer. In addition to the emissions of CH4, CH3D and C2H6 previously identified, the spectrum shows the first firm identification of ethylene C2H4. The inferred column density above the 0.2-mbar level is in the range (1.1 - 3) x 10(exp 14) molecules/cm. To produce this low amount, previous photochemical models invoked rapid mixing between the source and sink regions of C2H4. We show that this requirement can be relaxed if recent laboratory measurements of CH4 photolysis branching ratios at Lyman alpha are used.

University of California, Los Angeles Campus School of Medicine Atomic Energy Project quarterly progress report for period ending March 31, 1952

DOE Office of Scientific and Technical Information (OSTI.GOV)

Warren, S.L.

1952-04-10

The fifteenth quarterly report being submitted for Contract No. AT04-1-GEN-12 is issued in accordance with Service Request Number 1 except for the report of the Alamogordo Section, Code 91810, which is submitted in accordance with the provisions of Service Request Number 2. Work is in progress on continuing existing projects. In addition, new projects have been initiated including the Kinetics and Mechanism of Protein Denaturation (10018); The Effect of Irradiation on the Constituents of Embryonic Serum (30033); and The Use of Controlled Atmospheres for Spectrographic Excitation Sources (40053). Many of the Project units are either wholly or partially completed andmore » the following initial reports are available: Identification of Ferritin in Blood of Dogs Subjected to Radiation from an Atomic Detonation (UCLA-180); The Nutritional Value of Intravenous Tapioca Dextrin in Normal and Irradiated Rabbits (UCLA-181); The-Decarboxylation and Reconstitution of Linoleic Acid (UCLA-183); Preparation and Properties of Thymus Nucleic Acid (UCLA-184); The Radiation Chemistry of Cysteine Solutions Part II. (a) The Action of Sulfite on the Irradiated Solutions; (b) The Effect on Cystine (UCLA-185); A Revolving Specimen Stage for the Electron Microscope (UCLA-178); An Automatic Geiger-Mueller Tube Tester (UCLA-186); The Value of Gamma Radiation Dosimetry in Atomic Warfare Including a Discussion of Practical Dosage Ranges (UCLA-187); and A New Plastic Tape Film Badge Holder (UCLA-189). Two additional reports were issued; one by Dr. Wilbur Selle entitled Attempts to Alter the Response to Ionizing Radiations from the School of Medicine, UCLA (UCLA-176), and two, a restricted distribution report from the Alamogordo Section entitled Field Observations and Preliminary Field Data Obtained by the UCLA Survey Group on Operation Jangle, November 1951 (UCLA-182).« less

Neptune's Eccentricity and the Nature of the Kuiper Belt

NASA Technical Reports Server (NTRS)

Ward, William R.; Hahn, Joseph M.

1998-01-01

The small eccentricity of Neptune may be a direct consequence of apsidal wave interaction with the trans-Neptune population of debris called the Kuiper belt. The Kuiper belt is subject to resonant perturbations from Neptune, so that the transport of angular momentum by density waves can result in orbital evolution of Neptune as well as changes in the structure of the Kuiper belt. In particular, for a belt eroded out to the vicinity of Neptune's 2:1 resonance at about 48 astronomical units, Neptune's eccentricity can damp to its current value over the age of the solar system if the belt contains slightly more than an earth mass of material out to about 75 astronomical units.

Voyager: Neptune Encounter Highlights

NASA Technical Reports Server (NTRS)

1989-01-01

Voyager encounter data are presented in computer animation (CA) and real (R) animation. The highlights include a view of 2 full rotations of Neptune. It shows spacecraft trajectory 'diving' over Neptune and intercepting Triton's orbit, depicting radiation and occulation zones. Also shown are a renegade orbit of Triton and Voyager's encounter with Neptune's Magnetopause. A model of the spacecraft's complex maneuvers during close encounters of Neptune and Triton is presented. A view from Earth of Neptune's occulation experiment is is shown as well as a recreation of Voyager's final pass. There is detail of Voyager's Image Compensation technique which produces Voyager images. Eighteen images were produced on June 22 - 23, 1989, from 57 million miles away. A 68 day sequence which provides a stroboscopic view - colorization approximates what is seen by the human eye. Real time images recorded live from Voyager on 8/24/89 are presented. Photoclinometry produced the topography of Triton. Three images are used to create a sequence of Neptune's rings. The globe of Neptune and 2 views of the south pole are shown as well as Neptune rotating. The rotation of a scooter is frozen in images showing differential motion. There is a view of rotation of the Great Dark Spot about its own axis. Photoclinometry provides a 3-dimensional perspective using a color mosaic of Triton images. The globe is used to indicate the orientation of Neptune's crescent. The east and west plumes on Triton are shown.

Neptune encounter highlights

NASA Astrophysics Data System (ADS)

1989-11-01

Voyager encounter data are presented in computer animation (CA) and real (R) animation. The highlights include a view of 2 full rotations of Neptune. It shows spacecraft trajectory 'diving' over Neptune and intercepting Triton's orbit, depicting radiation and occulation zones. Also shown are a renegade orbit of Triton and Voyager's encounter with Neptune's Magnetopause. A model of the spacecraft's complex maneuvers during close encounters of Neptune and Triton is presented. A view from Earth of Neptune's occulation experiment is is shown as well as a recreation of Voyager's final pass. There is detail of Voyager's Image Compensation technique which produces Voyager images. Eighteen images were produced on June 22 - 23, 1989, from 57 million miles away. A 68 day sequence which provides a stroboscopic view - colorization approximates what is seen by the human eye. Real time images recorded live from Voyager on 8/24/89 are presented. Photoclinometry produced the topography of Triton. Three images are used to create a sequence of Neptune's rings. The globe of Neptune and 2 views of the south pole are shown as well as Neptune rotating. The rotation of a scooter is frozen in images showing differential motion. There is a view of rotation of the Great Dark Spot about its own axis. Photoclinometry provides a 3-dimensional perspective using a color mosaic of Triton images. The globe is used to indicate the orientation of Neptune's crescent. The east and west plumes on Triton are shown.

Generation of Shear Alfvén Waves by Repetitive High Power Microwave Pulses Near the Electron Plasma Frequency - A laboratory study of a ``Virtual Antenna''

NASA Astrophysics Data System (ADS)

Wang, Yuhou; Gekelman, Walter; Pribyl, Patrick; van Compernolle, Bart; Papadopoulos, Konstantinos

2015-11-01

ELF / ULF waves are important in terrestrial radio communications but difficult to launch using ground-based structures due to their enormous wavelengths. In spite of this generation of such waves by field-aligned ionospheric heating modulation was first demonstrated using the HAARP facility. In the future heaters near the equator will be constructed and laboratory experiments on cross-field wave propagation could be key to the program's success. Here we report a detailed laboratory study conducted on the Large Plasma Device (LaPD) at UCLA. In this experiment, ten rapid pulses of high power microwaves (250 kW X-band) near the plasma frequency were launched transverse to the background field, and were modulated at a variable fraction (0.1-1.0) of fci. Along with bulk electron heating and density modification, the microwave pulses generated a population of fast electrons. The field-aligned current carried by the fast electrons acted as an antenna that radiated shear Alfvén waves. It was demonstrated that a controllable arbitrary frequency (f

A New Model for a Multi-Disciplinary Engineering Summer Research Program for High School Seniors: Program Overview, Effectiveness, and Outcomes

ERIC Educational Resources Information Center

Kittur, H.; Shaw, L.; Herrera, W.

2017-01-01

The High School Summer Research Program (HSSRP) is a rigorous eight-week research experience that challenges high school students to a novel scientific question in an engineering laboratory at the Henry Samueli School of Engineering and Applied Science (HSSEAS) at the University of California, Los Angeles (UCLA). The program collates highly…

Recent progress in Precambrian paleobiology

NASA Technical Reports Server (NTRS)

Schopf, J. W.

1986-01-01

Ongoing studies at UCLA include the following: (1) investigations in Archean and Proterozoic sequences of various locations; (2) laboratory and field studies of modern microbial biocoenoses (analogues of Precambrian microbial communities) especially those at Laguna Mormona, Baja California, Mexico; (3) development of new laboratory techniques for the separation and concentration of minute cellularly preserved fossils for isotopic and organic geochemical analyses; and (4) assembly of a computerized database for assessment of the timing and nature of major events occurring during Precambrian biotic evolution, and of the potential applicability of ancient microbiotas to problems of global biostratigraphy and biogeography.

77 FR 39507 - Notice of Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2012-07-03

... Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA AGENCY: National Park Service, Interior. ACTION: Notice. SUMMARY: The Fowler Museum at UCLA has completed an inventory of human remains and associated... human remains and associated funerary objects may contact the Fowler Museum at UCLA. Repatriation of the...

76 FR 48176 - Notice of Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2011-08-08

... A detailed assessment of the human remains was made by the Fowler Museum at UCLA professional staff... Museum at UCLA, Los Angeles, CA AGENCY: National Park Service, Interior. ACTION: Notice. SUMMARY: The Fowler Museum at UCLA has completed an inventory of human remains, in consultation with the appropriate...

76 FR 35995 - Taking and Importing Marine Mammals; Taking Marine Mammals Incidental to Operation and...

Federal Register 2010, 2011, 2012, 2013, 2014

2011-06-21

... of the Neptune Liquefied Natural Gas Facility of Massachusetts; Correction AGENCY: National Marine... rule; correction. SUMMARY: NMFS, upon application from Neptune LNG LLC (Neptune), issued regulations... activities, at the Neptune Deepwater Port (the Port) in Massachusetts Bay for a period of 5 years. The final...

UCLA's Institute for Planets and Exoplanets: Structuring an Education and Public Outreach Program from the Ground Up

NASA Astrophysics Data System (ADS)

Curren, I. S.; Jewitt, D. C.

2014-12-01

Geoscience education and public outreach efforts (EPO), both formal and informal, are critical to increasing science literacy amongst members of the public and securing the next generation of geoscientists. At UCLA, the Institute for Planets and Exoplanets (iPLEX) has developed a multifaceted program to administer meaningful and original hands-on education and outreach to the public, teachers/professors, and students. To build the program, we first developed a virtual "home base" using Wordpress. With the needs of our community in mind, we structured the website to serve three categories of individuals: the public, teachers/professors, and volunteers. To serve the public, we have developed a series of informal education events (e.g., Exploring Your Universe) that bring thousands of science enthusiasts to campus. For those unable to participate in hands-on demonstrations or for those who would like to see them again, informational videos were developed and made available on our online Physical Demonstrations Digital Library (PDDL). The PDDL contains a second set of videos that are tutorial in nature and specifically designed with teachers, TAs and professors in mind. In addition, we have produced a publicly available annual newsletter written at the level of the informed public that details exciting and current planetary research at UCLA. Another facet of the program, designed with teachers in mind is our application-based private outreach event system in which teachers may choose to have volunteers come to their school with interactive demos or to come to UCLA to speak with scientists and tour laboratories. The final branch of the iPLEX EPO and education program caters to volunteers and includes an online "hub" where volunteers can register for events, download demonstration information packets, and discuss tips with other volunteers. We have recently developed a "Science Education, Outreach, and Communication" course to be integrated into UCLA's undergraduate geology curriculum that will serve twofold to train new volunteers and educate young scientists on how to communicate their field to the public. Feedback from participants indicates an overall increase in geoscience EPO participation and satisfaction from the public, teachers, and volunteers alike since iPLEX's program was emplaced.

NEPTUNE'S WILD DAYS: CONSTRAINTS FROM THE ECCENTRICITY DISTRIBUTION OF THE CLASSICAL KUIPER BELT

DOE Office of Scientific and Technical Information (OSTI.GOV)

Dawson, Rebekah I.; Murray-Clay, Ruth, E-mail: rdawson@cfa.harvard.edu

2012-05-01

Neptune's dynamical history shaped the current orbits of Kuiper Belt objects (KBOs), leaving clues to the planet's orbital evolution. In the 'classical' region, a population of dynamically 'hot' high-inclination KBOs overlies a flat 'cold' population with distinct physical properties. Simulations of qualitatively different histories for Neptune, including smooth migration on a circular orbit or scattering by other planets to a high eccentricity, have not simultaneously produced both populations. We explore a general Kuiper Belt assembly model that forms hot classical KBOs interior to Neptune and delivers them to the classical region, where the cold population forms in situ. First, wemore » present evidence that the cold population is confined to eccentricities well below the limit dictated by long-term survival. Therefore, Neptune must deliver hot KBOs into the long-term survival region without excessively exciting the eccentricities of the cold population. Imposing this constraint, we explore the parameter space of Neptune's eccentricity and eccentricity damping, migration, and apsidal precession. We rule out much of parameter space, except where Neptune is scattered to a moderately eccentric orbit (e > 0.15) and subsequently migrates a distance {Delta}a{sub N} = 1-6 AU. Neptune's moderate eccentricity must either damp quickly or be accompanied by fast apsidal precession. We find that Neptune's high eccentricity alone does not generate a chaotic sea in the classical region. Chaos can result from Neptune's interactions with Uranus, exciting the cold KBOs and placing additional constraints. Finally, we discuss how to interpret our constraints in the context of the full, complex dynamical history of the solar system.« less

Neptune aerocapture mission and spacecraft design overview

NASA Technical Reports Server (NTRS)

Bailey, Robert W.; Hall, Jeff L.; Spliker, Tom R.; O'Kongo, Nora

2004-01-01

A detailed Neptune aerocapture systems analysis and spacecraft design study was performed as part of NASA's In-Space Propulsion Program. The primary objectives were to assess the feasibility of a spacecraft point design for a Neptune/Triton science mission. That uses aerocapture as the Neptune orbit insertion mechanism. This paper provides an overview of the science, mission and spacecraft design resulting from that study.

Voyager at Neptune: 1989

NASA Technical Reports Server (NTRS)

1989-01-01

The Voyager mission has taken advantage of a rare planetary alignment that occurs at intervals of about 175 years and affords an extraordinary opportunity: a grand tour by a single spacecraft of the outer planets Jupiter, Saturn, Uranus, and Neptune. Voyager 2 will fly past Nepture and its large moon Triton on August 24, 1989. The discovery of Neptune, along with its current history is discussed. The imaging challenges, tracking and data acquisition, and the Voyager spacecraft are explained. Data will be gathered on the ring arcs of Neptune, the atmosphere and surface of Neptune, Triton, and Nereid (the smaller moon).

The Voyager encounter with Neptune

NASA Technical Reports Server (NTRS)

Stone, E. C.; Miner, E. D.

1991-01-01

The investigations carried out by the Voyager Neptune/Interstellar Mission are discussed. Attention is given to the location of the various science instruments and the spacecraft subsystems on the Voyager spacecraft and to the charactgeristics of eleven instruments used in the Voyager mission. The Voyager 1 and 2 trajectories from the launch through the Voyager-2 Neptune encounter are presented together with data for the Neptune encounter events.

1981N1 - A Neptune arc?

NASA Technical Reports Server (NTRS)

Hubbard, W. B.

1986-01-01

An object in the vicinity of Neptune detected in 1981 by simultaneous stellar occultation measurements at observatories near Tucson, Arizona, was interpreted as a new Neptune satellite. A reinterpretation suggests that it may have instead been a Neptune arc similar to one observed in 1984. The 1981 object, however, did not occult the star during simultaneous observations at Flagstaff, Arizona. This result constrains possible arc geometries.

COMPOSITIONAL DIVERSITY IN THE ATMOSPHERES OF HOT NEPTUNES, WITH APPLICATION TO GJ 436b

DOE Office of Scientific and Technical Information (OSTI.GOV)

Moses, J. I.; Line, M. R.; Visscher, C.

2013-11-01

Neptune-sized extrasolar planets that orbit relatively close to their host stars—often called {sup h}ot Neptunes{sup —}are common within the known population of exoplanets and planetary candidates. Similar to our own Uranus and Neptune, inefficient accretion of nebular gas is expected produce hot Neptunes whose masses are dominated by elements heavier than hydrogen and helium. At high atmospheric metallicities of 10-10,000 times solar, hot Neptunes will exhibit an interesting continuum of atmospheric compositions, ranging from more Neptune-like, H{sub 2}-dominated atmospheres to more Venus-like, CO{sub 2}-dominated atmospheres. We explore the predicted equilibrium and disequilibrium chemistry of generic hot Neptunes and find thatmore » the atmospheric composition varies strongly as a function of temperature and bulk atmospheric properties such as metallicity and the C/O ratio. Relatively exotic H{sub 2}O, CO, CO{sub 2}, and even O{sub 2}-dominated atmospheres are possible for hot Neptunes. We apply our models to the case of GJ 436b, where we find that a CO-rich, CH{sub 4}-poor atmosphere can be a natural consequence of a very high atmospheric metallicity. From comparisons of our results with Spitzer eclipse data for GJ 436b, we conclude that although the spectral fit from the high-metallicity forward models is not quite as good as the best fit obtained from pure retrieval methods, the atmospheric composition predicted by these forward models is more physically and chemically plausible in terms of the relative abundance of major constituents. High-metallicity atmospheres (orders of magnitude in excess of solar) should therefore be considered as a possibility for GJ 436b and other hot Neptunes.« less

Neptune in Primary Colors

NASA Image and Video Library

1998-08-02

These two NASA Hubble Space Telescope images provide views of weather on opposite hemispheres of Neptune. Taken Aug. 13, 1996; these composite images blend information from different wavelengths to bring out features of Neptune blustery weather.

Structural Design for a Neptune Aerocapture Mission

NASA Technical Reports Server (NTRS)

Dyke, R. Eric; Hrinda, Glenn A.

2004-01-01

A multi-center study was conducted in 2003 to assess the feasibility of and technology requirements for using aerocapture to insert a scientific platform into orbit around Neptune. The aerocapture technique offers a potential method of greatly reducing orbiter mass and thus total spacecraft launch mass by minimizing the required propulsion system mass. This study involved the collaborative efforts of personnel from Langley Research Center (LaRC), Johnson Space Flight Center (JSFC), Marshall Space Flight Center (MSFC), Ames Research Center (ARC), and the Jet Propulsion Laboratory (JPL). One aspect of this effort was the structural design of the full spacecraft configuration, including the ellipsled aerocapture orbiter and the in-space solar electric propulsion (SEP) module/cruise stage. This paper will discuss the functional and structural requirements for each of these components, some of the design trades leading to the final configuration, the loading environments, and the analysis methods used to ensure structural integrity. It will also highlight the design and structural challenges faced while trying to integrate all the mission requirements. Component sizes, materials, construction methods and analytical results, including masses and natural frequencies, will be presented, showing the feasibility of the resulting design for use in a Neptune aerocapture mission. Lastly, results of a post-study structural mass optimization effort on the ellipsled will be discussed, showing potential mass savings and their influence on structural strength and stiffness

The Formation of Mini-Neptunes

NASA Astrophysics Data System (ADS)

Venturini, Julia; Helled, Ravit

2017-10-01

Mini-Neptunes seem to be common planets. In this work we investigate the possible formation histories and predicted occurrence rates of mini-Neptunes, assuming that the planets form beyond the iceline. We consider pebble and planetesimal accretion accounting for envelope enrichment and two different opacity conditions. We find that the formation of mini-Neptunes is a relatively frequent output when envelope enrichment by volatiles is included, and that there is a “sweet spot” for mini-Neptune formation with a relatively low solid accretion rate of ˜10-6 M ⊕ yr-1. This rate is typical for low/intermediate-mass protoplanetary disks and/or disks with low metallicities. With pebble accretion, envelope enrichment and high opacity favor the formation of mini-Neptunes, with more efficient formation at large semimajor axes (˜30 au) and low disk viscosities. For planetesimal accretion, such planets can also form without enrichment, with the opacity being a key aspect in the growth history and favorable formation location. Finally, we show that the formation of Neptune-like planets remains a challenge for planet formation theories.

The origin of carbon monoxide in Neptunes's atmosphere

NASA Technical Reports Server (NTRS)

Lodders, K.; Fegley, B., Jr.

1994-01-01

The CO abundance in the observable atmosphere of Neptune can be plausibly explained by rapid vertical mixing from the deeper atmosphere if Neptune has a greater complement of water than Uranus. Thermochemical equilibrium and kinetic calculations reveal that Neptune must and Uranus may have about 10 times more oxygen than carbon, whereas for Jupiter and Saturn equal enrichments of carbon and oxygen are satifactory to explain the observed CO abundances by deep vertical mixing. Relative to hydrogen and solar composition, the respective enrichment factors for carbon and oxygen are 41, 440 (Neptune); 32, less than or equal 260 (Uranus); 6.6, 6.6 (Saturn); and 2.8, 2.8 (Jupiter). Because water ice is the most refractory ice among the ices assumed to be present in the outer solar nebula, the most massive H2O enrichment is expected for the outermost planet of this group. Thus, Neptune can indeed be regarded as the 'god of the seas.'

Relativistic electron diffraction at the UCLA Pegasus photoinjector laboratory.

PubMed

Musumeci, P; Moody, J T; Scoby, C M

2008-10-01

Electron diffraction holds the promise to yield real-time resolution of atomic motion in an easily accessible environment like a university laboratory at a fraction of the cost of fourth-generation X-ray sources. Currently the limit in time-resolution for conventional electron diffraction is set by how short an electron pulse can be made. A very promising solution to maintain the highest possible beam intensity without excessive pulse broadening from space charge effects is to increase the electron energy to the MeV level where relativistic effects significantly reduce the space charge forces. Rf photoinjectors can in principle deliver up to 10(7)-10(8) electrons packed in bunches of approximately 100-fs length, allowing an unprecedented time resolution and enabling the study of irreversible phenomena by single-shot diffraction patterns. The use of rf photoinjectors as sources for ultrafast electron diffraction has been recently at the center of various theoretical and experimental studies. The UCLA Pegasus laboratory, commissioned in early 2007 as an advanced photoinjector facility, is the only operating system in the country, which has recently demonstrated electron diffraction using a relativistic beam from an rf photoinjector. Due to the use of a state-of-the-art ultrashort photoinjector driver laser system, the beam has been measured to be sub-100-fs long, at least a factor of 5 better than what measured in previous relativistic electron diffraction setups. Moreover, diffraction patterns from various metal targets (titanium and aluminum) have been obtained using the Pegasus beam. One of the main laboratory goals in the near future is to fully develop the rf photoinjector-based ultrafast electron diffraction technique with particular attention to the optimization of the working point of the photoinjector in a low-charge ultrashort pulse regime, and to the development of suitable beam diagnostics.

Hubble View of Neptune

NASA Image and Video Library

1998-08-02

These NASA Hubble Space Telescope views of the blue-green planet Neptune provide three snapshots of changing weather conditions. The images were taken in 1994 on 3 separate days when Neptune was 2.8 billion miles 4.5 billion kilometers from Earth.

Development of a petrochronology laboratory in Russia

NASA Astrophysics Data System (ADS)

Yavryan, M.; Powerman, V.; Nourgaliev, D. K.

2017-12-01

Each year more and more U-Pb detrital zircon studies are coming from Russia. However, the latest developments in zircon studies, namely combining U-Pb age with the measurements of REE concentrations and Lu-Hf isotopy on the same grain, have been unavailable in Russia. Kazan Federal U. has undertaken certain efforts in order to develop Russia's first petrochronology laboratory. The following equipment was recently purchased, installed and put into operation: Neptune Plus HR MC ICPMS, with jet-interface and RPQ filter. iCAP-Qc quadruple ICPMS. 2 x NWR213 laser ablation systems; one of them equipped with the TwoVol2 ablation chamber. Helium gas is used to flush the ablation chamber; 5 ml/min. of nitrogen is mixed downstream before plasma in order to increase the signal. The following methods have been set up at KFU on the Neptune Plus ICPMS: (1) U-Pb geochronology on zircons. A set of standards have been dated (R33, 91500, Plesovice, Mudtank, GJ-1, AS-3); (2) U-Pb geochronology on perovskites. We have collected, separated and analyzed Baikal Tazheran 463 Ma perovskite, previously dated on TIMS (e.g., Ireland et al., 1990; Li et al., 2010), using 91500 zircon as a primary standard. We intend to start using Tazheran perovskite as an in-house standard for dating perovskites. (3) Lu-Hf isotopy on a set of standard zircons. All results will be presented during the poster session. Our next steps will include setting the (a) U-Pb geochronology and (b) REE measurements on the quadruple MS; (c) splitting the ablation stream into two and directing them to Neptune for Lu-Hf measurements and to iCAP for either U-Pb, or REE, or both types of measurements; (d) experimenting with pre-ablation in order to diminish common lead, with (e) rastering during ablation to diminish downhole fractionation, with (f) squid signal smoothing device.

The Revised Pole Model and New Observations of Triton

NASA Astrophysics Data System (ADS)

Zhang, H.-Y.; Shen, K.-X.; Qiao, R.-Ch; Dourneau, G.; Yu, Y.

2015-10-01

We used 3108 Earth-based astrometric observations from the Natural Satellite Data Center (NSDC) over more than 30 years time span from 1975 to 2006 for determining the epoch state vectors of the Neptunes largest satellite Triton. In integrating the perturbation equation, the barycentric frame of Neptune-Triton system is adopted, and in considering the oblateness perturbation due to Neptune, a revised pole model describing the precession of the Neptune's pole is used in our calculation. Moreover, a total of 1095 new observed positions of Triton were collected during 46 nights of observations in 2007, 2008 and 2009. We compared our observations to two ephemerides of Triton and most of the available planetary ephemerides of Neptune.

Neptune and Titan Observed with Keck Telescope Adaptive Optics

DOE Office of Scientific and Technical Information (OSTI.GOV)

Max, C.E.; Macintosh, B.A.; Gibbard, S.

2000-05-05

The authors report on observations taken during engineering science validation time using the new adaptive optics system at the 10-m Keck II Telescope. They observe Neptune and Titan at near-infrared wavelengths. These objects are ideal for adaptive optics imaging because they are bright and small, yet have many diffraction-limited resolution elements across their disks. In addition Neptune and Titan have prominent physical features, some of which change markedly with time. They have observed infrared-bright storms on Neptune, and very low-albedo surface regions on Titan, Saturn's largest moon, Spatial resolution on Neptune and Titan was 0.05-0.06 and 0.04-0.05 arc sec, respectively.

Neptune Polar Orbiter with Probes

NASA Technical Reports Server (NTRS)

Bienstock, Bernard; Atkinson, David; Baines, Kevin; Mahaffy, Paul; Steffes, Paul; Atreya, Sushil; Stern, Alan; Wright, Michael; Willenberg, Harvey; Smith, David;

Neptune Through a Clear Filter

NASA Image and Video Library

1999-07-25

On July 23, 1989, NASA Voyager 2 spacecraft took this picture of Neptune through a clear filter on its narrow-angle camera. The image on the right has a latitude and longitude grid added for reference. Neptune Great Dark Spot is visible on the left.

Stratospheric ethane on Neptune - Comparison of groundbased and Voyager IRIS retrievals

NASA Technical Reports Server (NTRS)

Kostiuk, Theodor; Romani, Paul; Espenak, Fred; Bezard, Bruno

1992-01-01

Near-simultaneous ground and spacecraft measurements of 12-micron ethane emission spectra during the Voyager encounter with Neptune have furnished bases for the determination of stratospheric ethane abundance and the testing and constraining of Neptune methane-photochemistry models. The ethane retrievals were sensitive to the thermal profile used. Contribution functions for warm thermal profiles peaked at higher altitudes, as expected, with the heterodyne functions covering lower-pressure regions. Both constant- and nonconstant-with-height profiles remain candidate distributions for Neptune's stratospheric ethane.

Participation in the Cluster Magnetometer Consortium for the Cluster Mission

NASA Technical Reports Server (NTRS)

Kivelson, Margaret

1997-01-01

Prof. M. G. Kivelson (UCLA) and Dr. R. C. Elphic (LANL) are Co-investigators on the Cluster Magnetometer Consortium (CMC) that provided the fluxgate magnetometers and associated mission support for the Cluster Mission. The CMC designated UCLA as the site with primary responsibility for the inter-calibration of data from the four spacecraft and the production of fully corrected data critical to achieving the mission objectives. UCLA was also charged with distributing magnetometer data to the U.S. Co-investigators. UCLA also supported the Technical Management Team, which was responsible for the detailed design of the instrument and its interface. In this final progress report we detail the progress made by the UCLA team in achieving the mission objectives.

Dynamics of a satellite and normalization around lagrangian points in the Neptune-Triton system

NASA Astrophysics Data System (ADS)

Yokoyama, T.; Stuchi, T. J.; Solórzano, C. R. H.; Corria, A. A.; Prado, A. F. B.; Winter, O. C.; Winter, S. M. G.; Sanchez, D. M.

Since a mission to Pluto-Charon is in progress a similar mission to Neptune-Triton system probably is just a matter of time Besides the interesting items listed in the Hammel s proposal to explore Neptune Hammel et al 2002 there are others very interesting points Triton is a very large satellite with M T M N approx 2 09 times 10 -4 where M T and M N are the masses of Triton and Neptune respectively Its current inclination with respect to Neptune s equator is about 157 345 0 This unusual high and retrograde inclination for a very large inner satellite makes this problem unique in our solar system Hammel et al 2002 also propose that a top priority in this mission should be a Neptune-Triton orbiter not just a flyby tour Therefore assuming a massless spacecraft orbiting Neptune-Triton system basically the system can be stated in terms of the classical restricted three body problem The new ingredient is the Neptune oblateness and the retrograde motion of Triton With some slight displacements the lagrangian equilibria points still exist as well as many of the properties of the classical problem In this work we first give an extensive numerical exploration in the case when the spacecraft orbits Triton considering Sun Neptune and its oblateness as disturbers In the plane bf a times bf I where bf a is the semi major axis and bf I is the inclination of the orbiter we give a plot of the stable regions where the massless can survive for thousand of years Retrograde and direct inclinations were

Long-term safety and efficacy of single-tablet combinations of solifenacin and tamsulosin oral controlled absorption system in men with storage and voiding lower urinary tract symptoms: results from the NEPTUNE Study and NEPTUNE II open-label extension.

PubMed

Drake, Marcus J; Chapple, Christopher; Sokol, Roman; Oelke, Matthias; Traudtner, Klaudia; Klaver, Monique; Drogendijk, Ted; Van Kerrebroeck, Philip

2015-02-01

Short-term trials have demonstrated the efficacy and safety of combination therapy using antimuscarinics and α-blockers in men with lower urinary tract symptoms (LUTS). The Study of Solifenacin Succinate and Tamsulosin Hydrochloride OCAS (oral controlled absorption system) in Males with Lower Urinary Tract Symptoms (NEPTUNE) II is the first long-term study using solifenacin (Soli) and the oral controlled absorption system formulation of tamsulosin (TOCAS). To evaluate long-term (up to 52 wk) safety and efficacy of flexible dosing of two fixed-dose combinations (FDC) of Soli plus TOCAS in men with moderate to severe storage symptoms and voiding symptoms. Patients with both storage and voiding LUTS, maximum urinary flow rate of 4.0-12.0 ml/s, prostate size <75 ml, and postvoid residuals ≤ 150 ml, who completed the 12-wk, double-blind NEPTUNE study could continue in the 40-wk, open-label NEPTUNE II study. FDC of Soli 6 mg plus TOCAS 0.4 mg, or Soli 9 mg plus TOCAS 0.4mg; patients could switch between doses in NEPTUNE II. Safety and efficacy data from NEPTUNE and NEPTUNE II were combined to cover a 52-wk period. Primary efficacy end points were total International Prostate Symptom Score (IPSS) and total urgency and frequency score (TUFS); secondary end points included IPSS storage and voiding subscores, micturition diary variables, and quality of life parameters. In all, 1066 men completed NEPTUNE and received one dose or more of study medication in NEPTUNE II. Treatment-emergent adverse events were reported in 499 (46.8%) patients who participated in NEPTUNE II; most were mild or moderate. Urinary retention occurred in 13 of 1208 (1.1%) patients receiving one or more FDCs in NEPTUNE and/or NEPTUNE II; 8 (0.7%) required catheterisation (acute urinary retention [AUR]). Reductions in total IPSS and TUFS during NEPTUNE were maintained for up to 52 wk of FDC treatment, with mean reductions of 9.0 (standard deviation [SD]: 5.7) and 10.1 (SD: 9.2), respectively, from baseline to end of treatment. Clinically relevant improvements were also observed for secondary efficacy end points. Long-term treatment with FDC Soli plus TOCAS was well tolerated and efficacious in men with storage and voiding LUTS, with a low incidence of AUR. Treatment with solifenacin plus tamsulosin in a fixed-dose combination tablet was well tolerated by men with lower urinary tract symptoms. Improvements in symptoms were achieved after 4 wk of treatment, with further improvements at week 16 maintained for up to 52 wk throughout the study. Copyright © 2014 European Association of Urology. Published by Elsevier B.V. All rights reserved.

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Bonnie Buratti, senior scientist at NASA's Jet Propultion Laboratory, speaks during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

Haze production rates in super-Earth and mini-Neptune atmosphere experiments

NASA Astrophysics Data System (ADS)

Hörst, Sarah M.; He, Chao; Lewis, Nikole K.; Kempton, Eliza M.-R.; Marley, Mark S.; Morley, Caroline V.; Moses, Julianne I.; Valenti, Jeff A.; Vuitton, Véronique

2018-04-01

Numerous Solar System atmospheres possess photochemically generated hazes, including the characteristic organic hazes of Titan and Pluto. Haze particles substantially impact atmospheric temperature structures and may provide organic material to the surface of a world, potentially affecting its habitability. Observations of exoplanet atmospheres suggest the presence of aerosols, especially in cooler (<800 K), smaller (<0.3× Jupiter's mass) exoplanets. It remains unclear whether the aerosols muting the spectroscopic features of exoplanet atmospheres are condensate clouds or photochemical hazes1-3, which is difficult to predict from theory alone4. Here, we present laboratory haze simulation experiments that probe a broad range of atmospheric parameters relevant to super-Earth- and mini-Neptune-type planets5, the most frequently occurring type of planet in our galaxy6. It is expected that photochemical haze will play a much greater role in the atmospheres of planets with average temperatures below 1,000 K (ref. 7), especially those planets that may have enhanced atmospheric metallicity and/or enhanced C/O ratios, such as super-Earths and Neptune-mass planets8-12. We explored temperatures from 300 to 600 K and a range of atmospheric metallicities (100×, 1,000× and 10,000× solar). All simulated atmospheres produced particles, and the cooler (300 and 400 K) 1,000× solar metallicity (`H2O-dominated' and CH4-rich) experiments exhibited haze production rates higher than our standard Titan simulation ( 10 mg h-1 versus 7.4 mg h-1 for Titan13). However, the particle production rates varied greatly, with measured rates as low as 0.04 mg h-1 (for the case with 100× solar metallicity at 600 K). Here, we show that we should expect great diversity in haze production rates, as some—but not all—super-Earth and mini-Neptune atmospheres will possess photochemically generated haze.

Haze production rates in super-Earth and mini-Neptune atmosphere experiments

NASA Astrophysics Data System (ADS)

Hörst, Sarah M.; He, Chao; Lewis, Nikole K.; Kempton, Eliza M.-R.; Marley, Mark S.; Morley, Caroline V.; Moses, Julianne I.; Valenti, Jeff A.; Vuitton, Véronique

2018-03-01

Numerous Solar System atmospheres possess photochemically generated hazes, including the characteristic organic hazes of Titan and Pluto. Haze particles substantially impact atmospheric temperature structures and may provide organic material to the surface of a world, potentially affecting its habitability. Observations of exoplanet atmospheres suggest the presence of aerosols, especially in cooler (<800 K), smaller (<0.3× Jupiter's mass) exoplanets. It remains unclear whether the aerosols muting the spectroscopic features of exoplanet atmospheres are condensate clouds or photochemical hazes1-3, which is difficult to predict from theory alone4. Here, we present laboratory haze simulation experiments that probe a broad range of atmospheric parameters relevant to super-Earth- and mini-Neptune-type planets5, the most frequently occurring type of planet in our galaxy6. It is expected that photochemical haze will play a much greater role in the atmospheres of planets with average temperatures below 1,000 K (ref. 7), especially those planets that may have enhanced atmospheric metallicity and/or enhanced C/O ratios, such as super-Earths and Neptune-mass planets8-12. We explored temperatures from 300 to 600 K and a range of atmospheric metallicities (100×, 1,000× and 10,000× solar). All simulated atmospheres produced particles, and the cooler (300 and 400 K) 1,000× solar metallicity (`H2O-dominated' and CH4-rich) experiments exhibited haze production rates higher than our standard Titan simulation ( 10 mg h-1 versus 7.4 mg h-1 for Titan13). However, the particle production rates varied greatly, with measured rates as low as 0.04 mg h-1 (for the case with 100× solar metallicity at 600 K). Here, we show that we should expect great diversity in haze production rates, as some—but not all—super-Earth and mini-Neptune atmospheres will possess photochemically generated haze.

Voyager's last encounter

NASA Technical Reports Server (NTRS)

Miner, Ellis D.

1989-01-01

Preliminary results from Voyager's encounter with Neptune are reviewed. The major events of the encounter are listed and the data on the atmosphere, magnetosphere, and ring-arc region of Neptune are discussed. The communications and photographical techniques used in the mission are examined. In addition, a search for Neptune satellites is considered.

50 CFR 217.178 - Renewal of Letters of Authorization and adaptive management.

Code of Federal Regulations, 2011 CFR

2011-10-01

... to Operation and Maintenance of the Neptune Liquefied Natural Gas Facility Off Massachusetts § 217... modify or augment the existing mitigation or monitoring measures (after consulting with Neptune regarding... modify the mitigation or monitoring measures: (1) Results from Neptune's monitoring from the previous...

Graduate Student Diversity. Graduate Focus: Issues in Graduate Education at UCLA.

ERIC Educational Resources Information Center

Hune, Shirley; Benkin, Ellen; Jordan, Patricia

This issue of Graduate Focus provides a brief status report on ethnic diversity at the University of California Los Angeles (UCLA). It includes an overview of relevant institutional data and notes various issues, concerns, and current activities. In graduate programs, UCLA designates as underrepresented minorities domestic students of…

2011 HM{sub 102}: DISCOVERY OF A HIGH-INCLINATION L5 NEPTUNE TROJAN IN THE SEARCH FOR A POST-PLUTO NEW HORIZONS TARGET

DOE Office of Scientific and Technical Information (OSTI.GOV)

Parker, Alex H.; Holman, Matthew J.; McLeod, Brian A.

We present the discovery of a long-term stable L5 (trailing) Neptune Trojan in data acquired to search for candidate trans-Neptunian objects for the New Horizons spacecraft to fly by during an extended post-Pluto mission. This Neptune Trojan, 2011 HM{sub 102}, has the highest inclination (29. Degree-Sign 4) of any known member of this population. It is intrinsically brighter than any single L5 Jupiter Trojan at H{sub V} {approx} 8.18. We have determined its gri colors (a first for any L5 Neptune Trojan), which we find to be similar to the moderately red colors of the L4 Neptune Trojans, suggesting similarmore » surface properties for members of both Trojan clouds. We also present colors derived from archival data for two L4 Neptune Trojans (2006 RJ{sub 103} and 2007 VL{sub 305}), better refining the overall color distribution of the population. In this document we describe the discovery circumstances, our physical characterization of 2011 HM{sub 102}, and this object's implications for the Neptune Trojan population overall. Finally, we discuss the prospects for detecting 2011 HM{sub 102} from the New Horizons spacecraft during its close approach in mid- to late-2013.« less

Aerocapture Guidance Performance for the Neptune Orbiter

NASA Technical Reports Server (NTRS)

Masciarelli, James P.; Westhelle, Carlos H.; Graves, Claude A.

2004-01-01

A performance evaluation of the Hybrid Predictor corrector Aerocapture Scheme (HYPAS) guidance algorithm for aerocapture at Neptune is presented in this paper for a Mission to Neptune and the Neptune moon Triton'. This mission has several challenges not experienced in previous aerocapture guidance assessments. These challengers are a very high Neptune arrival speed, atmospheric exit into a high energy orbit about Neptune, and a very high ballistic coefficient that results in a low altitude acceleration capability when combined with the aeroshell LD. The evaluation includes a definition of the entry corridor, a comparison to the theoretical optimum performance, and guidance responses to variations in atmospheric density, aerodynamic coefficients and flight path angle for various vehicle configurations (ballistic numbers). The benefits of utilizing angle-of-attack modulation in addition to bank angle modulation to improve flight performance is also discussed. The results show that despite large sensitivities in apoapsis targeting, the algorithm performs within the allocated AV budget for the Neptune mission bank angle only modulation. The addition of angle-of-attack modulation with as little as 5 degrees of amplitude significantly improves the scatter in final orbit apoapsis. Although the angle-of-attack modulation complicates the vehicle design, the performance enhancement reduces aerocapture risk and reduces the propellant consumption needed to reach the high energy target orbit for a conventional propulsion system.

The First Neptune Analog or Super-Earth with a Neptune-Like Orbit: MOA-2013-BLG-605Lb

NASA Technical Reports Server (NTRS)

Sumi, T.; Bennett, D. P.; Udalski, A.; Gould, A.; Poleski, R.; Bond, I. A.; Skowron, J.; Rattenbury, N.; Pogge, R. W.; Bensby, T.

2016-01-01

We present the discovery of the first Neptune analog exoplanet or super-Earth with a Neptune-like orbit, MOA- 2013-BLG-605Lb. This planet has a mass similar to that of Neptune or a super-Earth and it orbits at 9 approximately 14 times the expected position of the snow line, a(sub snow), which is similar to Neptune's separation of 11 a(sub snow) from the Sun. The planet/host-star mass ratio is q = (3.6 +/- 0.7) × 10(exp -4) and the projected separation normalized by the Einstein radius is s = 2.39 +/- 0.05. There are three degenerate physical solutions and two of these are due to a new type of degeneracy in the microlensing parallax parameters, which we designate "the wide degeneracy." The three models have (i) a Neptune-mass planet with a mass of M(sub p) = 21(+6/-7)(M) orbiting a low-mass M-dwarf with a mass of M(sub h) = 0.19(+0.05/-0.06 (solar mass)), (ii) a mini-Neptune with M(sub p) = 7.9(+1.8/-1.5)(M)) orbiting a brown dwarf host with M(sub h) = 0.068(+0.019/-0.011(solar mass)), and (iii) a super-Earth with M(sub p) = 3.2(+0.5/-0.3(M)) orbiting a low-mass brown dwarf host with M(sub h) = 0.025(+0.005/-0.004)(solar mass)), which is slightly favored. The 3D planet-host separations are 4.6(+4.7/-1.2)au, 2.1(+1.0/-0.2)au, and 0.94(+0.67/-0.02)au, which are 8.9(+10.5/-1.4)m 12(+7/-1), or 14(+11/-1) times larger than a(sub snow) for these models, respectively. Keck adaptive optics observations confirm that the lens is faint. This discovery suggests that low-mass planets with Neptune-like orbits are common. Therefore processes similar to the one that formed Neptune in our own solar system or cold super-Earths may be common in other solar systems.

UCLA Plans Online Encyclopedia of Egyptology

ERIC Educational Resources Information Center

Howard, Jennifer

2006-01-01

The University of California at Los Angeles (UCLA) has unveiled plans for what appears to be the world's first online, peer-reviewed encyclopedia devoted to ancient Egypt. The "UCLA Encyclopedia of Egypt," which in April won a $325,000 grant from the National Endowment for the Humanities, will include material in Arabic as well as…

Neptune: a bioinformatics tool for rapid discovery of genomic variation in bacterial populations

PubMed Central

Marinier, Eric; Zaheer, Rahat; Berry, Chrystal; Weedmark, Kelly A.; Domaratzki, Michael; Mabon, Philip; Knox, Natalie C.; Reimer, Aleisha R.; Graham, Morag R.; Chui, Linda; Patterson-Fortin, Laura; Zhang, Jian; Pagotto, Franco; Farber, Jeff; Mahony, Jim; Seyer, Karine; Bekal, Sadjia; Tremblay, Cécile; Isaac-Renton, Judy; Prystajecky, Natalie; Chen, Jessica; Slade, Peter

2017-01-01

Abstract The ready availability of vast amounts of genomic sequence data has created the need to rethink comparative genomics algorithms using ‘big data’ approaches. Neptune is an efficient system for rapidly locating differentially abundant genomic content in bacterial populations using an exact k-mer matching strategy, while accommodating k-mer mismatches. Neptune’s loci discovery process identifies sequences that are sufficiently common to a group of target sequences and sufficiently absent from non-targets using probabilistic models. Neptune uses parallel computing to efficiently identify and extract these loci from draft genome assemblies without requiring multiple sequence alignments or other computationally expensive comparative sequence analyses. Tests on simulated and real datasets showed that Neptune rapidly identifies regions that are both sensitive and specific. We demonstrate that this system can identify trait-specific loci from different bacterial lineages. Neptune is broadly applicable for comparative bacterial analyses, yet will particularly benefit pathogenomic applications, owing to efficient and sensitive discovery of differentially abundant genomic loci. The software is available for download at: http://github.com/phac-nml/neptune. PMID:29048594

On the oblateness and rotation rate of Neptune's atmosphere

NASA Technical Reports Server (NTRS)

Hubbard, W. B.

1986-01-01

Recent observations of a stellar occultation by Neptune give an oblateness of 0.022 + or - 0.004 for Neptune's atmosphere at the 1-microbar pressure level. This results is consistent with hydrostatic equilibrium at a uniform atmospheric rotation period of 15 hours, although the error bars on quantities used in the calculation are such that an 18-hour period is not excluded. The oblateness of a planetary atmosphere is determined from stellar occultations by measuring the times at which a specified point on immersion or emersion occultation profiles is reached. Whether this standard procedure for deriving the shape of the atmosphere is consistent with what is known about vertical and horizontal temperature gradients in Neptune's atmosphere is evaluated. The nature of the constraint placed on the interior mass distribution by an oblateness determined in this manner is consided, as is the effects of possible differential rotation. A 15-hour Neptune internal mass distribution is approximately homologous to Uranus', but an 18-hour period is not. The implications for Neptune's interior structure if its body rotation period is actually 18 hours are discussed.

The Atmospheric Diversity of Mini-Neptunes in Multi-planet Systems

NASA Astrophysics Data System (ADS)

Crossfield, Ian

2017-08-01

Mini-Neptunes, planets 2-4 times the size of the Earth, are anintriguing population. They are an abundant outcome of planetformation and occur around more than a quarter of all stars -- yetthey are absent in the Solar System. Mini-Neptunes bridge the gapbetween terrestrial planets and gas giants, and atmospherecharacterization of these planets has much to reveal about their currentproperties, origins, and evolutionary histories. However, only a handful of mini-Neptunes have been amenable to atmospheric study so far.We propose a survey of four mini-Neptunes recently discovered by ourteam around bright, nearby stars. These observations will nearlydouble the number of planets in this size range with measuredtransmission spectra. Our observations will yield high-precisionconstraints on the planets' atmospheric metallicities, elementalabundances, C/O ratios, and aerosol content. With a greatly expandedmini-Neptune sample, we will identify trends in planet properties as afunction of equilibrium temperature, UV irradiation, planet mass, andstellar spectral type. These trends will also identify specificpromising targets for further study with JWST, and will help usprioritize follow-up and atmospheric characterization of themany small planets expected from the TESS survey.

Did Triton Destroy Neptune's First Moons?

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2017-11-01

Neptunes moon system is not what we would expect for a gas giant in our solar system. Scientists have now explored the possibility that Neptune started its life with an ordinary system of moons that was later destroyed by the capture of its current giant moon, Triton.An Odd SystemOur current understanding of giant-planet formation predicts a period of gas accretion to build up the large size of these planets. According to models, the circumplanetary gas disks that surround the planets during this time then become the birthplaces of the giant planets satellite systems, producing systems of co-planar and prograde (i.e., orbiting in the same direction as the planets rotation) satellites similar to the many-moon systems of Jupiter or Saturn.Tritons orbit is tilted relative to the inner Neptunian satellite orbits. [NASA, ESA, and A. Feild (STScI)]Neptune, however, is quirky. This gas giant has surprisingly few satellites only 14 compared to, say, the nearly 70 moons of Jupiter and most of them are extremely small. One of Neptunes moons is an exception to this, however: Triton, which contains 99.7% of the mass of Neptunes entire satellite system!Tritons orbit has a number of unusual properties. The orbit is retrograde Triton orbits in the opposite direction as Neptunes rotation which is unique behavior among large moons in our solar system. Tritons orbit is also highly inclined, and yet the moons path is nearly circular and lies very close to Neptune.The distribution of impact velocities in the authors simulations for primordial satellite interactions with Triton, in three cases of different satellite mass ratios. In the low-mass case a third of the mass ratio of the Uranian satellite system 88% of simulations ended with Triton surviving on its high-inclination orbit. The survival rate was only 12% in the high-mass case. [Adapted from Rufu et al. 2017]How did this monster of a satellite get its strange properties, and why is Neptunes system so odd compared to what we would expect for a gas giants satellites? Two scientists, Raluca Rufu (Weizmann Institute of Science, Israel) and Robin Canup (Southwest Research Institute), propose an explanation in which Triton long ago wreaked havoc on a former system of satellites around Neptune.Destruction After CaptureRufu and Canup explore the scenario in which Neptune once had an ordinary, prograde system of moons around it that resembled those of the other gas giants. Triton, the authors suggest, may have been a former Kuiper belt object that was then captured by Neptune. The ensuing interactions between retrograde Triton and Neptunes original, prograde satellite system may have then resulted in the destruction of this original system, leaving behind only Triton and Neptunes other current satellites.Nereid, a small irregular moon of Neptune, orbits at an average distance of more than 15 times that of Triton. Models of Tritons orbital evolution must also account for the preservation of satellites like this one. [NASA]Using N-body simulations that model a newly captured Triton and a likely primordial prograde system of moons, Rufu and Canup show that if the moons have a mass ratio similar to that of Uranuss system or smaller, Tritons interactions with it have a substantial likelihood of reproducing the current Neptunian satellite system. They even demonstrate that the interactions decrease Tritons initial semimajor axis quickly enough to prevent smaller, outer satellites like Nereid from being kicked out of the system.If the authors picture is correct, then it neatly explains why Neptunes satellite system looks so unusual compared to Jupiters or Saturns which means that our models of how primordial systems of moons form around gas giants still holdstrong.CitationRaluca Rufu and Robin M. Canup 2017 AJ 154 208. doi:10.3847/1538-3881/aa9184

Uranus and Neptune orbiter missions via solar electric propulsion

NASA Technical Reports Server (NTRS)

Friedlander, A. L.; Brandenburg, R. K.

1971-01-01

The characteristics and capabilities of solar electric propulsion for performing orbiter missions at the planets Uranus and Neptune are described. An assessment of the scientific objectives and instrumentation requirements, their relation to orbit size selection, and parametric analysis of solar electric propulsion trajectory/payload performance are included. Utilizing the Titan 3D/Centaur launch vehicle, minimum flight times of about 3400 days to Uranus and 5300 days to Neptune are required to place the TOPS spacecraft into the nominal orbits. It has been shown that solar electric propulsion can be used effectively to accomplish elliptical orbiter missions at Uranus and Neptune. However, because of the very long flight time required, these mission profiles are not too attractive. Previous studies have shown that nuclear electric propulsion, if developed, would allow much faster trips; 5 years to Uranus and 8 years to Neptune.

Voyager 2 Neptune targeting strategy

NASA Technical Reports Server (NTRS)

Potts, C. L.; Francis, K.; Matousek, S. E.; Cesarone, R. J.; Gray, D. L.

1989-01-01

The success of the Voyager 2 flybys of Neptune and Triton depends upon the ability to correct the spacecraft's trajectory. Accurate spacecraft delivery to the desired encounter conditions will promote the maximum science return. However, Neptune's great distance causes large a priori uncertainties in Neptune and Triton ephemerides and planetary system parameters. Consequently, the 'ideal' trajectory is unknown beforehand. The targeting challenge is to utilize the gradually improving knowledge as the spacecraft approaches Neptune to meet the science objectives, but with an overriding concern for spacecraft safety and a desire to limit propellant expenditure. A unique targeting strategy has been developed in response to this challenge. Through the use of a Monte Carlo simulation, candidate strategies are evaluated by the degree to which they meet these objectives and are compared against each other in determining the targeting strategy to be adopted.

A thick cloud of Neptune Trojans and their colors.

PubMed

Sheppard, Scott S; Trujillo, Chadwick A

2006-07-28

The dynamical and physical properties of asteroids offer one of the few constraints on the formation, evolution, and migration of the giant planets. Trojan asteroids share a planet's semimajor axis but lead or follow it by about 60 degrees near the two triangular Lagrangian points of gravitational equilibrium. Here we report the discovery of a high-inclination Neptune Trojan, 2005 TN(53). This discovery demonstrates that the Neptune Trojan population occupies a thick disk, which is indicative of "freeze-in" capture instead of in situ or collisional formation. The Neptune Trojans appear to have a population that is several times larger than the Jupiter Trojans. Our color measurements show that Neptune Trojans have statistically indistinguishable slightly red colors, which suggests that they had a common formation and evolutionary history and are distinct from the classical Kuiper Belt objects.

Engineering-Level Model Atmospheres for Titan and Neptune

NASA Technical Reports Server (NTRS)

Justus, C. G.; Duvall, Aleta; Johnson, D. L.

2003-01-01

Engineering-level atmospheric models for Titan and Neptune have been developed for use in NASA s systems analysis studies of aerocapture applications in missions to the outer planets. Analogous to highly successful Global Reference Atmospheric Models for Earth (GRAM, Justus et al., 2000) and Mars (Mars-GRAM, Justus and Johnson, 2001, Justus et al., 2002) the new models are called Titan-GRAM and Neptune-GRAM. Like GRAM and Mars-GRAM, an important feature of Titan-GRAM and Neptune-GRAM is their ability to simulate quasi-random perturbations for Monte- Carlo analyses in developing guidance, navigation and control algorithms, and for thermal systems design.

Confirmatory factor analysis of the Revised UCLA Loneliness Scale (UCLA LS-R) in individuals over 65.

PubMed

Ausín, Berta; Muñoz, Manuel; Martín, Teresa; Pérez-Santos, Eloísa; Castellanos, Miguel Ángel

2018-01-08

The UCLA LS-R is the most extensively used scale to assess loneliness. However, few studies examine the scale's use on older individuals. The goal of the study is to analyse the suitability of the scale´s structure for assessing older individuals. The UCLA LS-R scale was administered to a random sample of 409 community-dwelling residents of Madrid (53% women) aged 65-84 years (obtained from the MentDis_ICF65+ study). Confirmatory factor analysis was used to assess the factor structure of the UCLA LS-R. The internal consistency of the scale obtained a Cronbach's alpha of .85. All the analysed models of factor structure of the UCLA LS-R achieved a fairly good fit and RMSEA values over .80. The models that best fit the empirical data are those of Hojat (1982) and Borges et al. (2008). The data suggest an equivalent effectiveness of UCLA LS-R in adults under 65 and over 65, which may indicate a similar structure of the loneliness construct in both populations. This outcome is consistent with the idea that loneliness has two dimensions: emotional loneliness and social loneliness. The use of short measures that are easy to apply and interpret should help primary care professionals identify loneliness problems in older individuals sooner and more accurately.

Impact of the University of California, Los Angeles/Charles R. Drew University Medical Education Program on medical students' intentions to practice in underserved areas.

PubMed

Ko, Michelle; Edelstein, Ronald A; Heslin, Kevin C; Rajagopalan, Shobita; Wilkerson, Luann; Colburn, Lois; Grumbach, Kevin

2005-09-01

To estimate the impact of a U.S. inner-city medical education program on medical school graduates' intentions to practice in underserved communities. The authors conducted an analysis of secondary data on 1,088 medical students who graduated from either the joint University of California, Los Angeles/Charles R. Drew University Medical Education Program (UCLA/Drew) or the UCLA School of Medicine between 1996 and 2002. Intention to practice in underserved communities was measured using students' responses to questionnaires administered at matriculation and graduation for program improvement by the Association of American Medical Colleges. Multivariate logistic regression analysis was used to compare the odds of intending to practice in underserved communities among UCLA/Drew students with those of their counterparts in the UCLA School of Medicine. Compared with students in the UCLA School of Medicine, UCLA/Drew students had greater adjusted odds of reporting intention to work in underserved communities at graduation, greater odds of maintaining or increasing such intentions between matriculation and graduation, and lower odds of decreased intention to work in underserved communities between matriculation and graduation. Training in the UCLA/Drew program was independently associated with intention to practice medicine in underserved communities, suggesting that a medical education program can have a positive effect on students' goals to practice in underserved areas.

Survival of a planet in short-period Neptunian desert under effect of photoevaporation

NASA Astrophysics Data System (ADS)

Ionov, Dmitry E.; Pavlyuchenkov, Yaroslav N.; Shematovich, Valery I.

2018-06-01

Despite the identification of a great number of Jupiter-like and Earth-like planets at close-in orbits, the number of `hot Neptunes' - the planets with 0.6-18 times of Neptune mass and orbital periods less than 3 d - turned out to be very small. The corresponding region in the mass-period distribution was assigned as the `short-period Neptunian desert'. The common explanation of this fact is that the gaseous planet with few Neptune masses would not survive in the vicinity of host star due to intensive atmosphere outflow induced by heating from stellar radiation. To check this hypothesis, we performed numerical simulations of atmosphere dynamics for a hot Neptune. We adopt the previously developed self-consistent 1D model of hydrogen-helium atmosphere with suprathermal electrons accounted. The mass-loss rates as a function of orbital distances and stellar ages are presented. We conclude that the desert of short-period Neptunes could not be entirely explained by evaporation of planet atmosphere caused by the radiation from a host star. For the less massive Neptune-like planet, the estimated upper limits of the mass-loss may be consistent with the photoevaporation scenario, while the heavier Neptune-like planets could not lose the significant mass through this mechanism. We also found the significant differences between our numerical results and widely used approximate estimates of the mass-loss.

33 CFR 165.T01-0542 - Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA.

Code of Federal Regulations, 2010 CFR

2010-07-01

... 33 Navigation and Navigable Waters 2 2010-07-01 2010-07-01 false Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. 165.T01-0542 Section 165.T01-0542 Navigation and Navigable Waters... Guard District § 165.T01-0542 Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. (a...

75 FR 34929 - Safety Zones: Neptune Deep Water Port, Atlantic Ocean, Boston, MA

Federal Register 2010, 2011, 2012, 2013, 2014

2010-06-21

...-AA00 Safety Zones: Neptune Deep Water Port, Atlantic Ocean, Boston, MA AGENCY: Coast Guard, DHS. ACTION..., Boston, MA; Final Rule (USCG-2009-0589), to protect vessels from the hazard posed by the presence of the... read as follows: Sec. 165.T01-0542 Safety Zones: Neptune Deepwater Port, Atlantic Ocean, Boston, MA. (a...

Neptune's Stormy Disposition

NASA Technical Reports Server (NTRS)

1998-01-01

Using powerful ground-and space-based telescopes, scientists have obtained a moving look at some of the wildest, weirdest weather in the solar system.

Combining simultaneous observations of Neptune made with the Hubble Space Telescope and NASA's Infrared Telescope Facility on Mauna Kea, Hawaii, a team of scientists led by Lawrence A. Sromovsky of the University of Wisconsin-Madison has captured the most insightful images to date of a planet whose blustery weather -- monster storms and equatorial winds of 900 miles per hour -- bewilders scientists.

Blending a series of Hubble images, Sromovsky's team constructed a time-lapse rotation movie of Neptune, permitting scientists to watch the ebb and flow of the distant planet's weather. And while the observations, presented here at a meeting of the American Astronomical Society's Division of Planetary Science, are helping scientists tease out clues to the planet's stormy weather, they also are deepening some of Neptune's mysteries, said Sromovsky.

The weather on Neptune, the eighth planet from the sun, is an enigma to begin with. The mechanism that drives its near-supersonic winds and giant storms has yet to be discerned.

On Earth, weather is driven by energy from the sun as it heats the atmosphere and oceans. On Neptune, the sun is 900 times dimmer and scientists have yet to understand how Neptune's weather-generating machinery can be so efficient.

'It's an efficient weather machine compared to Earth,' said Sromovsky. 'It seems to run on almost no energy.'

In an effort to dissect the distant planet's atmosphere and monitor its bizarre weather, Sromovsky and his colleagues obtained a series of measurements and images over the span of three of Neptune's rotations.

From those observations, Sromovsky said it is possible to measure Neptune's circulation and view a 'strange menagerie of variable, discrete cloud features and zonal bands' of weather. Moreover, the new observations enabled Sromovsky's team to probe some of the deeper features of the atmosphere and to map Neptune's cloud tops.

'We can show some clouds are higher than others, that altitudes vary,' he said. Knowing something about the topography of Neptune's clouds, provides a direct way to measure Neptune's powerful winds.

A looming mystery, he said, is the fate of huge dark spots, possibly giant storms. When the planetary probe Voyager visited Neptune in 1989, it detected the Great Dark Spot, a pulsating feature nearly the size of the Earth itself. Two years ago, Hubble observations showed the spot had disappeared, and that another, smaller spot had emerged. But instead of growing to a large-scale storm like the Great Dark Spot, the new spot appears to be trapped at a fixed latitude and may be declining in intensity, said Sromovsky, a senior scientist at UW-Madison's Space Science and Engineering Center.

'They behave like storms, and the Great Dark Spot was an exaggerated features we haven't seen on any other planet. They seem to come and go, and rather than an exciting development of these dark spots, they dissipate.'

Another strange aspect of the distant planet's weather are distinct bands of weather that run parallel to the Neptunian equator. The weather bands encircle the planet and, in some respects, may be similar to the equatorial region of the Earth where tropical heat provides abundant energy to make clouds.

'We can see regions of latitude where Neptune consistently generates bright clouds,' said Sromovsky. The regions are both above and below the planet's equator, but he added that it was uncertain what their explanation is in terms of atmospheric circulation.

Sromovsky said that compared to the look provided by the Voyager spacecraft, Neptune is a different place: 'The character of Neptune is different from what it was at the time of Voyager. The planet seems stable, yet different.'

Sromovsky's Hubble observations were made with Wide Field Planetary Camera 2 and the Near Infrared Camera and Multi-Object Spectrometer. The different instruments allowed observations to be made in a variety of wavelengths, each providing a different set of information about Neptune's clouds, their structures and how they circulate.

The Voyager encounter with Uranus and Neptune

NASA Technical Reports Server (NTRS)

Miner, Ellis D.

1986-01-01

Voyager 2 approaches Uranus at a relative low phase angle and high southerly latitude. Only when the spacecraft is very close to Uranus does the geometry change appreciably. Most of the important observations occur within six hours of closest approach. Voyager flies through an Earth and solar occulation zone and leaves Uranus at a relatively high phase angle of about 145 degrees. There isn't much of an opportunity to look at the equatorial region of the planet. At Neptune, on the other hand, the approach is more nearly equatorial (about 35 deg S lat). Voyager 2 will come much closer to Nepture than to any of the other gas giants as it skims within about 2000 km of Neptune's cloudtops. It will pass through earth and solar occultation zones at both Neptune and its satellite, Triton. Again, Voyager 2 will leave Neptune at about 35 deg S latitude. Voyager operational instrument, interplanetary trajectories and planetary encounters are briefly discussed.

Optical navigation during the Voyager Neptune encounter

NASA Technical Reports Server (NTRS)

Riedel, J. E.; Owen, W. M., Jr.; Stuve, J. A.; Synnott, S. P.; Vaughan, R. M.

1990-01-01

Optical navigation techniques were required to successfully complete the planetary exploration phase of the NASA deep-space Voyager mission. The last of Voyager's planetary encounters, with Neptune, posed unique problems from an optical navigation standpoint. In this paper we briefly review general aspects of the optical navigation process as practiced during the Voyager mission, and discuss in detail particular features of the Neptune encounter which affected optical navigation. New approaches to the centerfinding problem were developed for both stars and extended bodies, and these are described. Results of the optical navigation data analysis are presented, as well as a description of the optical orbit determination system and results of its use during encounter. Partially as a result of the optical navigation processing, results of scientific significance were obtained. These results include the discovery and orbit determination of several new satellites of Neptune and the determination of the size of Triton, Neptune's largest moon.

Global magnetic anomaly and aurora of Neptune

NASA Technical Reports Server (NTRS)

Cheng, Andrew F.

1990-01-01

The large offset and tilt of Neptune's dipole magnetic field combine to create a global magnetic anomaly, analogous to but much more important than earth's South Atlantic Anomaly. Energetic particle precipitation loss within the Neptune anomaly creates 'atmospheric drift shadows' within which particle fluxes are greatly reduced. The energetic particle dropout observed by Voyager near closest approach occurred near the predicted times when Voyager passed within the atmospheric drift shadow. Extremely soft, structured bursts of ions and electrons within the drift shadow may result from plasma wave-induced pitch angle scattering of trapped particles confined near the magnetic equator. The dropout does not necessarily imply that Voyager passed through an earth-like discrete auroral zone, as earlier reported. The ion and electron fluxes observed within the dropout period correspond to particles that must precipitate to Neptune's atmosphere within the anomaly region. This anomaly precipitation can account for a major portion of the ultraviolet emissions previously identified as Neptune aurora.

Psychometric Qualities of the UCLA Loneliness Scale-Version 3 as Applied in a Turkish Culture

ERIC Educational Resources Information Center

Durak, Mithat; Senol-Durak, Emre

2010-01-01

The University of California, Los Angeles, Loneliness Scale-Version 3 (UCLA LS3) is the most frequently used loneliness assessment tool. This study aimed to examine the psychometric properties of the UCLA LS3 by utilizing two separate and independent samples: Turkish university students (n = 481) and elderly (n = 284). The results demonstrate that…

Developing the next Generation of Education Researchers: UCLA's Experience with the Spencer Foundation Research Training Grant

ERIC Educational Resources Information Center

Dorr, Aimee; Arms, Emily; Hall, Valerie

2008-01-01

Background/Context: In the early 1990s, the Spencer Foundation instituted an Institutional Research Training Grant (RTG) program to improve the preparation of the next generation of education researchers. UCLA received an RTG in the first round of competition. Purpose/Objective/Research Question/Focus of Study: UCLA's Spencer RTG program sought to…

UCLA High Speed, High Volume Laboratory Network for Infectious Diseases

DTIC Science & Technology

2008-04-01

included: Peter B . Jahrling, David E. Swayne, Jeffrey K . Taubenberger. Those present from LANL included: Tony J. Beugelsdijk (Co-PI) and Gary Resnick...www.whitehouse.gov/news/releases/2007/10/20071018-10.html Xu X, Smith CB, Mungall BA, Lindstrom SE, Hall HE, Subbarao K , et al. Intercontinental Circulation... Subbarao K , Klimov A, Katz J, Regnery H, Lim W, Hall H, et al. Characterization of an avian influenza A (H5N1) virus isolated from a child with a fatal

Oblateness, radius, and mean stratospheric temperature of Neptune from the 1985 August 20 occultation

NASA Technical Reports Server (NTRS)

Hubbard, W. B.; Nicholson, Philip D.; Lellouch, Emmanuel; Sicardy, Bruno; Brahic, Andre; Vilas, Faith

1987-01-01

The oblateness and equatorial radius of Neptune at the 1-microbar pressure level, together with the position angle of the projected spin axis, are the goals of a general oblate atmosphere model for Neptune employing a data ensemble obtained from the occultation of a bright IR star that provided accurate measurements of the limb position at these and several other stations. The observed reduction in central flash intensity is explained by a 150-135 K temperature decrease as pressure rises from 1 to 400 microbar. Attention is given to the implications of these oblateness results for models of the Neptune interior.

Methane photochemistry and methane production on Neptune

NASA Technical Reports Server (NTRS)

Romani, P. N.; Atreya, S. K.

1988-01-01

The Neptune stratosphere's methane photochemistry is presently studied by means of a numerical model in which the observed mixing ratio of methane prompts photolysis near the CH4 homopause. Haze generation by methane photochemistry has its basis in the formation of hydrocarbon ices and polyacetylenes; the hazes can furnish the requisite aerosol haze at the appropriate pressure levels required by observations of Neptune in the visible and near-IR. Comparisons of model predictions with Uranus data indicate a lower ratio of polyacetylene production to hydrocarbon ice, as well as a lower likelihood of UV postprocessing of the acetylene ice to polymers on Neptune, compared to Uranus.

Evaluation of stability of interface between CCM (Co-Cr-Mo) UCLA abutment and external hex implant.

PubMed

Yoon, Ki-Joon; Park, Young-Bum; Choi, Hyunmin; Cho, Youngsung; Lee, Jae-Hoon; Lee, Keun-Woo

2016-12-01

The purpose of this study is to evaluate the stability of interface between Co-Cr-Mo (CCM) UCLA abutment and external hex implant. Sixteen external hex implant fixtures were assigned to two groups (CCM and Gold group) and were embedded in molds using clear acrylic resin. Screw-retained prostheses were constructed using CCM UCLA abutment and Gold UCLA abutment. The external implant fixture and screw-retained prostheses were connected using abutment screws. After the abutments were tightened to 30 Ncm torque, 5 kg thermocyclic functional loading was applied by chewing simulator. A target of 1.0 × 10 6 cycles was applied. After cyclic loading, removal torque values were recorded using a driving torque tester, and the interface between implant fixture and abutment was evaluated by scanning electronic microscope (SEM). The means and standard deviations (SD) between the CCM and Gold groups were analyzed with independent t-test at the significance level of 0.05. Fractures of crowns, abutments, abutment screws, and fixtures and loosening of abutment screws were not observed after thermocyclic loading. There were no statistically significant differences at the recorded removal torque values between CCM and Gold groups ( P >.05). SEM analysis revealed that remarkable wear patterns were observed at the abutment interface only for Gold UCLA abutments. Those patterns were not observed for other specimens. Within the limit of this study, CCM UCLA abutment has no statistically significant difference in the stability of interface with external hex implant, compared with Gold UCLA abutment.

Detection of CS in Neptune's atmosphere from ALMA observations

NASA Astrophysics Data System (ADS)

Moreno, R.; Lellouch, E.; Cavalié, T.; Moullet, A.

2017-12-01

Context. The large and vertically non-uniform abundance of CO in Neptune's atmosphere has been interpreted as the result of past cometary impact(s), either single or distributed in size and time, which could also be at the origin of Neptune's HCN. Aims: We aim to provide observational support for this scenario by searching for other comet-induced species, in particular carbon sulfide (CS) which has been observed continuously in Jupiter since the 1994 Shoemaker-Levy 9 impacts. Methods: In April 2016 we used the ALMA interferometer to search for CS(7-6) at 342.883 GHz in Neptune. Results: We report on the detection of CS in Neptune's atmosphere, the first unambiguous observation of a sulfur-bearing species in a giant planet beyond Jupiter. Carbon sulfide appears to be present only at submillibar levels, with a column density of (2.0-3.1) × 1012 cm-2, and a typical mixing ratio of (2-20) × 10-11 that depends on its precise vertical location. The favoured origin of CS is deposition by a putative large comet impact several centuries ago, and the strong depletion of CS with respect to CO - compared to the Jupiter case - is likely due to the CS sticking to aerosols or clustering to form polymers in Neptune's lower stratosphere. Conclusions: The CS detection, along with recent analyses of the CO profile, reinforces the presumption of a large comet impact into Neptune 1000 yr ago, that delivered CO, CS, and HCN at the same time.

HELIUM ATMOSPHERES ON WARM NEPTUNE- AND SUB-NEPTUNE-SIZED EXOPLANETS AND APPLICATIONS TO GJ 436b

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hu, Renyu; Yung, Yuk L.; Seager, Sara, E-mail: renyu.hu@jpl.nasa.gov

2015-07-01

Warm Neptune- and sub-Neptune-sized exoplanets in orbits smaller than Mercury’s are thought to have experienced extensive atmospheric evolution. Here we propose that a potential outcome of this atmospheric evolution is the formation of helium-dominated atmospheres. The hydrodynamic escape rates of Neptune- and sub-Neptune-sized exoplanets are comparable to the diffusion-limited escape rate of hydrogen, and therefore the escape is heavily affected by diffusive separation between hydrogen and helium. A helium atmosphere can thus be formed—from a primordial hydrogen–helium atmosphere—via atmospheric hydrodynamic escape from the planet. The helium atmosphere has very different abundances of major carbon and oxygen species from those ofmore » a hydrogen atmosphere, leading to distinctive transmission and thermal emission spectral features. In particular, the hypothesis of a helium-dominated atmosphere can explain the thermal emission spectrum of GJ 436b, a warm Neptune-sized exoplanet, while also being consistent with the transmission spectrum. This model atmosphere contains trace amounts of hydrogen, carbon, and oxygen, with the predominance of CO over CH{sub 4} as the main form of carbon. With our atmospheric evolution model, we find that if the mass of the initial atmosphere envelope is 10{sup −3} planetary mass, hydrodynamic escape can reduce the hydrogen abundance in the atmosphere by several orders of magnitude in ∼10 billion years. Observations of exoplanet transits may thus detect signatures of helium atmospheres and probe the evolutionary history of small exoplanets.« less

LAPTAG: Los Angeles Physics Teachers Alliance Group and the UCLA Basic Plasma User Facility.

NASA Astrophysics Data System (ADS)

Gekelman, Walter

2001-10-01

LAPTAG was founded in 1993 during a meeting sponsored by the APS, which encouraged high schools and Universities to form alliances. There are currently about twenty high schools, several community colleges and two Universities (UCLA and USC) involved. At first LAPTAG organized tours of laboratories at UCLA, USC, JPL, General Atomics and the Mt. Wilson Observatory and had meetings in which issues on curricula were discussed. It became obvious after awhile that in order for the group to last that projects were necessary. An early project involved having the high school faculty and students create Websites for most of the schools. This was before most the schools could afford Internet connections and Web authoring tools did not exist. Then with funding from the UC Office of the President, a seismology project was initiated and ten schools received seismometers. There were lectures by geologists and staff members of the Southern California Earthquake center; results were reported on the Web. In the spring of 1999 LAPTAG gave seven posters at the Condensed Matter APS meeting in Los Angeles. A web based astronomy course was created and high school students controlled the Mount Wilson telescope remotely and studied a variable star. Our latest project, funded by the Department of Energy resulted in the construction of a plasma lab dedicated to LAPTAG. The lab has equipment that is used by practicing plasma physicists (tone-burst generators, digital scopes, digital data acquisition and computerized probe drives) as well as software (LabView, PVwave). The high school students and teachers built the machine and all the associated diagnostics. Examples of the experiments will be given, however it is not a cookbook lab. As new experiments are introduced the same difficulties we all face must be overcome; the students take part in this. The LAPD laboratory is now a National User Facility and LAPTAG is a key component of its outreach program. We have met with the director of science for the Los Angeles Unified School district, and others, to muster resources to allow many more schools to participate. This and plans for other programs such as the Integration of Art and Science, will be presented.

Neptune - Unexpected and predicted: Prognosis of theory and Voyager-2 observations

NASA Astrophysics Data System (ADS)

Chechel'Nitskii, A. M.

1992-08-01

The impact of the Voyager-2 discoveries at Neptune on theory are reviewed. The theories of the shell structure of astronomical systems, shell hierarchy, the multicomponent cosmic medium, weak and power elite orbits, quantization of dynamic parameters, and transspheres are summarized and their relevance to the Neptune system, particularly the rings, is considered in the context of the findings of Voyager-2.

Photochemical Modeling of CH3 Abundances in the Outer Solar System

NASA Technical Reports Server (NTRS)

Lee, Anthony Y. T.; Yung, Yuk L.; Moses, Julianne

2000-01-01

Recent measurements of methyl radicals (CH3) in the upper atmospheres of Saturn and Neptune by the Infrared Space Observatory (ISO) provide new constraints to photochemical models of hydrocarbon chemistry in the outer solar system. The derived column abundances of CH3 on Saturn above 10 mbar and Neptune above the 0.2 mbar pressure level are (2.5 - 6.0) x 10(exp 13) / sq cm and (0.7 - 2.8) x 10(exp 13) / sq cm, respectively. We use the updated Caltech/Jet Propulsion Laboratory photochemical model, which incorporates hydrocarbon photochemistry, vertical molecular and bulk atmospheric eddy diffusion, and realistic radiative transfer modeling, to study the CH3 abundances in the upper atmosphere of the giant planets and Titan. We identify the key reactions that control the concentrations of CH3 in the model, such as the three-body recombination reaction, CH3 + CH3 + M yields C2H6 + M. We evaluate and extrapolate the three-body rate constant of this reaction to the low-temperature limit (1.8 x 10(exp -16) T(sup -3.75) e(sup -300/T), T < 300 K) and compare methyl radical abundances in five atmospheres: Jupiter, Saturn, Uranus, Neptune, and Titan. The sensitivity of our models to the rate coefficients for the reactions H + CH3 + M yields CH4 + M, H + C2H3 yields C2H2 + H2, (sup 1)CH2 + H2 yields CH3 + H, and H + C2H5 yields 2CH3, the branching ratios of CH4 photolysis, vertical mixing in the five atmospheres, and Lyman alpha photon enhancement at the orbit of Neptune have all been tested. The results of our model CH3 abundances for both Saturn (5.1 x 10(exp 13) / sq cm) and Neptune (2.2 x 10(exp 13) / sq cm) show good agreement with ISO Short Wavelength Spectrometer measurements. Using the same chemical reaction set, our calculations also successfully generate vertical profiles of stable hydrocarbons consistent with Voyager and ground-based measurements in these outer solar system atmospheres. Predictions of CH3 column concentrations (for p <= 0.2 mbar) in the atmospheres of Jupiter (3.3 x 10(exp 13) /sq cm), Uranus (2.5 x 10(exp 12) / sq cm), and Titan (1.9 x 10(exp 15) / sq cm) may be checked by future observations.

Millimeter-wave spectra of the Jovian planets

NASA Technical Reports Server (NTRS)

Joiner, Joanna; Steffes, Paul G.

1991-01-01

The millimeter wave portion of the electromagnetic spectrum is critical for understanding the subcloud atmospheric structure of the Jovian planets (Jupiter, Saturn, Uranus, and Neptune). This research utilizes a combination of laboratory measurements, computer modeling, and radio astronomical observation in order to obtain a better understanding of the millimeter-wave spectra of the Jovian planets. The pressure broadened absorption from gaseous ammonia (NH3) and hydrogen sulfide (H2S) was measured in the laboratory under simulated conditions for the Jovian atmospheres. Researchers developed new formalisms for computing the absorptivity of gaseous NH3 and H2S based on their laboratory measurements. They developed a radiative transfer and thermochemical model to predict the abundance and distribution of absorbing constituents in the Jovian atmospheres. They used the model to compute the millimeter wave emission from the Jovian planets.

First Earth-based observations of Neptune's satellite Proteus

NASA Astrophysics Data System (ADS)

Colas, F.; Buil, C.

1992-08-01

Proteus (Neptune III) was discovered from Voyager Spacecraft images in 1989 (Smith, 1989). It was never observed from ground-based observatories because of its magnitude (m = 20.3) and closeness to Neptune (maximum elongation = 6 arcsec). In October 1991, we used the 2.2 m telescope at the European Southern Observatory (La Silla, Chile) to look for it. The observation success is mainly due to the use of an anti blooming CCD and to good seeing conditions (less than 1 arcsec). We give the differential positions of Proteus referred to Neptune and we compare with theoretical positions issued from Voyager's data (Owen et al., 1991). We found that the rms orbital residual was about 0.1 arcsec.

Some aspects of the cosmogonic outward migration of Neptune. Co-planar migration

NASA Astrophysics Data System (ADS)

Neslušan, L.; Jakubík, M.

2013-10-01

Considering a simple model of the cosmogonic outward migration of Neptune, we investigate if the assumption of an extremely low orbital inclination of small bodies in a once-existing proto-planetary disk could influence the structure of reservoirs of the objects in the trans-Neptunian region. We found no significant influence. Our models predict only the existence of the mean-motion resonances (MMRs) with Neptune 2:3, 3:5, 1:2, and an anemic scattered disk (MMRs 3:4, 5:7, and 9:11 are also indicated). To explain the classical Edgeworth-Kuiper belt, relatively abundant 4:7 and 2:5 MMRs, and the more numerous scattered disk, we need to assume that, e.g., the outer boundary of the original proto-planetary disk considerably exceeded the distance of the current Neptune's orbit (Neptune probably ended its migration at the distance, where the disk's density started to be sub-critical), or that some Pluto-sized objects resided inside the MMRs and in the distant parts of the original proto-planetary disk.

Evaluation of stability of interface between CCM (Co-Cr-Mo) UCLA abutment and external hex implant

PubMed Central

Yoon, Ki-Joon; Park, Young-Bum; Choi, Hyunmin; Cho, Youngsung; Lee, Jae-Hoon

2016-01-01

PURPOSE The purpose of this study is to evaluate the stability of interface between Co-Cr-Mo (CCM) UCLA abutment and external hex implant. MATERIALS AND METHODS Sixteen external hex implant fixtures were assigned to two groups (CCM and Gold group) and were embedded in molds using clear acrylic resin. Screw-retained prostheses were constructed using CCM UCLA abutment and Gold UCLA abutment. The external implant fixture and screw-retained prostheses were connected using abutment screws. After the abutments were tightened to 30 Ncm torque, 5 kg thermocyclic functional loading was applied by chewing simulator. A target of 1.0 × 106 cycles was applied. After cyclic loading, removal torque values were recorded using a driving torque tester, and the interface between implant fixture and abutment was evaluated by scanning electronic microscope (SEM). The means and standard deviations (SD) between the CCM and Gold groups were analyzed with independent t-test at the significance level of 0.05. RESULTS Fractures of crowns, abutments, abutment screws, and fixtures and loosening of abutment screws were not observed after thermocyclic loading. There were no statistically significant differences at the recorded removal torque values between CCM and Gold groups (P>.05). SEM analysis revealed that remarkable wear patterns were observed at the abutment interface only for Gold UCLA abutments. Those patterns were not observed for other specimens. CONCLUSION Within the limit of this study, CCM UCLA abutment has no statistically significant difference in the stability of interface with external hex implant, compared with Gold UCLA abutment. PMID:28018564

Occultation detection of a Neptunian ring-like arc

NASA Technical Reports Server (NTRS)

Hubbard, W. B.; Brahic, A.; Sicardy, B.; Roques, F.; Elicer, L.-R.; Vilas, F.

1986-01-01

The apparent closest approach of the star SAO186001 to Neptune was observed photoelectrically on July 22, 1984 at Cerro Tololo Inter-American Observatory. A 32-percent signal drop, lasting about 1.2 s, was probably caused by a partially transparent arc of material at a distance of 67,000 km from Neptune. Neptune's arc(s) do not vary smoothly with azimuth, unlike the rings of other Jovian planets.

Plasma and radio waves from Neptune: Source mechamisms and propagation

NASA Technical Reports Server (NTRS)

Menietti, J. Douglas

1994-01-01

The purpose of this project was to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as it flew by Neptune. The study has included data analysis, theoretical and numerical calculations, and ray tracing to determine the possible source mechanisms and locations of the radiation, including the narrowband bursty and smooth components of the Neptune radio emission.

NEPTUNE'S DYNAMIC ATMOSPHERE FROM KEPLER K2 OBSERVATIONS: IMPLICATIONS FOR BROWN DWARF LIGHT CURVE ANALYSES.

PubMed

Simon, Amy A; Rowe, Jason F; Gaulme, Patrick; Hammel, Heidi B; Casewell, Sarah L; Fortney, Jonathan J; Gizis, John E; Lissauer, Jack J; Morales-Juberias, Raul; Orton, Glenn S; Wong, Michael H; Marley, Mark S

2016-02-01

Observations of Neptune with the Kepler Space Telescope yield a 49 day light curve with 98% coverage at a 1 minute cadence. A significant signature in the light curve comes from discrete cloud features. We compare results extracted from the light curve data with contemporaneous disk-resolved imaging of Neptune from the Keck 10-m telescope at 1.65 microns and Hubble Space Telescope visible imaging acquired nine months later. This direct comparison validates the feature latitudes assigned to the K2 light curve periods based on Neptune's zonal wind profile, and confirms observed cloud feature variability. Although Neptune's clouds vary in location and intensity on short and long timescales, a single large discrete storm seen in Keck imaging dominates the K2 and Hubble light curves; smaller or fainter clouds likely contribute to short-term brightness variability. The K2 Neptune light curve, in conjunction with our imaging data, provides context for the interpretation of current and future brown dwarf and extrasolar planet variability measurements. In particular we suggest that the balance between large, relatively stable, atmospheric features and smaller, more transient, clouds controls the character of substellar atmospheric variability. Atmospheres dominated by a few large spots may show inherently greater light curve stability than those which exhibit a greater number of smaller features.

Photochemical Haze Formation in the Atmospheres of Super-Earths and Mini-Neptunes

NASA Technical Reports Server (NTRS)

He, Chao; Hoerst, Sarah M.; Lewis, Nikole K.; Yu, Xinting; Moses, Julianne I.; Kempton, Eliza M.- R.; Marley, Mark S.; McGuiggan, Patricia; Morley, Caroline V.; Valenti, Jeff A.;

Tidal interaction: A possible explanation for geysers and other fluid phenomena in the Neptune-Triton system

NASA Technical Reports Server (NTRS)

Kelly, W. D.; Wood, C. L.

1993-01-01

Discovery of geyser-like plumes on the surface of Triton was a highlight of Voyager 2's passage through the Neptune planetary system. Remarkable as these observations were, they were not entirely without precedent. Considering the confirmed predictions for the 1979 Voyager Jovian passage, it was logical to consider other solar system bodies beside Io where tidal effects could be a significant factor in surface processes. It was our intuition that the Neptune-Triton gravitational bond acting at high inclination to the Neptune equator and the fact that Neptune was a fluid body was significant oblateness would produce tidal and mechanical forces that could be transformed into thermal energy vented on Triton's surface. Prior to the Voyager flyby, others have noted that capture and evolution of Triton's orbit from extreme eccentricity to near circular state today would have resulted in significant tidal heating, but these analysts disregard current day forces. Our calculations indicate that the time varying forces between Neptune-Triton fall midway between those exerted in the Earth-Moon and Jupiter-Io systems, and considering the low level of other energy inputs, this source of internal energy should not be ignored when seeking an explanation for surface activity. In each planet-satellite case, residual or steady-state eccentricity causes time-varying stresses on internal satellite strata. In the case of Jupiter the residual eccentricity is due largely to Galilean satellite interactions, particularly Io-Europa, but in the case of Neptune-Triton, it is the effect of Triton's inclined orbit about an oblate primary.

Reproducibility of the NEPTUNE descriptor-based scoring system on whole-slide images and histologic and ultrastructural digital images.

PubMed

Barisoni, Laura; Troost, Jonathan P; Nast, Cynthia; Bagnasco, Serena; Avila-Casado, Carmen; Hodgin, Jeffrey; Palmer, Matthew; Rosenberg, Avi; Gasim, Adil; Liensziewski, Chrysta; Merlino, Lino; Chien, Hui-Ping; Chang, Anthony; Meehan, Shane M; Gaut, Joseph; Song, Peter; Holzman, Lawrence; Gibson, Debbie; Kretzler, Matthias; Gillespie, Brenda W; Hewitt, Stephen M

2016-07-01

The multicenter Nephrotic Syndrome Study Network (NEPTUNE) digital pathology scoring system employs a novel and comprehensive methodology to document pathologic features from whole-slide images, immunofluorescence and ultrastructural digital images. To estimate inter- and intra-reader concordance of this descriptor-based approach, data from 12 pathologists (eight NEPTUNE and four non-NEPTUNE) with experience from training to 30 years were collected. A descriptor reference manual was generated and a webinar-based protocol for consensus/cross-training implemented. Intra-reader concordance for 51 glomerular descriptors was evaluated on jpeg images by seven NEPTUNE pathologists scoring 131 glomeruli three times (Tests I, II, and III), each test following a consensus webinar review. Inter-reader concordance of glomerular descriptors was evaluated in 315 glomeruli by all pathologists; interstitial fibrosis and tubular atrophy (244 cases, whole-slide images) and four ultrastructural podocyte descriptors (178 cases, jpeg images) were evaluated once by six and five pathologists, respectively. Cohen's kappa for inter-reader concordance for 48/51 glomerular descriptors with sufficient observations was moderate (0.40

Resonance Occupation in the Kuiper Belt: Case Examples of the 5:2 and Trojan Resonances

NASA Astrophysics Data System (ADS)

Chiang, E. I.; Jordan, A. B.; Millis, R. L.; Buie, M. W.; Wasserman, L. H.; Elliot, J. L.; Kern, S. D.; Trilling, D. E.; Meech, K. J.; Wagner, R. M.

2003-07-01

As part of our ongoing Deep Ecliptic Survey (DES) of the Kuiper belt, we report on the occupation of the 1:1 (Trojan), 4:3, 3:2, 7:4, 2:1, and 5:2 Neptunian mean motion resonances (MMRs). The previously unrecognized occupation of the 1:1 and 5:2 MMRs is not easily understood within the standard model of resonance sweeping by a migratory Neptune over an initially dynamically cold belt. Among all resonant Kuiper belt objects (KBOs), the three observed members of the 5:2 MMR discovered by DES possess the largest semimajor axes (a~55.4 AU), the highest eccentricities (e~0.4), and substantial orbital inclinations (i~10deg). Objects (38084) 1999HB12 and possibly 2001KC77 can librate with modest amplitudes of ~90° within the 5:2 MMR for at least 1 Gyr. Their trajectories cannot be explained by close encounters with Neptune alone, given the latter's current orbit. The dynamically hot orbits of such 5:2 resonant KBOs, unlike hot orbits of previously known resonant KBOs, may imply that these objects were preheated to large inclination and large eccentricity prior to resonance capture by a migratory Neptune. Our first discovered Neptunian Trojan, 2001QR322, may not owe its existence to Neptune's migration at all. The trajectory of 2001QR322 is remarkably stable; the object can undergo tadpole-type libration about Neptune's leading Lagrange (L4) point for at least 1 Gyr with a libration amplitude of 24°. Trojan capture probably occurred while Neptune accreted the bulk of its mass. For an assumed albedo of 12%-4%, our Trojan is ~130-230 km in diameter. Model-dependent estimates place the total number of Neptune Trojans resembling 2001QR322 at ~20-60. Their existence helps to rule out violent orbital histories for Neptune.

Initial draft of CSE-UCLA evaluation model based on weighted product in order to optimize digital library services in computer college in Bali

NASA Astrophysics Data System (ADS)

Divayana, D. G. H.; Adiarta, A.; Abadi, I. B. G. S.

2018-01-01

The aim of this research was to create initial design of CSE-UCLA evaluation model modified with Weighted Product in evaluating digital library service at Computer College in Bali. The method used in this research was developmental research method and developed by Borg and Gall model design. The results obtained from the research that conducted earlier this month was a rough sketch of Weighted Product based CSE-UCLA evaluation model that the design had been able to provide a general overview of the stages of weighted product based CSE-UCLA evaluation model used in order to optimize the digital library services at the Computer Colleges in Bali.

On the origin of Triton

NASA Astrophysics Data System (ADS)

Celebonovic, V.

1986-01-01

The origin of Triton, based on the theory of materials under high pressure by Savic and Kasanin (1962, 1965), is described. The mean molecular weight (A) and the volume of one gram mole of Triton's material (V) are evaluated using its values of mass and radius; it is calculated that A = 67 + or - 2 and V = 3 + or - 2. These values are compared with Celebonovic's (1983) model of Neptune; it is observed that the mean molecular weight of Triton is ten times larger than Neptune's. The cause of this large variation in chemical composition is investigated. It is hypothesized that Triton and Neptune formed in different regions of the solar system, and that Triton was ejected from its primordial orbit and was later captured by Neptune.

Magnetostrophic balance in planetary dynamos - Predictions for Neptune's magnetosphere

NASA Technical Reports Server (NTRS)

Curtis, S. A.; Ness, N. F.

1986-01-01

With the purpose of estimating Neptune's magnetic field and its implications for nonthermal Neptune radio emissions, a new scaling law for planetary magnetic fields was developed in terms of externally observable parameters (the planet's mean density, radius, mass, rotation rate, and internal heat source luminosity). From a comparison of theory and observations by Voyager it was concluded that planetary dynamos are two-state systems with either zero intrinsic magnetic field (for planets with low internal heat source) or (for planets with the internal heat source sufficiently strong to drive convection) a magnetic field near the upper bound determined from magnetostrophic balance. It is noted that mass loading of the Neptune magnetosphere by Triton may play an important role in the generation of nonthermal radio emissions.

Voyager radio science observations of neptune and triton.

PubMed

Tyler, G L; Sweetnam, D N; Anderson, J D; Borutzki, S E; Campbell, J K; Eshleman, V R; Gresh, D L; Gurrola, E M; Hinson, D P; Kawashima, N; Kursinski, E R; Levy, G S; Lindal, G F; Lyons, J R; Marouf, E A; Rosen, P A; Simpson, R A; Wood, G E

1989-12-15

The Voyager 2 encounter with the Neptune system included radio science investigations of the masses and densities of Neptune and Triton, the low-order gravitational harmonics of Neptune, the vertical structures of the atmospheres and ionospheres of Neptune and Triton, the composition of the atmosphere of Neptune, and characteristics of ring material. Demanding experimental requirements were met successfully, and study of the large store of collected data has begun. The initial search of the data revealed no detectable effects of ring material with optical depth tau [unknown] 0.01. Preliminary representative results include the following: 1.0243 x 10(26) and 2.141 x 10(22) kilograms for the masses of Neptune and Triton; 1640 and 2054 kilograms per cubic meter for their respective densities; 1355 +/- 7 kilometers, provisionally, for the radius of Triton; and J(2) = 3411 +/- 10(x 10(-6)) and J(4) = -26(+12)(-20)(x10(-6)) for Neptune's gravity field (J>(2) and J(4) are harmonic coefficients of the gravity field). The equatorial and polar radii of Neptune are 24,764 +/- 20 and 24,340 +/- 30 kllometers, respectively, at the 10(5)-pascal (1 bar) pressure level. Neptune's atmosphere was probed to a pressure level of about 5 x 10(5) pascals, and effects of a methane cloud region and probable ammonia absorption below the cloud are evident in the data. Results for the mixing ratios of helium and ammonia are still being investigated; the methane abundance below the clouds is at least 1 percent by volume. Derived temperature-pressure profiles to 1.2 x 10(5) pascals and 78 kelvins (K) show a lapse rate corresponding to "frozen" equilibrium of the para- and ortho-hydrogen states. Neptune's ionosphere exhibits an extended topside at a temperature of 950 +/- 160 K if H(+) is the dominant ion, and narrow ionization layers of the type previously seen at the other three giant planets. Triton has a dense ionosphere with a peak electron concentration of 46 x 10(9) per cubic meter at an altitude of 340 kilometers measured during occultation egress. Its topside plasma temperature is about 80 +/- 16 K if N(2)(+) is the principal ion. The tenuous neutral atmosphere of Triton produced distinct signatures in the occultation data; however, the accuracy of the measurements is limited by uncertainties in the frequency of the spacecraft reference oscillator. Preliminary values for the surface pressure of 1.6 +/- 0.3 pascals and an equivalent isothermal temperature of 48 +/- 5 K are suggested, on the assumption that molecular nitrogen dominates the atmosphere. The radio data may be showing the effects of a thermal inversion near the surface; this and other evidence imply that the Triton atmosphere is controlled by vapor-pressure equilibrium with surface ices, at a temperature of 38 K and a methane mixing ratio of about 10(-4).

The knowledge-attitude dissociation in geriatric education: can it be overcome?

PubMed

Koh, Gerald C H; Merchant, Reshma A; Lim, Wee Shiong; Amin, Zubair

2012-09-01

A knowledge-attitude dissociation often exists in geriatrics where knowledge but not attitudes towards elderly patients improve with education. This study aims to determine whether a holistic education programme incorporating multiple educational strategies such as early exposure, ageing simulation and small group teaching results in improving geriatrics knowledge and attitudes among medical students. We administered the 18-item University of California Los Angeles (UCLA) Geriatric Knowledge Test (GKT) and the Singapore-modified 16-item UCLA Geriatric Attitudes Test (GAT) to 2nd year students of the old curriculum in 2009 (baseline reference cohort, n = 254), and before and after the new module to students of the new curriculum in 2010 (intervention cohort, n = 261), both at the same time of the year. At baseline, between the baseline reference and intervention cohort, there was no difference in knowledge (UCLA-GKT Score: 31.6 vs 33.5, P = 0.207) but attitudes of the intervention group were worse than the baseline reference group (UCLA-GAT Score: 3.53 vs 3.43, P = 0.003). The new module improved both the geriatric knowledge (UCLA-GKT Score: 34.0 vs 46.0, P <0.001) and attitudes (UCLA-GAT Score: 3.43 vs 3.50, P <0.001) of the intervention cohort. A geriatric education module incorporating sound educational strategies improved both geriatric knowledge and attitudes among medical students.

Mapping the stability region of the 3:2 Neptune-Pluto resonance

NASA Technical Reports Server (NTRS)

Levison, H. F.; Stern, S. A.

1993-01-01

Pluto and Charon are most likely the remnants of a large number of objects that existed in the Uranus-Neptune region at early epochs of the solar system. Numerical integrations have shown that, in general, such objects were ejected from the planetary region on timescales of approximately 10(exp 7) years after Neptune and Uranus reached their current masses. It is thought that the Pluto-Charon system survived to current times without being dynamically removed in this way because it is trapped in a set of secular and mean motion resonances with Neptune. The best-known Pluto-Neptune orbit coupling is the 3:2 mean motion resonance discovered almost 30 years ago by C. Cohen and E. Hubbard. These workers showed that the resonance angle, delta is equivalent to 3(lambda(sub P)) - 2(lambda(sub N)) - omega-bar(sub P) where omega-bar(sub P) is the longitude of perihelion of the Pluto-Charon system, and lambda(sub N) and lambda(sub P) are the mean longitude of Neptune and Pluto-Charon respectively, librates about 180 deg with an amplitude, A(sub delta), of 76 deg. A numerical simulation project to map out the stability region of the 3:2 resonance is reported. The results of these simulations are important to understanding whether Pluto's long-term heliocentric stability requires only the 3:2 resonance, or whether it instead requires one or more of the other Pluto-Neptune resonances. Our study also has another important application. By investigating stability timescales as a function of orbital elements, we gain insight into the fraction of orbital phase space which the stable 3:2 resonance occupies. This fraction is directly related to the probability that the Pluto-Charon system (and possibly other small bodies) could have been captured into this resonance.

In-Flight Calibration Processes for the MMS Fluxgate Magnetometers

NASA Technical Reports Server (NTRS)

Bromund, K. R.; Leinweber, H. K.; Plaschke, F.; Strangeway, R. J.; Magnes, W.; Fischer, D.; Nakamura, R.; Anderson, B. J.; Russell, C. T.; Baumjohann, W.;

Uranus and Neptune

NASA Technical Reports Server (NTRS)

Bergstralh, J. T. (Editor)

1984-01-01

A scientific framework within which to plan the Voyager encounters with Uranus and Neptune was sought. Specific objectives were: (1) to assess the current state of knowledge of Uranus and Neptune, their magnetospheres, and their respective systems of satellites and rings (if any), (2) to identify important scientific issues that can be addressed effectively by Voyager, and (3) to provide an opportunity for Voyager investigators to interact with other scientists knowledgeable in the field of physical studies of the Uranian and Neptunian systems.

Spitzer Space Telescope Mid-IR Light Curves of Neptune

NASA Technical Reports Server (NTRS)

Stauffer, John; Marley, Mark S.; Gizis, John E.; Rebull, Luisa; Carey, Sean J.; Krick, Jessica; Ingalls, James G.; Lowrance, Patrick; Glaccum, William; Kirkpatrick, J. Davy;

The vertical distribution and origin of HCN in Neptune's atmosphere

NASA Technical Reports Server (NTRS)

Lellouch, Emmanuel; Romani, Paul N.; Rosenqvist, Jan

1994-01-01

Measurements and modeling of the (3-2) rotational line of hydrogen cyanide at 265.9 GHz in Neptune's atmosphere are presented. High signal-to-noise observations provide information on the HCN vertical distribution in Neptune's stratosphere. The HCN mixing ratio is found to be nearly uniform with height above the condensation level. Best fits occur for HCN distributions that have a slight increase with altitude. A least-squares analysis yields a mixing ratio of (3.2 +/- 0.8)10(exp -10) at 2 mbar and a mean mixing ratio scale height of 250(sup 750)(sub -110) km in the 0.1-3 mbar region. To interpret these results, we developed a photochemical model of HCN. HCN formation is initiated by the reaction between CH3 radicals, produced from methane photochemistry, and N atoms. The primary sink for HCN is condensation, with minor contributions from photolysis and chemical losses. Two possible sources of N atoms are investigated: (1) infall of N escaped from Triton's upper atmosphere, and (2) galactic cosmic ray (GCR) impact on internal N2. Given the uncertainties on (i) the transport and possible ionization of N in Neptune's magnetosphere, and the fate of N(+) reaching Neptune's upper atmosphere and (ii) the N2 mixing ratio in Neptune's deep atmosphere, we suggest that both sources of N atoms may significantly contibute to the formation of HCN.

Welcome to Outer Space

NASA Technical Reports Server (NTRS)

1999-01-01

This video gives a brief history of the Jet Propulsion Laboratory, current missions and what the future may hold. Scenes includes various planets in the solar system, robotic exploration of space, discussions on the Hubble Space Telescope, the source of life, and solar winds. This video was narrated by Jodie Foster. Animations include: close-up image of the Moon; close-up images of the surface of Mars; robotic exploration of Mars; the first mapping assignment of Mars; animated views of Jupiter; animated views of Saturn; and views of a Giant Storm on Neptune called the Great Dark Spot.

Structure and evolution of Uranus and Neptune

NASA Technical Reports Server (NTRS)

Hubbard, W. B.; Macfarlane, J. J.

1980-01-01

Three-layer interior models of Uranus and Neptune with central rocky cores, mantles of water, methane, and ammonia (the 'ices'), and outer envelopes primarily composed of hydrogen and helium are presented. The models incorporate a new H2O equation of state based on experimental data which is considerably 'softer' than previous H2O equations of state. Corrections for interior temperatures approximately 5000 K are included in the models, and the thermal evolution of both planets is investigated using recent heat flow measurements. It is found that the evolutionary considerations are consistent with gravitational field data in supporting models with approximately solar abundances of 'ice' and 'rock'. Evolutionary considerations indicate that initial temperatures and luminosities for Uranus and Neptune were not substantially higher than the present value. Both planets apparently have relatively small approximately 1-2 earth masses) hydrogen-helium envelopes, with Neptune's envelope smaller than Uranus'. A monotonic trend is evident among the Jovian planets: all have central rock-ice cores of approximately 15 earth masses, but with hydrogen-helium envelopes which decrease in mass from Jupiter to Saturn to Uranus to Neptune.

VizieR Online Data Catalog: Broadband photometry of Neptune from K2 (Rowe+, 2017)

NASA Astrophysics Data System (ADS)

Rowe, J. F.; Gaulme, P.; Lissauer, J. J.; Marley, M. S.; Simon, A. A.; Hammel, H. B.; Silva Aguirre, V.; Barclay, T.; Benomar, O.; Boumier, P.; Caldwell, D. A.; Casewell, S. L.; Chaplin, W. J.; Colon, K. D.; Corsaro, E.; Davies, G. R.; Fortney, J. J.; Garcia, R. A.; Gizis, J. E.; Haas, M. R.; Mosser, B.; Schmider, F.-X.

2017-08-01

The K2 C3 field provided the first opportunity to observe the planet Neptune for up to 80 days with short-cadence (1 minute) sampling (the C3 campaign had an actual duration of 69.2 days, limited by on-board data storage). We were awarded sufficient pixel allocation from Guest Observer Programs GO3060 (PI: Rowe) and GO3057 (PI: Gaulme) to continuously monitor Neptune for 49 days. Short-cadence target pixel files were obtained from Mikulski Archive for Space Telescopes (MAST). The Neptune short-cadence subraster was spread across 161 FITS files. Each file contained 1 column of time-series pixel data. Each target pixel file contains observations starting on 2014 November 15 and finishing on 2015 January 18. (1 data file).

ARC-1989-A89-7007

NASA Image and Video Library

1989-08-21

The bright cirrus-like clouds of Neptune change rapidly, often forming and dissipation over periods of several to tens of hours. In this sequence spanning two rotations of Neptune (about 36 hours) Voyager 2 observed cloud evolution in the region around the Great Dark Spot (GDS) at an effective resolution of about 100 km (62 miles) per pixel. The surprisingly rapid changes which occur over the 18 hours separating each panel shows that in this region Neptune's weather is perhaps as dynamic and variable as that of the Earth. However, the scale is immense by our standards--the Earth and the GDS are of similar size -- and in Neptune's frigid atmosphere, where temperatures are as low as 55 degree Kelvin (-360F), the cirrus clouds are composed of frozen methane rather than Earth's crystalse of water ice.

H2 S3(1) and S4(1) transitions in the atmospheres of Neptune and Uranus - Observations and analysis

NASA Technical Reports Server (NTRS)

Smith, Wm. Hayden; Baines, Kevin H.

1990-01-01

The present observational results for Neptune's S3(1) and S4(1) H2 lines show the former line's measured equivalent width to be the same as for this feature in Uranus, repeating the equality already established between the two planets for the latter feature. It is also noted that the observed ratio of the H2 S3(0)/S3(1) lines for Neptune's atmosphere is reproduced by models belonging to the family of models created by Baines and Smith (1990); by comparison with the earlier Uranus models of Baines and Bergstrahl (1986), the greater continuum absorption of Neptune is responsible for the increased S3(0)/S3(1) line ratio near 0.82 microns.

The discoveries of Neptune and Triton.

NASA Astrophysics Data System (ADS)

Moore, P.

The story of the tracking-down of Neptune has been told many times, but even today there are still discrepancies in the various accounts, to say nothing of conflicting opinions. To some people, John Couch Adams is a shining hero and George Biddell Airy a black villain; to others it is Le Verrier who is the hero, and Adams an unimportant member of the supporting cast. Of course, all this is absurd. In the author's view, the true discoverers of Neptune were Johann Gottfried Galle and Heinrich D'Arrest.

Working group for planetary system nomenclature

NASA Technical Reports Server (NTRS)

1993-01-01

Most of the activity of the Working Group and Task Group of the IAU during these three years has been centered on the nomenclature of Neptune's satellites and rings as revealed by the Voyager spacecraft. The emphasis is now shifting to Venus, in preparation for the detailed radar mapping of that planet begun by the Magellan spacecraft in August 1990. Approval has been asked for nomenclature of the Earth's moon, Venus, Mars, and Triton features as well as 4 other Neptune satellites and three Neptune rings.

First generation atmospheric probes (10-BARS) for Uranus and Neptune

NASA Technical Reports Server (NTRS)

Sullivan, R. J.; Waters, J. I.; Dunkin, J. H.

1972-01-01

The feasibility of atmospheric entry probe missions to Uranus and Neptune is studied, and preliminary estimates of missions parameters are presented. Most of the study results are applicable, with only minor modifications, to Uranus-Neptune entry probes included on any type of outer planet mission. Trajectory dynamics is discussed first because it imposes some important constraints upon the total time available for data transmission, which in turn determines the descent rate. This last quantity provides important information for the design of the scientific payload.

Service Learning Course in Which Undergraduates and Middle School Students Investigate Levels of Pathogen Indicating Bacteria in Beach Sand

NASA Astrophysics Data System (ADS)

Imamura, G.; Mika, K.; Lin, T.; Lee, C.; Lin, C.; Jay, J.

2007-12-01

Service-learning is a pedagogy that combines academic rigor with activities that address human and community needs. Over the past three years, we have developed a service-learning course that involves UCLA students working with 6th graders in an economically disadvantaged neighborhood to address issues of environmental science and health. This past year UCLA students conducted a research project in collaboration with a middle school class to investigate levels of pathogen-indicating organisms in beach sand near the Santa Monica pier. All students were taught necessary methods in class by the UCLA professor, and then met at the field site. Fieldwork involved collection of water and sand samples from various locations, extraction of bacteria from sand by shaking with buffer and decanting, and addition of sample to growth media that allow quantification of two organisms, Escherichia coli and enterococci. These organisms are typically used to indicate fecal contamination of water. Methods were straightforward and were accomplished by the 6th graders with only modest supervision by the UCLA students. Results showed extremely high levels of pathogen indicating organisms in the vicinity of a diverted stormdrain, indicating a continuing problem with the diversion. Levels decreased with distance away from the stormdrain, indicating migration of the organisms from the site of the diversion. UCLA students then visited the sixth grade classroom to help the sixth graders create Powerpoint posters including statement of hypotheses, graphs of the results, pictures of the entire process, and conclusions. Middle school students then visited UCLA to tour the campus and present their posters at a poster session hosted by the Center for Embedded Networked Sensing at UCLA. Desired outcomes at the 6th grade level included: 1) increased interest in science; 2) greater knowledge of and interest in attending college; and 3) enhanced knowledge of and feeling of political empowerment concerning environmental health issues. Outcomes for the UCLA students included: 1) gains in learning through the action of teaching; 2) awareness of education justice issues in Los Angeles; and 3) enhanced feeling of personal commitment to community and political advocacy work.

Observations of Uranus and Neptune in Spanish Telescopes: Calar Alto/PlanetCam, WHT/Ingrid y GTC/Osiris

NASA Astrophysics Data System (ADS)

Hueso, R.; Sánchez-Lavega, A.; Ordonez-Etxeberria, I.; Rojas, J. F.; Pérez-Hoyos, S.; Mendikoa, I.

2017-03-01

The astronomical observation of the atmospheres of Uranus and Neptune poses unique challenges. Both planets are relatively dimm objects (visual magnitude of +5.3 and +7.7) and have small angular sizes (3.7” and 2.4” at opposition). Both worlds have atmospheres that are very dynamic, specially Neptune. These atmospheres are dominated by intense zonal winds that reach 450 m/s and where seasonal evolution changes the band patterns present in these planets. Thanks to the atmospheric methane gas, when observing Uranus and Neptune in near infrared wavelengths their upper clouds become well contrasted and bright and observations at different methane absorption bands allow to sample the atmosphere at different vertical layers. Both worlds are subject to the development of bright cloud patterns, some times of convective origin and whose activity can extend over weeks to several months or years. In the last few years we have surveyed the atmospheric activity of Uranus and Neptune with instruments able to improve the spatial resolution of the images beyond the limits impose by the atmospheric seeing. We use the Lucky Imaging technique (fast observation of several short-exposure frames combined with automatic selection of best frames and coregistration for stacking). We present image observations of Uranus and Neptune obtained with the instruments: OSIRIS at Grantecan as well as the AstraLux and PlanetCam UPV/EHU cameras on the 2.2m telescope at Calar Alto observatory. These observations are compared with other observations acquired by amateur astronomers able to obtain resolve cloud features in Uranus and Neptune. We compare these observations with images acquired with Adaptive Optics instruments at the William Herschel with the NAOMI+Ingrid instruments and Keck II and with Hubble Space Telescope images. We show the importance of surveying the atmospheric activity of these planets with a variety of telescopes. Two science cases are presented: The study of convective storms in Uranus in 2014 and the study of bright non convective features in Neptune in 2015.

Magnetic fields at neptune.

PubMed

Ness, N F; Acuña, M H; Burlaga, L F; Connerney, J E; Lepping, R P; Neubauer, F M

1989-12-15

The National Aeronautics and Space Administration Goddard Space Flight Center-University of Delaware Bartol Research Institute magnetic field experiment on the Voyager 2 spacecraft discovered a strong and complex intrinsic magnetic field of Neptune and an associated magnetosphere and magnetic tail. The detached bow shock wave in the supersonic solar wind flow was detected upstream at 34.9 Neptune radii (R(N)), and the magnetopause boundary was tentatively identified at 26.5 R(N) near the planet-sun line (1 R(N) = 24,765 kilometers). A maximum magnetic field of nearly 10,000 nanoteslas (1 nanotesla = 10(-5) gauss) was observed near closest approach, at a distance of 1.18 R(N). The planetary magnetic field between 4 and 15 R(N) can be well represented by an offset tilted magnetic dipole (OTD), displaced from the center of Neptune by the surprisingly large amount of 0.55 R(N) and inclined by 47 degrees with respect to the rotation axis. The OTD dipole moment is 0.133 gauss-R(N)(3). Within 4 R(N), the magnetic field representation must include localized sources or higher order magnetic multipoles, or both, which are not yet well determined. The obliquity of Neptune and the phase of its rotation at encounter combined serendipitously so that the spacecraft entered the magnetosphere at a time when the polar cusp region was directed almost precisely sunward. As the spacecraft exited the magnetosphere, the magnetic tail appeared to be monopolar, and no crossings of an imbedded magnetic field reversal or plasma neutral sheet were observed. The auroral zones are most likely located far from the rotation poles and may have a complicated geometry. The rings and all the known moons of Neptune are imbedded deep inside the magnetosphere, except for Nereid, which is outside when sunward of the planet. The radiation belts will have a complex structure owing to the absorption of energetic particles by the moons and rings of Neptune and losses associated with the significant changes in the diurnally varying magnetosphere configuration. In an astrophysical context, the magnetic field of Neptune, like that of Uranus, may be described as that of an "oblique" rotator.

W3MAMCAT: a world wide web based tool for mammillary and catenary compartmental modeling and expert system distinguishability.

PubMed

Russell, Solomon; Distefano, Joseph J

2006-07-01

W(3)MAMCAT is a new web-based and interactive system for building and quantifying the parameters or parameter ranges of n-compartment mammillary and catenary model structures, with input and output in the first compartment, from unstructured multiexponential (sum-of-n-exponentials) models. It handles unidentifiable as well as identifiable models and, as such, provides finite parameter interval solutions for unidentifiable models, whereas direct parameter search programs typically do not. It also tutorially develops the theory of model distinguishability for same order mammillary versus catenary models, as did its desktop application predecessor MAMCAT+. This includes expert system analysis for distinguishing mammillary from catenary structures, given input and output in similarly numbered compartments. W(3)MAMCAT provides for universal deployment via the internet and enhanced application error checking. It uses supported Microsoft technologies to form an extensible application framework for maintaining a stable and easily updatable application. Most important, anybody, anywhere, is welcome to access it using Internet Explorer 6.0 over the internet for their teaching or research needs. It is available on the Biocybernetics Laboratory website at UCLA: www.biocyb.cs.ucla.edu.

Neptune

NASA Image and Video Library

1999-10-14

This photograph of Neptune shows three of the features that NASA Voyager 2 has been photographing during recent weeks. At the north is the Great Dark Spot, accompanied by bright, white clouds that undergo rapid changes in appearance.

Throwing Icebergs at White Dwarfs

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2017-08-01

Where do the metals come from that pollute the atmospheres of many white dwarfs? Close-in asteroids may not be the only culprits! A new study shows that distant planet-size and icy objects could share some of the blame.Pollution ProblemsArtists impression of rocky debris lying close around a white dwarf star. [NASA/ESA/STScI/G. Bacon]When a low- to intermediate-mass star reaches the end of its life, its outer layers are blown off, leaving behind its compact core. The strong gravity of this white dwarf causes elements heavier than hydrogen and helium to rapidly sink to its center in a process known as sedimentation, leaving an atmosphere that should be free of metallic elements.Therefore its perhaps surprising that roughly 2550% of all white dwarfs are observed to have atmospheric pollution by heavy elements. The short timescales for sedimentation suggest that these elements were added to the white dwarf recently but how did they get there?Bringing Ice InwardIn the generally accepted theory, pre-existing rocky bodies or an orbiting asteroid belt survive the stars evolution, later accreting onto the final white dwarf. But this scenario doesnt explain a few observations that suggest white dwarfs might be accreting larger planetary-size bodies and bodies with ices and volatile materials.Dynamical evolution of a Neptune-like planet (a) and a Kuiper belt analog object (b) in wide binary star systems. Both have large eccentricity excitations during the white dwarf phase. [Stephan et al. 2017]How might you get large or icy objects which would begin on very wide orbits close enough to a white dwarf to become disrupted and accrete? Led by Alexander Stephan, a team of scientists at UCLA now suggest that the key is for the white dwarf to be in a binary system.Influence of a CompanionIn the authors model, the white-dwarf progenitor is orbited by both a distant stellar companion (a common occurrence) and a number of large potential polluters, which could have masses between that of a large asteroid up to several times the mass of Jupiter. These potential polluters have very wide orbits that allow them to maintain ice and volatile materials.At the end of the progenitors lifetime it loses a significant amount of mass, causing the orbits of the surviving objects in the system to expand. After this stage, the stellar companion gravitationally perturbs the potential polluters onto extremely eccentric orbits, bringing these massive and long-period objects close enough accrete onto what is now the white dwarf.The Need for ObservationsThe likelihood distributions for orbital parameters of the systems that result in white dwarfs polluted by Neptune-like planets and Kuiper-belt-analog objects. The black arrows mark the parameters for one of the few observed systems, WD 1425+540, for comparison. [Stephan et al. 2017]By running large Monte Carlo simulations, Stephan and collaborators demonstrate that this scenario can successfully produce accretion of both Neptune-like planets and Kuiper-belt-analog objects. Their simulation results indicate that 1% of all white dwarfs should accrete Neptune-like planets, and 7.5% of all white dwarfs should accrete Kuiper-belt-analog objects.While these fractions are broadly consistent with observations, its hard to say with certainty whether this model is correct, as observations are scant. Only 200 polluted white dwarfs have been observed, and of these, only 15 have had detailed abundance measurements made. Next steps for understanding white-dwarf pollution certainly must includegathering more observations of polluted white dwarfs and establishing the statistics of what is polluting them.CitationAlexander P. Stephan et al 2017 ApJL 844 L16. doi:10.3847/2041-8213/aa7cf3

First Atmosphere Characterization of the Benchmark Exo-Neptune WASP-107b

NASA Astrophysics Data System (ADS)

Kreidberg, Laura

2016-10-01

WASP-107b is a newly announced transiting planet that is the highest signal-to-noise target for transmission spectroscopy discovered in the last decade, thanks to its low surface gravity and small, bright host star. The planet is in the intriguing transition region between ice and gas giants, with a mass comparable to Neptune and a radius similar to Jupiter. Relative to other benchmark systems, WASP-107b has a cool equilibrium temperature (780 K), where methane and water are both expected to be abundant. The planet therefore provides a unique opportunity for spectroscopic characterization of carbon and oxygen chemistry. With its large expected signal, WASP-107b also provides an excellent laboratory to study aerosol formation. The features are so large that even if thick clouds/haze are present at very high altitudes (0.1 mbar), it will still be possible to detect absorption features peeking out above them. Here we propose a reconnaissance observation of a single transit of WASP-107b. This measurement will vet the planet's atmosphere composition and test for the presence of aerosols so that the community can decide on the best follow-up strategy for this exciting system.

Progress on the Cluster Mission

NASA Technical Reports Server (NTRS)

Kivelson, Margaret; Khurana, Krishan; Acuna, Mario (Technical Monitor)

2002-01-01

Prof M. G. Kivelson and Dr. K. K. Khurana (UCLA (University of California, Los Angeles)) are co-investigators on the Cluster Magnetometer Consortium (CMC) that provided the fluxgate magnetometers and associated mission support for the Cluster Mission. The CMC designated UCLA as the site with primary responsibility for the inter-calibration of data from the four spacecraft and the production of fully corrected data critical to achieving the mission objectives. UCLA will also participate in the analysis and interpretation of the data. The UCLA group here reports its excellent progress in developing fully intra-calibrated data for large portions of the mission and an excellent start in developing inter-calibrated data for selected time intervals, especially extended intervals in August, 2001 on which a workshop held at ESTEC in March, 2002 focused. In addition, some scientific investigations were initiated and results were reported at meetings.

The librarian as research informationist: a case study.

PubMed

Federer, Lisa

2013-10-01

How can an embedded research informationist add value to the scientific output of research teams? The University of California-Los Angeles (UCLA) Louise M. Darling Biomedical Library is an academic health sciences library serving the clinical, educational, and research needs of the UCLA community. A grant from the National Library of Medicine funded a librarian to join a UCLA research team as an informationist. The informationist meets regularly with the research team and provides guidance related to data management, preservation, and other information-related issues. Early results suggest that the informationist's involvement has influenced the team's data gathering, storage, and curation methods. The UCLA Library has also changed the librarian's title to research informationist to reflect the new activities that she performs. The research informationist role provides an opportunity for librarians to become effective members of research teams and improve research output.

Clinical experiences utilizing wireless remote control and an ASP model backup archive for a disaster recovery event

NASA Astrophysics Data System (ADS)

Liu, Brent J.; Documet, Luis; Documet, Jorge; Huang, H. K.; Muldoon, Jean

2004-04-01

An Application Service Provider (ASP) archive model for disaster recovery for Saint John"s Health Center (SJHC) clinical PACS data has been implemented using a Fault-Tolerant Archive Server at the Image Processing and Informatics Laboratory, Marina del Rey, CA (IPIL) since mid-2002. The purpose of this paper is to provide clinical experiences with the implementation of an ASP model backup archive in conjunction with handheld wireless technologies for a particular disaster recovery scenario, an earthquake, in which the local PACS archive and the hospital are destroyed and the patients are moved from one hospital to another. The three sites involved are: (1) SJHC, the simulated disaster site; (2) IPIL, the ASP backup archive site; and (3) University of California, Los Angeles Medical Center (UCLA), the relocated patient site. An ASP backup archive has been established at IPIL to receive clinical PACS images daily using a T1 line from SJHC for backup and disaster recovery storage. Procedures were established to test the network connectivity and data integrity on a regular basis. In a given disaster scenario where the local PACS archive has been destroyed and the patients need to be moved to a second hospital, a wireless handheld device such as a Personal Digital Assistant (PDA) can be utilized to route images to the second hospital site with a PACS and reviewed by radiologists. To simulate this disaster scenario, a wireless network was implemented within the clinical environment in all three sites: SJHC, IPIL, and UCLA. Upon executing the disaster scenario, the SJHC PACS archive server simulates a downtime disaster event. Using the PDA, the radiologist at UCLA can query the ASP backup archive server at IPIL for PACS images and route them directly to UCLA. Implementation experiences integrating this solution within the three clinical environments as well as the wireless performance are discussed. A clinical downtime disaster scenario was implemented and successfully tested. Radiologists were able to successfully query PACS images utilizing a wireless handheld device from the ASP backup archive at IPIL and route the PACS images directly to a second clinical site at UCLA where they and the patients are located at that time. In a disaster scenario, using a wireless device, radiologists at the disaster health care center can route PACS data from an ASP backup archive server to be reviewed in a live clinical PACS environment at a secondary site. This solution allows Radiologists to use a wireless handheld device to control the image workflow and to review PACS images during a major disaster event where patients must be moved to a secondary site.

The Moons of Uranus, Neptune and Pluto.

ERIC Educational Resources Information Center

Brown, Robert Hamilton; Cruikshank, Dale P.

1985-01-01

In preparation for the Voyager flybys in 1989, the pace of ground-based investigations of the moons of Uranus, Neptune, and Pluto has quickened considerably. Information derived from these investigations is presented. (JN)

Orbits of the inner satellites of Neptune

NASA Astrophysics Data System (ADS)

Brozovic, Marina; Showalter, Mark R.; Jacobson, Robert Arthur; French, Robert S.; de Pater, Imke; Lissauer, Jack

2018-04-01

We report on the numerically integrated orbits of seven inner satellites of Neptune, including S/2004 N1, the last moon of Neptune to be discovered by the Hubble Space Telescope (HST). The dataset includes Voyager imaging data as well as the HST and Earth-based astrometric data. The observations span time period from 1989 to 2016. Our orbital model accounts for the equatorial bulge of Neptune, perturbations from the Sun and the planets, and perturbations from Triton. The initial orbital integration assumed that the satellites are massless, but the residuals improved significantly as the masses adjusted toward values that implied that the density of the satellites is in the realm of 1 g/cm3. We will discuss how the integrated orbits compare to the precessing ellipses fits, mean orbital elements, current orbital uncertainties, and the need for future observations.

The near real time image navigation of pictures returned by Voyager 2 at Neptune

NASA Technical Reports Server (NTRS)

Underwood, Ian M.; Bachman, Nathaniel J.; Taber, William L.; Wang, Tseng-Chan; Acton, Charles H.

1990-01-01

The development of a process for performing image navigation in near real time is described. The process was used to accurately determine the camera pointing for pictures returned by the Voyager 2 spacecraft at Neptune Encounter. Image navigation improves knowledge of the pointing of an imaging instrument at a particular epoch by correlating the spacecraft-relative locations of target bodies in inertial space with the locations of their images in a picture taken at that epoch. More than 8,500 pictures returned by Voyager 2 at Neptune were processed in near real time. The results were used in several applications, including improving pointing knowledge for nonimaging instruments ('C-smithing'), making 'Neptune, the Movie', and providing immediate access to geometrical quantities similar to those traditionally supplied in the Supplementary Experiment Data Record.

In-Flight Calibration Processes for the MMS Fluxgate Magnetometers

NASA Astrophysics Data System (ADS)

Bromund, K. R.; Leinweber, H. K.; Plaschke, F.; Strangeway, R. J.; Magnes, W.; Fischer, D.; Nakamura, R.; Anderson, B. J.; Russell, C. T.; Baumjohann, W.; Chutter, M.; Torbert, R. B.; Le, G.; Slavin, J. A.; Kepko, L.

2015-12-01

The calibration effort for the Magnetospheric Multiscale Mission (MMS) Analog Fluxgate (AFG) and Digital Fluxgate (DFG) magnetometers is a coordinated effort between three primary institutions: University of California, Los Angeles (UCLA); Space Research Institute, Graz, Austria (IWF); and Goddard Space Flight Center (GSFC). Since the successful deployment of all 8 magnetometers on 17 March 2015, the effort to confirm and update the ground calibrations has been underway during the MMS commissioning phase. The in-flight calibration processes evaluate twelve parameters that determine the alignment, orthogonalization, offsets, and gains for all 8 magnetometers using algorithms originally developed by UCLA and the Technical University of Braunschweig and tailored to MMS by IWF, UCLA, and GSFC. We focus on the processes run at GSFC to determine the eight parameters associated with spin tones and harmonics. We will also discuss the processing flow and interchange of parameters between GSFC, IWF, and UCLA. IWF determines the low range spin axis offsets using the Electron Drift Instrument (EDI). UCLA determines the absolute gains and sensor azimuth orientation using Earth field comparisons. We evaluate the performance achieved for MMS and give examples of the quality of the resulting calibrations.

Discovery of a Bright Equatorial Storm on Neptune

NASA Astrophysics Data System (ADS)

Molter, E. M.; De Pater, I.; Alvarez, C.; Tollefson, J.; Luszcz-Cook, S.

2017-12-01

Images of Neptune, taken with the NIRC2 instrument during testing of the new Twilight Zone observing program at Keck Observatory, revealed an extremely large bright storm system near Neptune's equator. The storm complex is ≈9,000 km across and brightened considerably between June 26 and July 2. Historically, very bright clouds have occasionally been seen on Neptune, but always in the midlatitude regions between ≈15° and ≈60° North or South. Voyager and HST observations have shown that cloud features large enough to dominate near-IR photometry are often "companion" clouds of dark anti-cyclonic vortices similar to Jupiter's Great Red Spot, interpreted as orographic clouds. In the past such clouds and their coincident dark vortices often persisted for one up to several years. However, the cloud complex we detect is unique: never before has a bright cloud been seen at, or so close to, the equator. The discovery points to a drastic departure in the dynamics of Neptune's atmosphere from what has been observed for the past several decades. Detections of the complex in multiple NIRC2 filters allows radiative transfer modeling to constrain the cloud's altitude and vertical extent.

Conceptual design of a pulsed-power accelerator optimized for megajoule-class 1-TPa dynamic-material-physics experiments

DOE PAGES

Stygar, William A.; Reisman, David B.; Stoltzfus, Brian S.; ...

2016-07-07

In this study, we have developed a conceptual design of a next-generation pulsed-power accelerator that is optmized for driving megajoule-class dynamic-material-physics experiments at pressures as high as 1 TPa. The design is based on an accelerator architecture that is founded on three concepts: single-stage electrical-pulse compression, impedance matching, and transit-time-isolated drive circuits. Since much of the accelerator is water insulated, we refer to this machine as Neptune. The prime power source of Neptune consists of 600 independent impedance-matched Marx generators. As much as 0.8 MJ and 20 MA can be delivered in a 300-ns pulse to a 16-mΩ physics load;more » hence Neptune is a megajoule-class 20-MA arbitrary waveform generator. Neptune will allow the international scientific community to conduct dynamic equation-of-state, phase-transition, mechanical-property, and other material-physics experiments with a wide variety of well-defined drive-pressure time histories. Because Neptune can deliver on the order of a megajoule to a load, such experiments can be conducted on centimeter-scale samples at terapascal pressures with time histories as long as 1 μs.« less

Neptune Aerocapture Systems Analysis

NASA Technical Reports Server (NTRS)

Lockwood, Mary Kae

2004-01-01

A Neptune Aerocapture Systems Analysis is completed to determine the feasibility, benefit and risk of an aeroshell aerocapture system for Neptune and to identify technology gaps and technology performance goals. The high fidelity systems analysis is completed by a five center NASA team and includes the following disciplines and analyses: science; mission design; aeroshell configuration screening and definition; interplanetary navigation analyses; atmosphere modeling; computational fluid dynamics for aerodynamic performance and database definition; initial stability analyses; guidance development; atmospheric flight simulation; computational fluid dynamics and radiation analyses for aeroheating environment definition; thermal protection system design, concepts and sizing; mass properties; structures; spacecraft design and packaging; and mass sensitivities. Results show that aerocapture can deliver 1.4 times more mass to Neptune orbit than an all-propulsive system for the same launch vehicle. In addition aerocapture results in a 3-4 year reduction in trip time compared to all-propulsive systems. Aerocapture is feasible and performance is adequate for the Neptune aerocapture mission. Monte Carlo simulation results show 100% successful capture for all cases including conservative assumptions on atmosphere and navigation. Enabling technologies for this mission include TPS manufacturing; and aerothermodynamic methods and validation for determining coupled 3-D convection, radiation and ablation aeroheating rates and loads, and the effects on surface recession.

Voyager 2 Uranus and Neptune targeting

NASA Technical Reports Server (NTRS)

Gray, D. L.; Cesarone, R. J.; Van Allen, R. E.

1982-01-01

Targeting strategies are developed for the Voyager 2 flybys of Uranus and Neptune/Triton. The need to maximize science return, conserve propellant, and maintain spacecraft safety presents a challenge, given the difficulty in estimating the spacecraft orbit relative to these outer planets. Expected propellant usage, science return, and targeting complexity are presented for each targeting strategy. For the dual encounter of Neptune and its satellite Triton, split targeting conditions are proposed to fix the most important conditions at each body, and thus minimize science losses resulting from Triton ephemeris uncertainties.

Absolute spectrophotometry of Titan, Uranus, and Neptune 3500-10,500 A

NASA Technical Reports Server (NTRS)

Neff, J. S.; Humm, D. C.; Bergstralh, J. T.; Cochran, A. L.; Cochran, W. D.; Barker, E. S.; Tull, R. G.

1984-01-01

The present absolute measurements of Titan, Uranus and Neptune geometric albedo spectra in the 3500-10,500 A range have a resolution of about 7 A, together with high SNR, in virtue of the exceptional effeciency of the spectrograph and Reticon detector employed. The high precision and spectral resolution of the data, which are in excellent agreement with the Uranus albedo measurements of Lockwood et al. (1983), make possible quantitative measurements of the effects of Raman scattering by H2 in the Uranus and Neptune atmospheres.

Mary S. Easton Center of Alzheimer’s Disease Research at UCLA: Advancing the Therapeutic Imperative

PubMed Central

Cummings, Jeffrey L.; Ringman, John; Metz, Karen

2010-01-01

The Mary S. Easton Center for Alzheimer’s Disease Research (UCLA-Easton Alzheimer’s Center) is committed to the “therapeutic imperative” and is devoted to finding new treatments for Alzheimer’s disease (AD) and to developing technologies (biomarkers) to advance that goal. The UCLA-Easton Alzheimer’s Center has a continuum of research and research-related activities including basic/foundational studies of peptide interactions; translational studies in transgenic animals and other animal models of AD; clinical research to define the phenotype of AD, characterize familial AD, develop biomarkers, and advance clinical trials; health services and outcomes research; and active education, dissemination, and recruitment activities. The UCLA-Easton Alzheimer’s Center is supported by the National Institutes on Aging, the State of California, and generous donors who share our commitment to developing new therapies for AD. The naming donor (Jim Easton) provided substantial funds to endow the center and to support projects in AD drug discovery and biomarker development. The Sidell-Kagan Foundation supports the Katherine and Benjamin Kagan Alzheimer’s Treatment Development Program, and the Deane F. Johnson Alzheimer’s Research Foundation supports the Deane F. Johnson Center for Neurotherapeutics at UCLA. The John Douglas French Alzheimer’s Research Foundation provides grants to junior investigators in critical periods of their academic development. The UCLA-Easton Alzheimer’s Center partners with community organizations including the Alzheimer’s Association California Southland Chapter and the Leeza Gibbons memory Foundation. Collaboration with pharmaceutical companies, biotechnology companies, and device companies is critical to developing new therapeutics for AD and these collaborations are embraced in the mission of the UCLA-Easton Alzheimer’s Center. The Center supports excellent senior investigators and serves as an incubator for new scientists, agents, models, technologies and concepts that will significantly influence the future of AD treatment and AD research. PMID:20110588

Student Health Advocates: A Program for Extending Health Services to UCLA Students

ERIC Educational Resources Information Center

Habibi, Michele; Levine, Eileen Nebel

1976-01-01

The article describes and evaluates the pilot Student Health Advocate Program of UCLA, a peer-staffed, general health outreach program designed to provide care for students' minor medical and emotional concerns. (MB)

An Analysis of Neptune's Stratospheric Haze Using High-Phase-Angle Voyager Images

NASA Technical Reports Server (NTRS)

Moses, Julianne I.; Rages, Kathy; Pollack, James B.

1995-01-01

We have inverted high-phase-angle Voyager images of Neptune to determine the atmospheric extinction coefficient as a function of altitude and the scattering phase function at a reference altitude. Comparisons between theoretical model and observations help separate the contributions from molecular Rayleigh and aerosol scattering and help determine the variation of the aerosol size, concentration, and scattering properties with altitude. Further comparisons between models and data allow us to place constraints on the location and composition of the hazes, the concentration and downward flux of certain condensible hydrocarbon gases, the eddy diffusion coefficient in the lower stratosphere, and the thermal profile in parts of Neptune's stratosphere. We find that a distinct stratospheric haze layer exists near 12(sub -1, sup +1) mbar in Neptune's lower stratosphere, most probably due to condensed ethane. The derived stratospheric haze production rate of 1.0(sub -0.3, sup +0.2) x 10(exp -15) g cm(exp -2) sec(exp -1) is substantially lower than photochemical model predictions. Evidence for hazes at higher altitudes also exists. Unlike the situation on Uranus, large particles (0.08-0.11 microns) may be present at high altitudes on Neptune (e.g., near 0.5 mbar), well above the region in which we expect the major hydrocarbon species to condense. Near 28 mbar, the mean particle size is about 0.13(sub -0.02, sup +0.02) microns with a concentration of 5(sub -3, sup +3) particles cm(exp -3). The cumulative haze extinction optical depth above 15 mbar in the clear filter is approx. 3 x 10(exp -3), and much of this extinction is due to scattering rather than absorption; thus, if our limb-scan sites are typical, the hazes cannot account for the stratospheric temperature inversion on Neptune and may not contribute significantly to atmospheric heating. We compare the imaging results with the results from other observations, including those of the Voyager Photopolarimeter Subsystem, and discuss differences between Neptune and Uranus.

50 CFR 217.176 - Applications for Letters of Authorization.

Code of Federal Regulations, 2011 CFR

2011-10-01

... Maintenance of the Neptune Liquefied Natural Gas Facility Off Massachusetts § 217.176 Applications for Letters.... Citizen (as defined by § 216.103) conducting the activity identified in § 217.170(a) (i.e., Neptune) must...

The clouds and winds of Neptune

NASA Astrophysics Data System (ADS)

Beebe, R.

1992-04-01

The atmospheric features of Neptune are described based on the images from Voyager 2 with comparisons made to the atmosphere of Uranus. Specific attention is given to the clear atmosphere's methane content and lack of the smog associated with Uranus. Neptune absorbs only a small amount of energy from sunlight and radiates about 2.7 times as much as it absorbs. The mechanisms that keep Neptune's atmosphere free of smog are thought to be upwelling enhanced by an outward heat flow and melting ice. The Voyager photographs show streaks of white clouds indicating strong winds and probably white ice in the upper atmosphere. The Great Dark Spot and a small triangular cloud are described in terms of their periods of rotation, and the wind speed is discussed in terms of cloud variations. The Great Dark Spot drifted equatorward during the observational period, and the drift yields some important clues regarding the nature of the Neptunian atmosphere and climate.

Aerocapture Systems Analysis for a Neptune Mission

NASA Technical Reports Server (NTRS)

Lockwood, Mary Kae; Edquist, Karl T.; Starr, Brett R.; Hollis, Brian R.; Hrinda, Glenn A.; Bailey, Robert W.; Hall, Jeffery L.; Spilker, Thomas R.; Noca, Muriel A.; O'Kongo, N.

2006-01-01

A Systems Analysis was completed to determine the feasibility, benefit and risk of an aeroshell aerocapture system for Neptune and to identify technology gaps and technology performance goals. The systems analysis includes the following disciplines: science; mission design; aeroshell configuration; interplanetary navigation analyses; atmosphere modeling; computational fluid dynamics for aerodynamic performance and aeroheating environment; stability analyses; guidance development; atmospheric flight simulation; thermal protection system design; mass properties; structures; spacecraft design and packaging; and mass sensitivities. Results show that aerocapture is feasible and performance is adequate for the Neptune mission. Aerocapture can deliver 1.4 times more mass to Neptune orbit than an all-propulsive system for the same launch vehicle and results in a 3-4 year reduction in trip time compared to all-propulsive systems. Enabling technologies for this mission include TPS manufacturing; and aerothermodynamic methods for determining coupled 3-D convection, radiation and ablation aeroheating rates and loads.

77 FR 25743 - Notice of Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2012-05-01

... no additional claimants come forward. DATES: Representatives of any Indian tribe that believes it has... after that date if no additional claimants come forward. The Fowler Museum at UCLA is responsible for...

Endogeneous sources: atmospheric organic syntheses, tholins and ground trust

NASA Astrophysics Data System (ADS)

Raulin, F.; Bernard, J.; Coll, P.; Nna Mvondo, D.; Ramirez, S.; Navarro-Gonzalez, R.

From the many simulation experiments which have been carried out for the last 50 years on gas phase organic synthesis but also from several theoretical modeling works, it is clear today that in situ production of organic molecules in planetary atmosphere is efficient only if the starting atmosphere is chemically reduced. In that case many simple organics can be produced like formaldehyde, (HCHO), hydrogen cyanide (HCN), cyanoacetylene (HC3N) and other nitriles, but also more complex refractory organics - usually named "tholins" - are obtained. Those tholins are still of very poorly known composition, but are of great exobiological interest since they are the precursors of many compounds of biological interest, in particular amino acids, purines and pyrimidines bases. How realistic are those experimental as well as theoretical simulations? The many planetary data which have been obtained until now on the so diversified planetary atmospheres of the solar system provide a fantastic opportunity to answer such question and validate the laboratory data with "ground trust". Indeed, at the exception of the Earth atmosphere (in which Life is the essential source of organics), any organic compound has been detected in the inner planets. On the contrary, all the outer planets, from Jupiter to Neptune (and even Pluto) involve organic chemical processes, through the chemistry of their atmosphere, and methane photochemistry. They are also present in the dense atmosphere of Titan, the largest satellite of Saturn, (in the gas and aerosol phases), in the much thinner atmosphere of Triton, the largest satellite of Neptune (mainly in the solid phase, on its surface), and on the surface of many of the other satellites of the outer planets. Thus, although we have so far no real direct evidence for this assumption, laboratory data strongly suggest that extraterrestrial organic chemistry systematically involves tholins-like matter. The different aspects of extraterrestrial atmospheric organic chemistry will be presented and discussed, on the basis of recent laboratory data, in particular from simulation experiments related to oxidized and reduced atmospheres and planetary observations.

Neptune Hot South Pole

NASA Image and Video Library

2007-09-18

These thermal images show a hot south pole on the planet Neptune. These warmer temperatures provide an avenue for methane to escape out of the deep atmosphere. The images were obtained with the Very Large Telescope in Chile Sept. 1 and 2, 2006.

Neptune

NASA Image and Video Library

1999-07-25

This image of Neptune was taken through the clear filter of the narrow-angle camera on July 16, 1989 by NASA Voyager 2 spacecraft. The image was processed by computer to show the newly resolved dark oval feature embedded in the middle of the dusky south

2016 FACET-II Science Workshop Summary Report

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hogan, Mark J.

The second in a series of FACET-II Science Workshops was held at SLAC National Accelerator Laboratory on October 17-19, 2016 [1]. The workshop drew thirty-five participants from eighteen different institutions including CERN, DESY, Ecole Polytechnique, FNAL, JAI, LBNL, LLNL, Radiabeam, Radiasoft, SLAC, Stony Brook, Strathclyde, Tech-X, Tsinghua, UC Boulder, UCLA and UT Austin. The 2015 workshop [2, 3] helped prioritize research directions for FACET-II. The 2016 workshop was focused on understanding what improvements are needed at the facility to support the next generation of experiments. All presentations are linked to the workshop website as a permanent record.

Updated Review of Planetary Atmospheric Electricity

NASA Astrophysics Data System (ADS)

Yair, Y.; Fischer, G.; Simões, F.; Renno, N.; Zarka, P.

2008-06-01

This paper reviews the progress achieved in planetary atmospheric electricity, with focus on lightning observations by present operational spacecraft, aiming to fill the hiatus from the latest review published by Desch et al. (Rep. Prog. Phys. 65:955 997, 2002). The information is organized according to solid surface bodies (Earth, Venus, Mars and Titan) and gaseous planets (Jupiter, Saturn, Uranus and Neptune), and each section presents the latest results from space-based and ground-based observations as well as laboratory experiments. Finally, we review planned future space missions to Earth and other planets that will address some of the existing gaps in our knowledge.

Updated Review of Planetary Atmospheric Electricity

NASA Astrophysics Data System (ADS)

Yair, Y.; Fischer, G.; Simões, F.; Renno, N.; Zarka, P.

This paper reviews the progress achieved in planetary atmospheric electricity, with focus on lightning observations by present operational spacecraft, aiming to fill the hiatus from the latest review published by Desch et al. (Rep. Prog. Phys. 65:955-997, 2002). The information is organized according to solid surface bodies (Earth, Venus, Mars and Titan) and gaseous planets (Jupiter, Saturn, Uranus and Neptune), and each section presents the latest results from space-based and ground-based observations as well as laboratory experiments. Finally, we review planned future space missions to Earth and other planets that will address some of the existing gaps in our knowledge.

77 FR 25739 - Notice of Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2012-05-01

... additional claimants come forward. DATES: Representatives of any Indian tribe that believes it has a cultural... claimants come forward. The Fowler Museum at UCLA is responsible for notifying the Big Pine Band of Owens...

Molecular profiling is not the future: it is now!

PubMed

Reddy, Bobby; Westcott, Gemma

2015-01-01

Bobby Reddy speaks to Gemma Westcott, Commissioning Editor: Dr Reddy graduated from the UCLA School of Medicine in 1996. Shortly after, he obtained an internship and did his residency in Internal Medicine at Harbor UCLA Medical Center. He then went on to do his fellowship in Hematology and Oncology at City of Hope. Since then, he has been working in private practice (full and part time) for the past 11 years and has had an academic appointment as teaching faculty at Harbor UCLA. Prior to his current role, Dr Reddy worked as a senior medical director as Caris Life Sciences.

Hubble Finds New Dark Spot on Neptune

NASA Image and Video Library

1998-08-02

In 1995, NASA Hubble Space Telescope discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet northern hemisphere was tilted away from Earth, the new feature appeared near the limb of the planet.

NEPTUNE: an under-sea plate scale observatory

NASA Technical Reports Server (NTRS)

Beauchamp, P. M.; Heath, G. R.; Maffei, A.; Chave, A.; Howe, B.; Wilcock, W.; Delaney, J.; Kirkham, H.

2002-01-01

The NEPTUNE project will establish a linked array of undersea observatories on the Juan de Fuca tectonic plate. This observatory will provide a new kind of research platform for real-time, long-term, plate-scale studies in the ocean and Earth sciences.

Origins of the rings of Uranus and Neptune. I - Statistics of satellite disruptions

NASA Technical Reports Server (NTRS)

Colwell, Joshua E.; Esposito, Larry W.

1992-01-01

The origin of the rings of Uranus and Neptune is considered by performing two types of stochastic simulations of the collisional history of small moons: Monte Carlo simulations in which only the largest surviving fragments from each disruption is followed, and a Markov chain approach which makes it possible to follow the size distribution from each disruption to arbitrarily small sizes. Results indicate that the population of small satellites around Uranus and Neptune have evolved through catastrophic fragmentation since the end of planet and satellite formation 3 to 4 billion years ago.

HUBBLE FINDS NEW DARK SPOT ON NEPTUNE

NASA Technical Reports Server (NTRS)

2002-01-01

NASA's Hubble Space Telescope has discovered a new great dark spot, located in the northern hemisphere of the planet Neptune. Because the planet's northern hemisphere is now tilted away from Earth, the new feature appears near the limb of the planet. The spot is a near mirror-image to a similar southern hemisphere dark spot that was discovered in 1989 by the Voyager 2 probe. In 1994, Hubble showed that the southern dark spot had disappeared. Like its predecessor, the new spot has high altitude clouds along its edge, caused by gasses that have been pushed to higher altitudes where they cool to form methane ice crystal clouds. The dark spot may be a zone of clear gas that is a window to a cloud deck lower in the atmosphere. Planetary scientists don t know how long lived this new feature might be. Hubble's high resolution will allow astronomers to follow the spot's evolution and other unexpected changes in Neptune's dynamic atmosphere. The image was taken on November 2, 1994 with Hubble's Wide Field Planetary Camera 2, when Neptune was 2.8 billion miles (4.5 billion kilometers) from Earth. Hubble can resolve features as small as 625 miles (1,000 kilometers) across in Neptune's cloud tops. Credit: H. Hammel (Massachusetts Institute of Technology) and NASA

Managing an Academic Library. Parts I and II.

ERIC Educational Resources Information Center

Werner, Gloria; Brudvig, Glenn

1985-01-01

Describes management experiences at University of California--Los Angeles (UCLA), University of Minnesota Biomedical Library, and California Institute of Technology. Discussions include development of ORION (UCLA's online technical processing and information system); organizational changes occurring as result of large-scale automation;…

Latest Developments in the Installation Planning for Stage 1, NEPTUNE Regional Cabled Observatory, Northeast Pacific

NASA Astrophysics Data System (ADS)

Barnes, C. R.

2004-12-01

NEPTUNE is a proposed innovative network of over 30 sub-sea observatories linked by over 3300 km of powered, fiber-optic cables covering the Juan de Fuca Plate (200,000 sq km), Northeast Pacific. Each observatory will host and power many scientific instruments on the surrounding seafloor, in boreholes in the seafloor, and buoyed up into the water column. Remotely operated and autonomous vehicles will reside at depth, recharge at observatories, and respond to distant labs. Continuous near-real-time multidisciplinary measurement series will extend over 30 years. Shore stations will be located in Port Alberni, BC and Nedonna Beach, OR. Major research themes include: the structure and seismic behavior of the ocean crust; the dynamics of hot and cold fluids and gas hydrates in the upper ocean crust and overlying sediments; ocean climate change and its effect on the ocean biota at all depths; and the barely known ecosystem dynamics and biodiversity of the deep-sea. All involve interacting processes, long term changes, and non-linear, chaotic, episodic events that are hard to study with traditional means. VENUS, MARS, and NEPTUNE will use many of the same cable and engineering systems with the former two acting as test-beds for the latter. NEPTUNE is an US/Canada (70/30) partnership with the total facility cost of about 250M. Over 40M has already been funded for NEPTUNE design and development and for VENUS and MARS. Funding for NEPTUNE Canada's installation contribution (CAN$62.4M) was announced in October 2003. With US NSF/MREFC funding not anticipated before FY 2006, the Northern Loop (Stage 1) of the Project will be installed by NEPTUNE Canada, which comprises a consortium of 12 Canadian universities, lead by the University of Victoria. Housed in new quarters at UVic, NEPTUNE Canada has hired a dozen staff members, with more of be appointed, and has purchased the former Teleglobe TPC4 Shore Station at Port Alberni. Current activities include: a) issuing an RFQu and RFP for the Wet Plant (cable/nodes) with a contract to be signed in Spring 2005, deployment in 2007 and most sensors deployed in 2008; b) arranging three Ocean Observing Systems workshops in 2004 to establish the community experiments, the desired observing systems, and the preferred node locations, c) initial planning for the Data Management and Archiving System (DMAS), and d) establishing MOUs with partner agencies including NSF/ORION, HIA/NRC, and DND. UVic also acts as the lead for the VENUS Project (www.venus.uvic.ca): a shallow-water, coastal observatory in southern BC whose installation has been funded for 2002-06. Over 60km of cable will be divided into three lines: Saanich Inlet (anoxic fiord), across the Strait of Georgia (from Fraser River delta), and across the Strait of Juan de Fuca (active circulation with Pacific Ocean). VENUS and Stage 1 of NEPTUNE will thus form a linked coastal/regional ocean observatory system. NEPTUNE North and VENUS will be among the first of many such cabled ocean observatories.

Building a Geologic Map of Neptune's Moon Triton

NASA Astrophysics Data System (ADS)

Martin, E. S.; Patthoff, D. A.; Bland, M. T.; Watters, T. R.; Collins, G. C.; Becker, T.

2018-06-01

Triton serves as a bridge between KBOs and icy satellites, and characterization of its terrains is important for advancing comparative planetological studies. We aim to create a geologic map of the Neptune-facing side of Triton at a scale of 1:5M.

Mary S. Easton Center of Alzheimer's Disease Research at UCLA: advancing the therapeutic imperative.

PubMed

Cummings, Jeffrey L; Ringman, John; Metz, Karen

2010-01-01

The Mary S. Easton Center for Alzheimer's Disease Research (UCLA-Easton Alzheimer's Center) is committed to the "therapeutic imperative" and is devoted to finding new treatments for Alzheimer's disease (AD) and to developing technologies (biomarkers) to advance that goal. The UCLA-Easton Alzheimer's Center has a continuum of research and research-related activities including basic/foundational studies of peptide interactions; translational studies in transgenic animals and other animal models of AD; clinical research to define the phenotype of AD, characterize familial AD, develop biomarkers, and advance clinical trials; health services and outcomes research; and active education, dissemination, and recruitment activities. The UCLAEaston Alzheimer's Center is supported by the National Institutes on Aging, the State of California, and generous donors who share our commitment to developing new therapies for AD. The naming donor (Jim Easton) provided substantial funds to endow the center and to support projects in AD drug discovery and biomarker development. The Sidell-Kagan Foundation supports the Katherine and Benjamin Kagan Alzheimer's Treatment Development Program, and the Deane F. Johnson Alzheimer's Research Foundation supports the Deane F. Johnson Center for Neurotherapeutics at UCLA. The John Douglas French Alzheimer's Research Foundation provides grants to junior investigators in critical periods of their academic development. The UCLA-Easton Alzheimer's Center partners with community organizations including the Alzheimer's Association California Southland Chapter and the Leeza Gibbons memory Foundation. Collaboration with pharmaceutical companies, biotechnology companies, and device companies is critical to developing new therapeutics for AD and these collaborations are embraced in the mission of the UCLA-Easton Alzheimer's Center. The Center supports excellent senior 3 investigators and serves as an incubator for new scientists, agents, models, technologies and concepts that will significantly influence the future of AD treatment and AD research.

Cuckoo in the Nest: The Fate of the Original Moons of Neptune

NASA Astrophysics Data System (ADS)

Cuk, Matija; Hamilton, Douglas P.

2016-10-01

Neptune's moon Triton is the largest captured satellite in the solar system, as indicated by its inclined retrograde orbit. The most likely mechanism for its capture is binary disruption, which ejected its former binary companion and placed Triton on a large, eccentric orbit around Neptune (Agnor and Hamilton 2006). While the tides would in principle circularize Triton's orbit (Goldreich et al. 1989), Triton's early orbit would have evolved much faster through interactions with preexisting moons of Neptune (Cuk and Gladman 2005). Assuming that the pre-existing moons of Neptune were similar to those of Uranus, analytical estimates are unclear on which outcome is most likely during moon-moon scattering. Cuk and Gladman (2005) suggested that collisions among the regular moons happen first, while Nogueira et al. (2011) find that collisions between Triton and an old moon, or an ejection should happen first. Here we use the general purpose (T+U) symplectic integrator to explore this short-lived epoch of orbit crossing in the Neptunian system. Our preliminary results indicate that Triton might have collided with one of the preexisting moons of Neptune before the regular satellites could have been destroyed in mutual collisions. Goldreich et al. (1989) claimed that a collision with a moon larger than Miranda would destroy Triton and therefore could be ruled out. However, using modern collisional disruption estimated from Stewart and Leinhardt (2012), we find that Triton could have accreted a 1000-km moon at relevant velocities without being disrupted. The product of this merger would have a much tighter orbit as the accreted moon would not have been retrograde like Triton. At the meeting we will present a more detailed exploration of possible post-capture configurations, and report quantitative probabilities for different outcomes of this exciting and violent episode of Triton's history.

Radial pressure in the solar nebula as affecting the motions of planetesimals. [toroidal particle concentration in planetary evolution

NASA Technical Reports Server (NTRS)

Whipple, F. L.

1973-01-01

Growing planetesimals and a range of drag laws depending on the Reynolds number and on the ratio of particle size to mean free path are considered. Particles spiral in the direction of positive gradient, thus being concentrated toward toroidal concentrations of gas. The effect increases with decreasing rates of particle growth, i.e., with increasing time scales of planet formation by accretion. In the outer regions, where evidence suggests that comets were formed and Uranus and Neptune were so accumulated, the effect of the pressure gradient is to clear the forming comets from those regions. The large mass of Neptune may have developed because of this effect, perhaps Neptune's solar distance was reduced from Bode's law, and perhaps no comet belt exists beyond Neptune. In the asteroid belt, on a slow time scale, the effect may have spiraled planetesimals toward Mars and Jupiter, thus contributing to the lack of planet formation in this region.

Habitable evaporated cores: transforming mini-Neptunes into super-Earths in the habitable zones of M dwarfs.

PubMed

Luger, R; Barnes, R; Lopez, E; Fortney, J; Jackson, B; Meadows, V

2015-01-01

We show that photoevaporation of small gaseous exoplanets ("mini-Neptunes") in the habitable zones of M dwarfs can remove several Earth masses of hydrogen and helium from these planets and transform them into potentially habitable worlds. We couple X-ray/extreme ultraviolet (XUV)-driven escape, thermal evolution, tidal evolution, and orbital migration to explore the types of systems that may harbor such "habitable evaporated cores" (HECs). We find that HECs are most likely to form from planets with ∼1 M⊕ solid cores with up to about 50% H/He by mass, though whether or not a given mini-Neptune forms a HEC is highly dependent on the early XUV evolution of the host star. As terrestrial planet formation around M dwarfs by accumulation of local material is likely to form planets that are small and dry, evaporation of small migrating mini-Neptunes could be one of the dominant formation mechanisms for volatile-rich Earths around these stars.

Featured Image: A New Dark Vortex on Neptune

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2018-03-01

This remarkable series of images by the Hubble Space Telescope (click for the full view) track a dark vortex only the fifth ever observed on Neptune as it evolves in Neptunes atmosphere. These Hubble images, presented in a recent study led by Michael Wong (University of California, Berkeley), were taken in 2015 September, 2016 May, 2016 October, and 2017 October; the observations have monitored the evolution of the vortex as it has gradually weakened and drifted polewards. Confirmation of the vortex solved a puzzle that arose in 2015, when astronomers spotted an unexplained outburst of cloud activity on Neptune. This outburst was likely a group of bright companion clouds that form as air flows over high-pressure dark vortices, causing gases to freeze into methane ice crystals. To learn more about what the authors have since learned by studying this vortex, check out the paper below.CitationMichael H. Wong et al 2018 AJ 155 117. doi:10.3847/1538-3881/aaa6d6

Time domain structures in a colliding magnetic flux rope experiment

NASA Astrophysics Data System (ADS)

Tang, Shawn Wenjie; Gekelman, Walter; Dehaas, Timothy; Vincena, Steve; Pribyl, Patrick

2017-10-01

Electron phase-space holes, regions of positive potential on the scale of the Debye length, have been observed in auroras as well as in laboratory experiments. These potential structures, also known as Time Domain Structures (TDS), are packets of intense electric field spikes that have significant components parallel to the local magnetic field. In an ongoing investigation at UCLA, TDS were observed on the surface of two magnetized flux ropes produced within the Large Plasma Device (LAPD). A barium oxide (BaO) cathode was used to produce an 18 m long magnetized plasma column and a lanthanum hexaboride (LaB6) source was used to create 11 m long kink unstable flux ropes. Using two probes capable of measuring the local electric and magnetic fields, correlation analysis was performed on tens of thousands of these structures and their propagation velocities, probability distribution function and spatial distribution were determined. The TDS became abundant as the flux ropes collided and appear to emanate from the reconnection region in between them. In addition, a preliminary analysis of the permutation entropy and statistical complexity of the data suggests that the TDS signals may be chaotic in nature. Work done at the Basic Plasma Science Facility (BaPSF) at UCLA which is supported by DOE and NSF.

Temperature Dependence of the Rate Constant for the CH3 Recombination Reaction: A Loss Process in Outer Planet Atmospheres

NASA Technical Reports Server (NTRS)

Cody, R. J.; Payne, W. A.; Thorn, R. P., Jr.; Romani, P. N.; Stief, L. J.; Nesbitt, F. L.; Iannone, M. A.; Tardy, D. C.

2002-01-01

The methyl free radical (CH3) has been observed in the atmospheres of Saturn and Neptune by the ISO satellite. There are discrepancies between the column densities for the CH3 radical derived from the ISO observations and the column densities derived from atmospheric photochemical models. For Neptune the model column density is 1.5 times that derived from ISO. For Saturn the model is 6 times that from ISO. The recombination of methyl radicals is the major loss process for methyl in these atmospheres. The serious disagreement between observed and calculated levels of CH3 has led to suggestions that the atmospheric models greatly underestimated the loss of CH3 due to poor knowledge of the rate of the reaction (1) CH3 + CH3 + M goes to C2H6 + M at the low temperatures and pressures of these atmospheric systems. Although the reaction CH3 + CH3 + M goes to C2H6 + M has been extensively studied both theoretically and experimentally, the laboratory conditions have been, with only a few exceptions, higher temperatures (T greater than 298K), higher pressures (P greater than or equal to 10 Torr - 13.3 mbar) or M=Ar rather than H2 or He as the bath gas.

The naming of Neptune

NASA Astrophysics Data System (ADS)

Kollerstrom, Nicholas

2009-03-01

Le Verrier chose the name of Neptune immediately after hearing of the correctness of his prediction. This fact soon became obscured by François Arago's pledge made before the French Académie des Sciences, claiming that Le Verrier had entrusted him with the naming of the new planet. Then, British and German sources weighed in with differing names, and Britain's claim to co-prediction of the planet's position was expressed by their proposal of the name, `Oceanus'. Eventually in February of 1847 Airy urged upon Le Verrier that the name he had originally proposed, namely `Neptune' should be accepted, because it was the only one that could secure consensus.

Transplant tourism in the United States: a single-center experience.

PubMed

Gill, Jagbir; Madhira, Bhaskara R; Gjertson, David; Lipshutz, Gerald; Cecka, J Michael; Pham, Phuong-Thu; Wilkinson, Alan; Bunnapradist, Suphamai; Danovitch, Gabriel M

2008-11-01

Transplant "tourism" typically refers to the practice of traveling outside the country of residence to obtain organ transplantation. This study describes the characteristics and outcomes of 33 kidney transplant recipients who traveled abroad for transplant and returned to University of California, Los Angeles (UCLA) for follow-up. Posttransplantation outcomes were compared between tourists and a matched cohort of patients who underwent transplantation at UCLA (matched for age, race, transplant year, dialysis time, previous transplantation, and donor type). Median follow-up time was 487 d (range 68 to 3056). Compared with all patients who underwent transplantation at UCLA, tourists included more Asians and had shorter dialysis times. Most patients traveled to their region of ethnicity with the majority undergoing transplantation in China (44%), Iran (16%), and the Philippines (13%). Living unrelated transplants were most common. Tourists presented to UCLA a median of 35 d after transplantation. Four patients required urgent hospitalization, three of whom lost their grafts. Seventeen (52%) patients had infections, with nine requiring hospitalization. One patient lost her graft and subsequently died from complications related to donor-contracted hepatitis B. One-year graft survival was 89% for tourists and 98% for the matched UCLA cohort (P = 0.75). The rate of acute rejection at 1 yr was 30% in tourists and 12% in the matched cohort. Tourists had a more complex posttransplantation course with a higher incidence of acute rejection and severe infectious complications.

Neptune in False Color

NASA Image and Video Library

1996-01-29

In this false color image of Neptune, objects that are deep in the atmosphere are blue, while those at higher altitudes are white. The image was taken by Voyager 2 wide-angle camera through an orange filter and two different methane filters. http://photojournal.jpl.nasa.gov/catalog/PIA00051

Plasma and radio waves from Neptune: Source mechanisms and propagation

NASA Astrophysics Data System (ADS)

Wong, H. K.

1994-03-01

This report summarizes results obtained through the support of NASA Grant NAGW-2412. The objective of this project is to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as if flew by Neptune. This study has included data analysis, theoretical and numerical calculations, ray tracing, and modeling to determine the possible source mechanism(s) and locations of the Neptune radio emissions. We have completed four papers, which are included in the appendix. The paper 'Modeling of Whistler Ray Paths in the Magnetosphere of Neptune' investigated the propagation and dispersion of lighting-generated whistler in the magnetosphere of Neptune by using three dimensional ray tracing. The two papers 'Numerical Simulations of Bursty Radio Emissions from Planetary Magnetospheres' and 'Numerical Simulations of Bursty Planetary Radio Emissions' employed numerical simulations to investigate an alternate source mechanism of bursty radio emissions in addition to the cyclotron maser instability. We have also studied the possible generation of Z and whistler mode waves by the temperature anisotropic beam instability and the result was published in 'Electron Cyclotron Wave Generation by Relativistic Electrons.' Besides the aforementioned studies, we have also collaborated with members of the PRA team to investigate various aspects of the radio wave data. Two papers have been submitted for publication and the abstracts of these papers are also listed in the appendix.

A Neptune Trojan Survey for the New Horizons Spacecraft

NASA Astrophysics Data System (ADS)

Sheppard, Scott

2010-06-01

Trojan asteroids share a planet's semi-major axis but lead (L4) or follow (L5) the planet by about 60 degrees near the two triangular Lagrangian points of equilibrium. These minor planets were likely captured in these locations around the planet formation epoch and thus their current dynamical and physical properties will help constrain the formation, evolution and migration of the planets. The Neptune Trojans currently consist of only six known objects, all in the leading L4 cloud. Three of these were discovered in our initial survey of the L4 region allowing us to determine that Neptune was likely on a much more eccentric orbit in the distant past. We propose to continue a survey for Neptune Trojans in the trailing L5 region and to recover promising candidates found in 2009A with Subaru. Only with knowledge of the Trojan numbers and orbits in both the L4 and L5 clouds will we be able to understand their formation and evolution and further constrain planet accretion and migration. In addition, the New Horizons spacecraft will pass through the Neptune L5 region in 2013 on its way to Pluto. It is important that we understand the possible dust production produced by collisions of the Trojans as well as find suitable Trojans that New Horizons will observe as it passes through the area.

Resonant Transneptunian Binaries: Evidence for Slow Migration of Neptune

NASA Technical Reports Server (NTRS)

Noll, Keith S.; Grundy, W. M.; Schlichting, H. E.; Murray-Clay, R. A.; Benecchi, S. B.

2012-01-01

As Neptune migrated, its mean-motion resonances preceded it into the planetesimal disk. The efficiency of capture into mean motion resonances depends on the smoothness of Neptune's migration and the local population available to be captured. The two strongest resonances, the 3:2 at 39.4 AU and 2:1 at 47.7 AU, straddle the core repository of the physically distinct and binary-rich Cold Classicals, providing a unique opportunity to test the details of Neptune's migration. Smooth migration should result in a measurable difference between the 3:2 and 2:1 resonant object properties, with low inclination 2:1s having a high fraction of red binaries, mirroring that of the Cold Classicals while the 3:2 will would have fewer binaries. Rapid migration would generate a more homogeneous result. Resonant objects observed with HST show a higher rate of binaries in the 2:1 relative to the 3:2, significant at the 2cr level. This suggests slow Neptune migration over a large enough distance that the 2:1 swept through the Cold Classical region. Colors are available for only a fraction of these targets but a prevalence of red objects in outer Resonances has been reported. We report here on ongoing observations with HST in cycle 19 targeting all unobserved Resonants with observations that will measure color and search for binary companions using the WFC3.

Neptune's inner magnetosphere and aurora: Energetic particle constraints

NASA Technical Reports Server (NTRS)

Mauk, B. H.; Krimigis, S. M.; Acuna, M. H.

1994-01-01

A dramatic and peculiar dropout of greater than 500-keV ions (but not electrons) was observed within Neptune's inner magnetosphere near 2 R(sub N) as the Voyager 2 spacecraft approached the planet. Unlike a number of other energetic particle features this feature could not be accounted for by known material bodies in the context of the most utilized magnetic field models (neither the offset tilted dipole models nor the spehrical harmonic model 'O8'). However, the configuration of Neptune's inner magnetosphere is highly uncertain. By applying a novel technique, utilizing energetic particle measurements, to constrain the magnetic field configuration of the inner regions, we show that appeals to unobserved materials within Neptune's system are unnecessary, and that the ion dropout feature was, in all likelihood, the result of ion interactions with maximum L excursions of the ring 1989N1R. The constraints also favor the se of the M2 magnetic field model (Selesnick, 1992) over the previous models. An electron feature was probably absent because the electron interactions with the ring occurred substantially before the ion interactions (about 2 hours for the electrons versus a few minutes for the ions). Pitch-angle scattering apparently eliminated the electron signature. Minimum scattering rates determined based on this premise yield enough electron precipitation power to explain the brightest component of Neptune's aurora. We propose that this bright component is analogous to the Earth's diffuse aurora.

Plasma and radio waves from Neptune: Source mechanisms and propagation

NASA Technical Reports Server (NTRS)

Wong, H. K.

1994-01-01

This report summarizes results obtained through the support of NASA Grant NAGW-2412. The objective of this project is to conduct a comprehensive investigation of the radio wave emission observed by the planetary radio astronomy (PRA) instrument on board Voyager 2 as if flew by Neptune. This study has included data analysis, theoretical and numerical calculations, ray tracing, and modeling to determine the possible source mechanism(s) and locations of the Neptune radio emissions. We have completed four papers, which are included in the appendix. The paper 'Modeling of Whistler Ray Paths in the Magnetosphere of Neptune' investigated the propagation and dispersion of lighting-generated whistler in the magnetosphere of Neptune by using three dimensional ray tracing. The two papers 'Numerical Simulations of Bursty Radio Emissions from Planetary Magnetospheres' and 'Numerical Simulations of Bursty Planetary Radio Emissions' employed numerical simulations to investigate an alternate source mechanism of bursty radio emissions in addition to the cyclotron maser instability. We have also studied the possible generation of Z and whistler mode waves by the temperature anisotropic beam instability and the result was published in 'Electron Cyclotron Wave Generation by Relativistic Electrons.' Besides the aforementioned studies, we have also collaborated with members of the PRA team to investigate various aspects of the radio wave data. Two papers have been submitted for publication and the abstracts of these papers are also listed in the appendix.

Examining Rotational Variability in the Upper Tropospheres and Lower Stratospheres of Uranus and Neptune from Herschel PACS OT1 Observations: Implications for the Stability of Temperature and Compositional Structure

NASA Astrophysics Data System (ADS)

Orton, G.; Feuchtgruber, H.; Fletcher, L.; Lellouch, E.; Moreno, R.; Billebaud, F.; Cavalie, T.; Decin, L.; Dobreijecvic, M.; Encrenaz, T.; Hartogh, P.; Jarchow, C.; Lara, L. M.; Liu, J.

2012-04-01

The power of high-resolution submillimeter spectroscopy of Uranus and Neptune was put to use to survey the rotational variability of stratospheric and tropospheric constituents of their atmospheres. These observations were motivated by the surprising discovery of as much as 12% rotational variability of emission from stratospheric constituents in the atmosphere of Uranus by the Spitzer Infrared Spectrometer and the detection of spatial variability in thermal images of Neptune's stratospheric emission (Orton et al. 2007, Astron. & Astrophys 473, L3). Our observing program consisted of three separate sequences of observations to look at the strongest lines of H2O in the high-resolution PACS spectra of both planets, whose upwelling radiance emerges from the same vertical region as the Spitzer IRS observations of Uranus and ground-based images of Neptune, and the strongest line of CH4 in the PACS spectrum of Neptune. We omitted measurements of CH4 lines in Uranus, which are almost non-detectable. We added the strongest HD line in Uranus to measure variability of tropospheric temperatures that could modulate stratospheric CH4 abundances through local cold-trapping and the strongest two HD lines in Neptune (Lellouch et al. 2010, Astron. & Astrophys. 518, L152) that determine both the tropopause temperature to limit local cold-trapping efficacy and the lower stratospheric temperature, to help differentiate between longitudinal variability of stratospheric H2O and CH4 abundances vs. temperatures. These were repeated over the 17-hour interval that is common to the equatorial rotation periods of both Uranus and Neptune. Although these lines had already been observed in Uranus and Neptune by PACS, no repeat measurements had ever been made to determine longitudinal variability. The observations were consistent with previous measurements, but no significant rotational variability was detected. It is possible that the absence of rotational variability in the HD and CH4 lines is because variability is confined to very low pressures, e.g. much lower than a microbar. However, the absence of variable emission from high-altitude exogenic H2O vapor is harder to explain, unless the variability seen in Uranus by Spitzer and in Neptune from the VLT, is not the result of variations in temperature by in the hydrocarbon abundances. Alternatively, the stratospheres of both planets are variable in time. The cause of such variability is unknown, but spatially confined outbursts have been detected in the visible and near infrared, and they may have as much influence on the stratosphere of Uranus as the great springtime storm in Saturn's northern hemisphere, creating a strong, localized "beacon" of thermal radiation (cf. Fletcher et al. 2011, Science, 332,1413) that could dominate the emission observed over the hemisphere.

Beyond Transfer Shock: Dimensions of Transfer Students' Adjustment.

ERIC Educational Resources Information Center

Laanan, Frankie Santos

This study examined the adjustment process of 727 students who transferred to the University of California, Los Angeles (UCLA) in fall 1994 or fall 1995. The Transfer Students' Questionnaire (TSQ) was organized into three main sections: social demographics, perceptions of the community college experience, and perception of the UCLA experience. The…

Changing Patterns of Cervical Disease in a Student Population.

ERIC Educational Resources Information Center

Rosenthal, Dorothy L.; And Others

1982-01-01

The Cytology Service at the University of California at Los Angeles (UCLA) Center for Health Sciences has examined about 4000 pap smears (each year) from the UCLA Student Health Service between 1973-1978. An apparently significant increase in abnormal pap smears in young college-age women is reported. (Authors/CJ)

Innovations in Student-Centered Interdisciplinary Teaching for General Education in Aging

ERIC Educational Resources Information Center

Damron-Rodriguez, JoAnn; Effros, Rita

2008-01-01

The University of California-Los Angeles (UCLA) General Education "Clusters" are innovations in student-centered undergraduate education focused on complex phenomena that require an interdisciplinary perspective. UCLA gerontology and geriatric faculty recognized the opportunity to introduce freshmen to the field of aging through this new…

2011 Women in Defense (WID) National Fall Conference

DTIC Science & Technology

2011-10-19

UCLA. She is also a graduate of the UCLA Executive Management Course and the University of Chicago Business Leadership Program. A member of the Air...Supercircuits Ms. Beth A. Shepard -Savery Cox Communications Hampton Roads, LLC Ms. Erin B. Sheppard McKenna Long & Aldridge, LLP Ms. Heidi L Shyu

Putting the Camps into UCLA's Curriculum.

ERIC Educational Resources Information Center

Matsumoto, Valerie

1993-01-01

Discusses the history and design of a project to integrate material on the internment of Japanese Americans in the Second World War into the curriculum at the University of California Los Angeles (UCLA). Proceedings of a seminar to develop the process are also reviewed, with suggestions for the future. (SLD)

The "Theft" of the Neptune Papers

NASA Astrophysics Data System (ADS)

Rawlins, Dennis

1994-10-01

Correspondence 1966-1993 attempting to flush out the long-secreted Royal Greenwich Observatory file on Neptune's discovery, hinting that it was in the possession of a former Chief Ass't to the Astronomer Royal. The file was ultimately found among his effects, four years after this article, when he unexpectedly died in Chile.

Aerospace Engineering Space Mission Concept Feasibility Study: A Neptune Mission Design Example

NASA Technical Reports Server (NTRS)

Esper, Jaime

2007-01-01

This viewgraph document reviews the feasibility study of a mission to Neptune. Included are discussions of the science instruments, the design methodology, the trajectory, the spacecraft design, the alternative propulsion systems, (chemical, solar electric (SEP)), the communications systems, the power systems, the thermal system.

Homogeneity of CdZnTe detectors

NASA Astrophysics Data System (ADS)

Hermon, H.; Schieber, M.; James, R. B.; Lund, J.; Antolak, A. J.; Morse, D. H.; Kolesnikov, N. N. P.; Ivanov, Y. N.; Goorsky, M. S.; Yoon, H.; Toney, J.; Schlesinger, T. E.

1998-02-01

We describe the current state of nuclear radiation detectors produced from single crystals of Cd 1- xZn xTe(CZT), with 0.04 < x < 0.4, grown by the vertical high pressure Bridgman (VHPB) method. The crystals investigated were grown commercially both in the USA and at the Institute of Solid State Physics, Chernogolska, Russia. The CZT was evaluated by Sandia National Laboratories and the UCLA and CMU groups using proton-induced X-ray emission (PIXE), X-ray diffraction (XRD), photoluminescence (PL), infrared (IR) transmission microscopy, leakage current measurements and response to nuclear radiation. We discuss the homogeneity of the various CZT crystals based on the results from these measurement techniques.

Recovery Act - LADWP Smart Grid Regional Demonstration Program Final Technical Report

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chiu, Sungly; Vohra, Surendra; Abdelshehid, Emil

LADWP collaborated with its project partners to carry out this demonstration in the designated areas to include two university campuses – the University of California, Los Angeles (UCLA) and the University of Southern California (USC) – surrounding neighborhoods, City of Los Angeles facilities, and LADWP power system test labs. The last project partner, Jet Propulsion Laboratory (JPL) was responsible for the cyber security aspects of the project. The program’s use cases provided insightful information to understand triggers for customers, distributors, and generators to adapt their behavior which aid in reducing system demands and costs, increasing energy efficiency, and increasing gridmore » reliability.« less

Naval Research Laboratory Ecological -- Photochemical -- Bio-optical--Numerical Experiment (Neptune) Version 1: A Portable, Flexible Modeling Environment Designed to Resolve Time-dependent Feedbacks Between Upper Ocean Ecology, Photochemistry, and Optics

DTIC Science & Technology

2007-02-21

dependent upon the carbon gross growth efficiency ( GGE ) and the C:N:P ratio of the organic substrate. This calculation and its structural...product of the temperature adjusted maximum gross carbon assimilation rate, the carbon gross growth efficiency ( GGE ), and the uptake kinetics for DOC...substrate: max T 4 [ ]( ) [ ]Cb b DOCg g GGE n DOC ⎛ ⎞ = ⎜ ⎟+⎝ ⎠ (21) and ( )( 30)max T m30 m30min[ , ]Kt Tb b bg g g e −= (22) To

Structure of scintillations in Neptune's occultation shadow

NASA Technical Reports Server (NTRS)

Hubbard, W. B.; Lellouch, Emmanuel; Sicardy, Bruno; Brahic, Andre; Vilas, Faith

1988-01-01

An exceptionally high-quality data set from a Neptune occultation is used here to derive a number of new results about the statistical properties of the fluctuations of the intensity distribution in various parts of Neptune's occultation shadow. An approximate numerical ray-tracing model which successfully accounts for many of the qualitative aspects of the observed intensity fluctuation distribution is introduced. Strong refractive scintillation is simulated by including the effects of 'turbulence' with projected atmospheric properties allowed to vary in both the direction perpendicular and parallel to the limb, and an explicit two-dimensional picture of a typical intensity distribution throughout an occulting planet's shadow is presented. The results confirm the existence of highly anisotropic turbulence.

The atmosphere of Neptune - Results of radio occultation measurements with the Voyager 2 spacecraft

NASA Technical Reports Server (NTRS)

Lindal, G. F.; Lyons, J. R.; Sweetnam, D. N.; Eshleman, V. R.; Hinson, D. P.

1990-01-01

This paper presents the vertical temperature and composition profiles of Neptune's troposphere and stratosphere, covering an altitude of 250 km, obtained from radio tracking data that were acquired during Voyager-2's occultation by Neptune, which began near 62 deg N planetographic latitude and ended near 45 deg S latitude. In the computations, the He/H2 abundance ratio 15/85 was adapted, which is consistent with solar abundance estimates and with recent results from Uranus. It was assumed that aerosols and heavier gases such as CH4, NH3, H2S, and H2O have a negligible effect on the microwave refractivity above the 0.5 bar pressure level.

Voyager 2 at Neptune - Imaging science results

NASA Technical Reports Server (NTRS)

Smith, B. A.; Soderblom, L. A.; Banfield, D.; Barnet, C.; Beebe, R. F.; Bazilevskii, A. T.; Bollinger, K.; Boyce, J. M.; Briggs, G. A.; Brahic, A.

1989-01-01

Neptune's atmosphere is revealed by Voyager 2 images to contain clouds of methane ice above a lower deck of hydrogen sulfide or ammonia ices, and to be dominated by an anticyclonic storm system designated the 'Great Dark Spot'; this bears both similarities and differences to the Great Red Spot of Jupiter. Like the rings of Uranus, those of Neptune are composed of very dark, but in addition very dusty, material. Six new regular satellites have been discovered whose radii range from 25 to 200 km. Triton is noted to be a differentiated body showing evidence of early surface-melting episodes. At least two active plumes are found on Triton, which may be driven by solar heating.

The UCLA Young Autism Project: A Reply to Gresham and Macmillan.

ERIC Educational Resources Information Center

Smith, Tristam; Lovass, O. Ivar

1997-01-01

Responds to "Autistic Recovery? An Analysis and Critique of the Empirical Evidence on the Early Intervention Project" (Gresham and MacMillan), which criticizes research showing the effectiveness of the UCLA Youth Autism Project program for children with autism. The article's misunderstandings are discussed and the program is explained. (CR)

Implementing Community Engagement as a Mission at the David Geffen School of Medicine at the University of California, Los Angeles.

PubMed

Chung, Bowen; Brown, Arleen; Moreno, Gerardo; Cuen, Pattie; Uy, Visith; Vangala, Sitaram; Bell, Douglas; Washington, A Eugene; Norris, Keith C; Mangione, Carol

2016-02-01

This manuscript describes the development and implementation of community engagement as a mission at UCLA's David Geffen School of Medicine (DGSOM) and UCLA Health System, and summarizes survey results documenting existing community-engaged projects and interest between 2010 to 2013.

Faith and Reason on Campus

ERIC Educational Resources Information Center

Adler, Norman

2007-01-01

According to a study of student religiosity conducted by the University of California-Los Angeles (UCLA), 80 percent of students express a strong interest in spirituality. They are not only spiritual, but they are also religious. Over half of all students attend religious services at least once per month. Indeed, according to the UCLA study, eight…

REFORMA/UCLA Mentor Program: A Mentoring Manual.

ERIC Educational Resources Information Center

Tauler, Sandra

Although mentoring dates back to Greek mythology, the concept continues to thrive in today's society. Mentoring is a strategy that successful people have known about for centuries. The REFORMA/UCLA Mentor Program has made use of this strategy since its inception in November 1985 at the Graduate School of Library and Information Science at the…

A Holistic Emphasis: The UCLA American Indian Studies Research Center.

ERIC Educational Resources Information Center

Champagne, Duane

2001-01-01

At UCLA, the American Indian Studies Center's structure as an organized research unit allows a platform for many activities not normally within the purview of departments. The Center implements a holistic, Native view of research, policy, community engagement, and education; has a library and publications; and is a gathering place for American…

California Librarians Black Caucus/UCLA Mentor Program Handbook.

ERIC Educational Resources Information Center

California Univ., Los Angeles. Graduate School of Library and Information Science.

This handbook for the Mentor Program of the California Librarians Black Caucus (CLBC) and the University of California Los Angeles (UCLA) Graduate School of Library and Information Science (GSLIS) begins by stating that the purpose of the program is to increase the number of African American librarians and other information professionals in…

Infrared spectroscopy of organics of planetological interest at low temperatures

NASA Technical Reports Server (NTRS)

Khanna, R. K.

1994-01-01

In the context of prebiotic chemistry in space, some of the outer planetary objects display H, C, N and O rich chemistry similar to the one in the biosphere of Earth. Of particular interest are Saturn's moon, Titan; Neptune's moon, Triton; and Pluto where extreme cold conditions prevail. Identifications of chemical species on these objects (surfaces and atmospheres) is essential to a better understanding of the radiation induced chemical reactions occuring thereon. There have been several ground based observations of these planetary objects in the infrared windows from 1 to 2.5 micrometers. Voyager also provided spectra in the thermal infrared (6 to 50 micrometers) region. Interpretation of these data require laboratory infrared spectra of relevant species under the temperature conditions appropriate to these objects. The results of some of these studies carried out in our laboratory and elsewhere and their impact on the analyses of the observed data will be summarized.

75 FR 51374 - Regulated Navigation Areas, Safety Zones, Security Zones; Deepwater Ports in Boston Captain of...

Federal Register 2010, 2011, 2012, 2013, 2014

2010-08-20

... Coast Guard is establishing regulated navigation areas (RNAs) and safety and security zones around the recently constructed Neptune Deepwater Port Facility, and modifying RNA and safety zone regulations for the... and Northeast Gateway deepwater ports. The Neptune RNAs will prohibit vessels from anchoring or...

The planets Uranus, Neptune, and Pluto (1971)

NASA Technical Reports Server (NTRS)

Palluconi, F. D.

1972-01-01

Design criteria relating to spacecraft intended to investigate the planets of Uranus, Neptune, and Pluto are presented. Assessments were made of the potential effects of environmental properties on vehicle performance. Pertinent data on the mass, radius, shape, mean density, rotational pole location, and mean orbital elements for the three planets are given in graphs and tables.

NEPTUNE Canada-status and planning

NASA Astrophysics Data System (ADS)

Bornhold, Brian D.

2005-04-01

Stage 1 of the joint Canada-U.S. NEPTUNE seafloor observatory has been funded by the Canada Foundation for Innovation and the British Columbia Knowledge Development Fund with an overall budget of $62.4 million. The network is designed to provide as close to real-time data and images as possible to be distributed to the research community, government agencies, educational institutions and the public via the Internet. Covering much of the northern segment of the Juan de Fuca Plate, this first phase of the NEPTUNE project is scheduled to be installed, with an initial suite of ``community experiments'', in 2008. As part of the planning, NEPTUNE Canada held a series of three workshops to develop the science plans for these ``community experiments'' these experiments have a budget of approximately $13 million. The experiments will cover the gamut of oceanographic science themes including various aspects of: ocean climate and marine productivity, seabed environments and biological communities, fluids at ocean ridges, gas hydrates and fluids on continental margins, plate tectonics processes, associated earthquakes and tsunamis. The next three years will be spent developing and testing the necessary instrumentation for deployment on the network.

ARC-1989-AC89-7001

NASA Image and Video Library

1989-08-21

Photo by Voyager 2 (JPL) During August 16 and 17, 1989, the Voyager 2 narrow-angle camera was used to photograph Neptune almost continuously, recording approximately two and one-half rotations of the planet. These images represent the most complete set of full disk Neptune images that the spacecraft will acquire. This picture from the sequence shows two of the four cloud features which have been tracked by the Voyager cameras during the past two months. The large dark oval near the western limb (the left edge) is at a latitude of 22 degrees south and circuits Neptune every 18.3 hours. The bright clouds immediately to the south and east of this oval are seen to substantially change their appearances in periods as short as four hours. The second dark spot, at 54 degrees south latitude near the terminator (lower right edge), circuits Neptune every 16.1 hours. This image has been processed to enchance the visibility of small features, at some sacrifice of color fidelity. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications. (JPL Ref: A-34611 Voyager 2-N29)

The Phase Space Structure Near Neptune Resonances in the Kuiper Belt

NASA Technical Reports Server (NTRS)

Malhotra, Renu

1996-01-01

The Solar system beyond Neptune is believed to house a population of small primordial bodies left over from the planet formation process. The region up to heliocentric distance -50 AU (a.k.a. the Kuiper Belt) may be the source of the observed short-period comets. In this region, the phase space structure near orbital resonances with Neptune is of special interest for the long-term stability of orbits. There is reason to believe that a significant fraction (perhaps most) of the Kuiper Belt objects reside preferentially in these resonance locations. This paper describes the dynamics of small objects near the major orbital resonances with Neptune. Estimates of the widths of stable resonance zones as well as the properties of resonant orbits are obtained from the circular, planar restricted three-body model. Although this model does not contain the full complexity of the long-term orbital dynamics of Kuiper Belt objects subject to the full N-body perturbations of all the planets, it does provide a baseline for the phase space structure and properties of resonant orbits in the trans-Neptunian Solar system.

ARC-1989-A89-7006

NASA Image and Video Library

1989-08-21

Range : 12 million km (7.5 million miles) Resolution 110 km (68 miles) per pixel. These 2 images of Neptune were taken by Voyager 2's narrow-angle camera. During the 17.6 hours between the left and right images, the Great Dark Spot, at 22 degrees south latitude (left of center), has completed a little less than one rotation of Neptune. The smaller dark spot, at 54 south, completed a little more than one rotation, as can be seen by comparing its relative positions in the two pictures. The Great Dark Spot and the smaller spot have a relative velocity of 100 meters per second (220 miles an hour). The light and dark bands circling Neptune indicate predominantly zonal (east-west) motion. The diffuse white feature north of the Great Dark Spot is near Neptune's equator, and rotates with about the same period as the Great Dark Spot. Streak of bright clouds at the south edge, and just east of the Great Dark Spot, are its constatnt companions, and change the details of their appearance, often within a few hours. Changing brightness of the cloud streaks could be a result of vertical mortions.

Uranus and Neptune: internal heat flow

NASA Astrophysics Data System (ADS)

Hofstadter, M. D.; Simon, A. A.; Banfield, D. J.; Fortney, J. J.; Hayes, A. G., Jr.; Hedman, M.; Hospodarsky, G. B.; Mandt, K.; Showalter, G. M.; Soderlund, K. M.; Turtle, E. P.; Hofstadter, M. D.; Sayanagi, K. M.; Simon, A. A.; Banfield, D. J.; Fortney, J. J.; Hayes, A.; Hedman, M.; Hospodarsky, G. B.; Mandt, K.; Showalter, G. M.; Soderlund, K. M.; Turtle, E. P.; Nettelmann, N.; Scheibe, L.; Redmer, R.

2017-12-01

Uranus and Neptune offer unique possibilities to study the behavior of gas-ice-rock mixtures at high pressures, the formation of planets, planetary magnetic field generation [1], and planetary atmospheres. While Uranus and Neptune interior models have been constructed that satisfy some of the observational constraints, so far there are no physically motivated models that are consistent with all of them. Especially the observed intrinsic heat fluxes pose challenges [2]. Here I present the thermal boundary layer approach [3] to explain both the extraordinary low heat flux of Uranus and the high heat flux of Neptune, and discuss implications. In particular, current models suggest miscibility of ices with rocks at P>1 Mbar and super-solar ice-to-rock ratios, for Uranus an irradiated exoplanet-like evolution in equilibrium with the stellar incident flux, and fully convective deep interiors. The Figure illustrates such an ice giant interior model.[1] Soderlund K.M., Heimpel, M.H., King E.M. Aurnou J.M. (2013), Icarus 224, 97 [2] Guillot T. (2005), Annu. Rev. Earth Planet. Sci. 33, 493 [3] Nettelmann N., Wang K., Fortney J.J. et al (2016), Icarus 275, 107

Monodeuterated methane in the outer solar system. IV - Its detection and abundance on Neptune

NASA Technical Reports Server (NTRS)

De Bergh, C.; Lutz, B. L.; Owen, T.; Maillard, J.-P.

1990-01-01

The 3nu2 band of CH3D was detected in the spectrum of Neptune near 1.6 micron recorded at a spectral resolution of 4/cm with the Cassegrain Fourier Transportation Spectrometer at the 3.6 m Canada-France-Hawaii Telescope CFHT) on Mauna Kea. The analysis of this spectrum, using spectral synthesis techniques, yielded a CH3D/CH4 ratio of about 0.0006, which corresponds to a global D/H ratio for Neptune of about 0.00012, if CH3D is in isotopic fractionation equilibrium with HD. This value is about an order of magnitude larger than an earlier estimate by Orton et al. (1987) based on deconvolution measurements of unresolved molecular emission in the 8-10-micron region. Comparison of this new determination with previous studies of CH3D in the outer solar system shows that, as in the case of Uranus, the D/H on Neptune is strongly enhanced over that found on Jupiter and Saturn and is comparable to the D/H in methane on Titan and in terrestrial methane and water.

Outreach and education in urban Los Angeles Schools: integration of research into middle and high school science curriculum through the NSF GK-12 SEE-LA program

NASA Astrophysics Data System (ADS)

Daniel, J. C.; Hogue, T. S.; Moldwin, M. B.; Nonacs, P.

2012-12-01

A National Science Foundation Graduate Teaching Fellows in K- 12 Education program at UCLA (SEE-LA; http://measure.igpp.ucla.edu/GK12-SEE-LA/ ) partners UCLA faculty and graduate students (fellows) with urban middle and high school science teachers and their students to foster programs of science and engineering exploration that bring the environment of Los Angeles into the classroom. UCLA science and engineering graduate fellows serve as scientists-in-residence at four partner schools to integrate inquiry-based science lessons, facilitate advancements in science content teaching, and ultimately, to improve their own science communication skills. As part of their fellowship, graduate students are required to develop three "major" lessons, including one based on their PhD research at UCLA. During the first four years of the project, the SEE-LA fellows have developed a range of research-based activities, including lessons on sustainable fisheries, ecosystems and remote sensing, earthquakes, urban water quality including invertebrate observations, and post-fire soil chemistry, among others. This presentation will provide an overview of the SEE-LA GK-12 program and development of research lessons that also address California State Science Standards. We also discuss potential sustainability of GK-12 type outreach and education programs. The SEE-LA program has provided development of graduate student communication and teaching skills while also contributing significantly to the integration of science education into K-12 curriculum in Los Angeles schools.

Transplant Tourism in the United States: A Single-Center Experience

PubMed Central

Gill, Jagbir; Madhira, Bhaskara R.; Gjertson, David; Lipshutz, Gerald; Cecka, J. Michael; Pham, Phuong-Thu; Wilkinson, Alan; Bunnapradist, Suphamai; Danovitch, Gabriel M.

2008-01-01

Background and objectives: Transplant “tourism” typically refers to the practice of traveling outside the country of residence to obtain organ transplantation. This study describes the characteristics and outcomes of 33 kidney transplant recipients who traveled abroad for transplant and returned to University of California, Los Angeles (UCLA) for follow-up. Design, settings, participants, & measurements: Posttransplantation outcomes were compared between tourists and a matched cohort of patients who underwent transplantation at UCLA (matched for age, race, transplant year, dialysis time, previous transplantation, and donor type). Median follow-up time was 487 d (range 68 to 3056). Results: Compared with all patients who underwent transplantation at UCLA, tourists included more Asians and had shorter dialysis times. Most patients traveled to their region of ethnicity with the majority undergoing transplantation in China (44%), Iran (16%), and the Philippines (13%). Living unrelated transplants were most common. Tourists presented to UCLA a median of 35 d after transplantation. Four patients required urgent hospitalization, three of whom lost their grafts. Seventeen (52%) patients had infections, with nine requiring hospitalization. One patient lost her graft and subsequently died from complications related to donor-contracted hepatitis B. One-year graft survival was 89% for tourists and 98% for the matched UCLA cohort (P = 0.75). The rate of acute rejection at 1 yr was 30% in tourists and 12% in the matched cohort. Conclusions: Tourists had a more complex posttransplantation course with a higher incidence of acute rejection and severe infectious complications. PMID:18922987

Understanding the mass-radius relation for sub-Neptunes: radius as a proxy for composition

DOE Office of Scientific and Technical Information (OSTI.GOV)

Lopez, Eric D.; Fortney, Jonathan J.

2014-09-01

Transiting planet surveys like Kepler have provided a wealth of information on the distribution of planetary radii, particularly for the new populations of super-Earth- and sub-Neptune-sized planets. In order to aid in the physical interpretation of these radii, we compute model radii for low-mass rocky planets with hydrogen-helium envelopes. We provide model radii for planets 1-20 M {sub ⊕}, with envelope fractions 0.01%-20%, levels of irradiation 0.1-1000 times Earth's, and ages from 100 Myr to 10 Gyr. In addition we provide simple analytic fits that summarize how radius depends on each of these parameters. Most importantly, we show that atmore » fixed H/He envelope fraction, radii show little dependence on mass for planets with more than ∼1% of their mass in their envelope. Consequently, planetary radius is to a first order a proxy for planetary composition, i.e., H/He envelope fraction, for Neptune- and sub-Neptune-sized planets. We recast the observed mass-radius relationship as a mass-composition relationship and discuss it in light of traditional core accretion theory. We discuss the transition from rocky super-Earths to sub-Neptune planets with large volatile envelopes. We suggest ∼1.75 R {sub ⊕} as a physically motivated dividing line between these two populations of planets. Finally, we discuss these results in light of the observed radius occurrence distribution found by Kepler.« less

Seasonal stratospheric photochemistry on Uranus and Neptune

NASA Astrophysics Data System (ADS)

Moses, Julianne I.; Fletcher, Leigh N.; Greathouse, Thomas K.; Orton, Glenn S.; Hue, Vincent

2018-06-01

A time-variable 1D photochemical model is used to study the distribution of stratospheric hydrocarbons as a function of altitude, latitude, and season on Uranus and Neptune. The results for Neptune indicate that in the absence of stratospheric circulation or other meridional transport processes, the hydrocarbon abundances exhibit strong seasonal and meridional variations in the upper stratosphere, but that these variations become increasingly damped with depth due to increasing dynamical and chemical time scales. At high altitudes, hydrocarbon mixing ratios are typically largest where the solar insolation is the greatest, leading to strong hemispheric dichotomies between the summer-to-fall hemisphere and winter-to-spring hemisphere. At mbar pressures and deeper, slower chemistry and diffusion lead to latitude variations that become more symmetric about the equator. On Uranus, the stagnant, poorly mixed stratosphere confines methane and its photochemical products to higher pressures, where chemistry and diffusion time scales remain large. Seasonal variations in hydrocarbons are therefore predicted to be more muted on Uranus, despite the planet's very large obliquity. Radiative-transfer simulations demonstrate that latitude variations in hydrocarbons on both planets are potentially observable with future JWST mid-infrared spectral imaging. Our seasonal model predictions for Neptune compare well with retrieved C2H2 and C2H6 abundances from spatially resolved ground-based observations (no such observations currently exist for Uranus), suggesting that stratospheric circulation - which was not included in these models - may have little influence on the large-scale meridional hydrocarbon distributions on Neptune, unlike the situation on Jupiter and Saturn.

What is Neptune's D/H ratio really telling us about its water abundance?

NASA Astrophysics Data System (ADS)

Ali-Dib, Mohamad; Lakhlani, Gunjan

2018-05-01

We investigate the deep-water abundance of Neptune using a simple two-component (core + envelope) toy model. The free parameters of the model are the total mass of heavy elements in the planet (Z), the mass fraction of Z in the envelope (fenv), and the D/H ratio of the accreted building blocks (D/Hbuild).We systematically search the allowed parameter space on a grid and constrain it using Neptune's bulk carbon abundance, D/H ratio, and interior structure models. Assuming solar C/O ratio and cometary D/H for the accreted building blocks are forming the planet, we can fit all of the constraints if less than ˜15 per cent of Z is in the envelope (f_{env}^{median} ˜ 7 per cent), and the rest is locked in a solid core. This model predicts a maximum bulk oxygen abundance in Neptune of 65× solar value. If we assume a C/O of 0.17, corresponding to clathrate-hydrates building blocks, we predict a maximum oxygen abundance of 200× solar value with a median value of ˜140. Thus, both cases lead to oxygen abundance significantly lower than the preferred value of Cavalié et al. (˜540× solar), inferred from model-dependent deep CO observations. Such high-water abundances are excluded by our simple but robust model. We attribute this discrepancy to our imperfect understanding of either the interior structure of Neptune or the chemistry of the primordial protosolar nebula.

Joint Radioisotope Electric Propulsion Studies - Neptune System Explorer

NASA Technical Reports Server (NTRS)

Khan, M. Omair; Amini, Rashied; Ervin, Joan; Lang, Jared; Landau, Damon; Oleson, Steven; Spilker, Thomas; Strange, Nathan

2011-01-01

The Neptune System Explorer (NSE) mission concept study assessed opportunities to conduct Cassini-like science at Neptune with a radioisotope electric propulsion (REP) based spacecraft. REP is based on powering an electric propulsion (EP) engine with a radioisotope power source (RPS). The NSE study was commissioned under the Joint Radioisotope Electric Propulsion Studies (JREPS) project, which sought to determine the technical feasibility of flagship class REP applications. Within JREPS, special emphasis was given toward identifying tall technology tent poles, as well as recommending any new RPS technology developments that would be required for complicated REP missions. Based on the goals of JREPS, multiple RPS (e.g. thermoelectric and Stirling based RPS) and EP (e.g. Hall and ion engines) technology combinations were traded during the NSE study to determine the most favorable REP design architecture. Among the findings from the study was the need for >400We RPS systems, which was driven by EP operating powers and the requirement for a long-lived mission in the deep solar system. Additionally multiple development and implementation risks were identified for the NSE concept, as well as REP missions in general. Among the strengths of the NSE mission would be the benefits associated with RPS and EP use, such as long-term power (approx. 2-3kW) at Neptune and flexible trajectory options for achieving orbit or tours of the Neptune system. Although there are still multiple issues to mitigate, the NSE concept demonstrated distinct advantages associated with using REP for deep space flagship-class missions.

HAT-P-26b: A Neptune-mass Exoplanet with Primordial Solar Heavy Element Abundance

NASA Astrophysics Data System (ADS)

Wakeford, Hannah R.; Sing, David K.; Kataria, Tiffany; Deming, Drake; Nikolov, Nikolay; Lopez, Eric; Tremblin, Pascal; Skalid Amundsen, David; Lewis, Nikole K.; Mandell, Avi; Fortney, Jonathan J.; Knutson, Heather; Benneke, Björn; Evans, Tom M.

2017-01-01

A trend in giant planet mass and atmospheric heavy elemental abundance was first noted last century from observations of planets in our own solar system. These four data points from Jupiter, Saturn, Uranus, and Neptune have served as a corner stone of planet formation theory. Here we add another point in the mass-metallicity trend from a detailed observational study of the extrasolar planet HAT-P-26b, which inhabits the critical mass regime near Neptune and Uranus. Neptune-sized worlds are among the most common planets in our galaxy and frequently exist in orbital periods very different from that of our own solar system ice giants. Atmospheric studies are the principal window into these worlds, and thereby into their formation and evolution, beyond those of our own solar system. Using the Hubble Space Telescope and Spitzer, from the optical to the infrared, we conducted a detailed atmospheric study of the Neptune-mass exoplanet HAT-P-26b over 0.5 to 4.5 μm. We detect prominent H2O absorption at 1.4 μm to 525 ppm in the atmospheric transmission spectrum. We determine that HAT-P-26b’s atmosphere is not rich in heavy elements (≈1.8×solar), which goes distinctly against the solar system mass-metallicity trend. This likely indicates that HAT-P-26b’s atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime with little contamination from metal-rich planetesimals.

HAT-P-26b: A Neptune-mass Exoplanet with Primordial Solar Heavy Element Abundance

NASA Astrophysics Data System (ADS)

Wakeford, Hannah; Sing, David; Deming, Drake; Kataria, Tiffany; Lopez, Eric

2016-10-01

A trend in giant planet mass and atmospheric heavy elemental abundance was first noted last century from observations of planets in our own solar system. These four data points from Jupiter, Saturn, Uranus, and Neptune have served as a corner stone of planet formation theory. Here we add another point in the mass-metallicity trend from a detailed observational study of the extrasolar planet HAT-P-26b, which inhabits the critical mass regime near Neptune and Uranus. Neptune-sized worlds are among the most common planets in our galaxy and frequently exist in orbital periods very different from that of our own solar system ice giants. Atmospheric studies are the principal window into these worlds, and thereby into their formation and evolution, beyond those of our own solar system. Using the Hubble Space Telescope and Spitzer, from the optical to the infrared, we conducted a detailed atmospheric study of the Neptune-mass exoplanet HAT-P-26b over 0.5 to 4.5 μm. We detect prominent H2O absorption at 1.4 μm to 525 ppm in the atmospheric transmission spectrum. We determine that HAT-P-26b's atmosphere is not rich in heavy elements (≈1.8×solar), which goes distinctly against the solar system mass-metallicity trend. This likely indicates that HAT-P-26b's atmosphere is primordial and obtained its gaseous envelope late in its disk lifetime with little contamination from metal-rich planetesimals.

Tilting Uranus without a Collision

NASA Astrophysics Data System (ADS)

Rogoszinski, Zeeve; Hamilton, Douglas P.

2016-10-01

The most accepted hypothesis for the origin of Uranus' 98° obliquity is a giant collision during the late stages of planetary accretion. This model requires a single Earth mass object striking Uranus at high latitudes; such events occur with a probability of about 10%. Alternatively, Uranus' obliquity may have arisen from a sequence of smaller impactors which lead to a uniform distribution of obliquities. Here we explore a third model for tilting Uranus using secular spin-orbit resonance theory. We investigate early Solar System configurations in which a secular resonance between Uranus' axial precession frequency and another planet's orbital node precession frequency might occur.Thommes et al. (1999) hypothesized that Uranus and Neptune initially formed between Jupiter and Saturn, and were then kicked outward. In our scenario, Neptune leaves first while Uranus remains behind. As an exterior Neptune slowly migrates outward, it picks up both Uranus and Saturn in spin-orbit resonances (Ward and Hamilton 2004; Hamilton and Ward 2004). Only a distant Neptune has a nodal frequency slow enough to resonate with Uranus' axial precession.This scenario, with diverging orbits, results in resonance capture. As Neptune migrates outward its nodal precession slows. While in resonance, Uranus and Saturn each tilt a bit further, slowing their axial precession rates to continually match Neptune's nodal precession rate. Tilting Uranus to high obliquities takes a few 100 Myrs. This timescale may be too long to hold Uranus captive between Jupiter and Saturn, and we are investigating how to reduce it. We also find that resonance capture is rare if Uranus' initial obliquity is greater than about 10°, as the probability of capture decreases as the planet's initial obliquity increases. We will refine this estimate by quantifying capture statistics, and running accretion simulations to test the likelihood of a low early obliquity. Our preliminary findings show that most assumptions about planetary accretion lead to nearly isotropic obliquity distributions for early Uranus. Thus, the odds of Uranus having an initial low obliquity is also about 10%.

Hubble Space Telescope Wide Field Planetary Camera 2 Observations of Neptune

NASA Technical Reports Server (NTRS)

1995-01-01

Two groups have recently used the Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC 2) to acquire new high-resolution images of the planet Neptune. Members of the WFPC-2 Science Team, lead by John Trauger, acquired the first series of images on 27 through 29 June 1994. These were the highest resolution images of Neptune taken since the Voyager-2 flyby in August of 1989. A more comprehensive program is currently being conducted by Heidi Hammel and Wes Lockwood. These two sets of observations are providing a wealth of new information about the structure, composition, and meteorology of this distant planet's atmosphere.

Neptune is currently the most distant planet from the sun, with an orbital radius of 4.5 billion kilometers (2.8 billion miles, or 30 Astronomical Units). Even though its diameter is about four times that of the Earth (49,420 vs. 12,742 km), ground-based telescopes reveal a tiny blue disk that subtends less than 1/1200 of a degree (2.3 arc-seconds). Neptune has therefore been a particularly challenging object to study from the ground because its disk is badly blurred by the Earth's atmosphere. In spite of this, ground-based astronomers had learned a great deal about this planet since its position was first predicted by John C. Adams and Urbain Leverrier in 1845. For example, they had determined that Neptune was composed primarily of hydrogen and helium gas, and that its blue color caused by the presence of trace amounts of the gas methane, which absorbs red light. They had also detected bright cloud features whose brightness changed with time, and tracked these clouds to infer a rotation period between 17 and 22 hours.

When the Voyager-2 spacecraft flew past the Neptune in 1989, its instruments revealed a surprising array of meteorological phenomena, including strong winds, bright, high-altitude clouds, and two large dark spots attributed to long-lived giant storm systems. These bright clouds and dark spots were tracked as they moved across the planet's disk, revealing wind speeds as large as 325 meters per second (730 miles per hour). The largest of the giant, dark storm systems, called the 'Great Dark Spot', received special attention because it resembled Jupiter's Great Red Spot, a storm that has persisted for more than three centuries. The lifetime of Neptune's Great Dark Spot could not be determined from the Voyager data alone, however, because the encounter was too brief. Its evolution was impossible to monitor with ground-based telescopes, because it could not be resolved on Neptune's tiny disk, and its contribution to the disk-integrated brightness of Neptune confused by the presence of a rapidly-varying bright cloud feature, called the 'Bright Companion' that usually accompanied the Great Dark spot.

The repaired Hubble Space Telescope provides new opportunities to monitor these and other phenomena in the atmosphere of the most distant planet. Images taken with WFPC-2's Planetary Camera (PC) can resolve Neptune's disk as well as most ground-based telescopes can resolve the disk of Jupiter. The spatial resolution of the HST WFPC-2 images is not as high as that obtained by the Voyager-2 Narrow-Angle Camera during that spacecraft's closest approach to Neptune, but they have a number of other assets that enhance their scientific value, including improved ultra-violet and infrared sensitivity, better signal-to-noise, and, and greater photometric accuracy.

The images of Neptune acquired by the WFPC-2 Science team in late June clearly demonstrate these capabilities. The side of the planet facing the Earth at the start of the program (11:36 Universal Time on July 27) was imaged in color filters spanning the ultraviolet (255 and 300-nm), visible (467, 588, 620, and 673- nm), and near-infrared (890-nm) parts of the spectrum. The planet then rotated 180 degrees in longitude, and the opposite hemisphere was imaged in a subset of these colors (300, 467, 588, 620, and 673-nm). The HST/WFPC-2 program more recently conducted by Hammel and Lockwood provides better longitude coverage, and a wider range of observing times, but uses a more restricted set of colors.

The ultraviolet pictures show an almost featureless disk that is slightly darker near the edge. The observed contrast increases in the blue, green, red, and near-infrared images, which reveal many of the features seen by Voyager 2, including the dark band near 60 S latitude and several distinct bright cloud features. The bright cloud features are most obvious in the red and infrared parts of the spectrum where methane gas absorbs most strongly (619 and 890 nm). These bright clouds thought to be high above the main cloud deck, and above much of the absorbing methane gas. The edge of the planet's disk also appears somewhat bright in these colors, indicating the presence of a ubiquitous, high-altitude haze layer.

The northern hemisphere is occupied by a single prominent cloud band centered near 30 N latitude. This planet-encircling feature may be the same bright cloud discovered last fall by ground-based observers. Northern hemisphere clouds were much less obvious at the time of the Voyager-2 encounter. The tropics are about 20 % darker than the disk average in the 890-nm images, and one of these images reveals a discrete bright cloud on the equator, near the edge of the disk. The southern hemisphere includes two broken bright bands. The largest and brightest is centered at 30 S latitude, and extends for least 40 degrees of longitude, like the Bright Companion to the Great Dark Spot. There is also a thin cloud band at 45 S latitude, which almost encircles the planet.

One feature that is conspicuous by its absence is the storm system known as the Great Dark Spot. The second smaller dark spot, DS2, that was seen during the Voyager-2 encounter was also missing. The absence of these dark spots was one of the biggest surprises of this program. The WFPC-2 Science team initially assumed that the two storm systems might be near the edge of the planet's disk, where they would not be particularly obvious. An analysis of their longitude coverage revealed that less than 20 degrees of longitude had been missed in the colors where these spots had their greatest contrast (467 and 588 nm). The Great Dark Spot covered almost 40 degrees of longitude at the time of the Voyager-2 fly-by. Even if it were on the edge of the disk, it would appear as a 'bite' out of the limb. Because no such feature was detected, we concluded that these features had vanished. This conclusion was reinforced by the more recent observations by Hammel and Lockwood, which also show no evidence of discrete dark spots.

These dramatic changes in the large-scale storm systems and planet-encircling clouds bands on Neptune are not yet completely understood, but they emphasize the dynamic nature of this planet's atmosphere, and the need for further monitoring. Additional HST WFPC-2 observations are planned for next summer. These two teams are continuing their analysis of these data sets to place improved constraints on these and other phenomena in Neptune's atmosphere.

Figure Captions:

These almost true-color pictures of Neptune were constructed from HST/WFPC2 images taken in blue (467-nm), green (588- nm), and red (673-nm) spectral filters. There is a bright cloud feature at the south pole, near the bottom right of the image. Bright cloud bands can be seen at 30S and 60S latitude. The northern hemisphere also includes a bright cloud band centered near 30N latitude. The second picture was compiled from images taken after the planet had rotated about 180 degrees of longitude (about 9 hours later) to show the opposite hemisphere.

The Wide Field/Planetary Camera 2 was developed by the Jet Propulsion Laboratory and managed by the Goddard Spaced Flight Center for NASA's Office of Space Science.

This image and other images and data received from the Hubble Space Telescope are posted on the World Wide Web on the Space Telescope Science Institute home page at URL http://oposite.stsci.edu/pubinfo/

77 FR 11571 - Notice of Intent To Repatriate Cultural Items: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2012-02-27

... Fowler Museum at UCLA acquired these unassociated funerary objects from Mr. Applegate in 1968 as part of... and the northern region of present day Mexico from time immemorial. Therefore, The Four Southern..., and other evidence, the Zuni Tribe of the Zuni Reservation, New Mexico, claims cultural affiliation...

Gift of $750-Million in Art to UCLA Would Be Biggest in American Higher Education.

ERIC Educational Resources Information Center

Desruisseaux, Paul

1987-01-01

An "agreement in principle" outlines a plan for the transfer of the art collections owned by the Norton Simon Foundation and the Norton Simon Art Foundation to UCLA, which would assume responsibility for operating the Norton Simon Museum in Pasadena, where much of the art is now exhibited. (MLW)

76 FR 36148 - Notice of Inventory Completion: Fowler Museum at UCLA, Los Angeles, CA

Federal Register 2010, 2011, 2012, 2013, 2014

2011-06-21

... was found in the Bird and Mammal collection of the UCLA Department of Biology and subsequently...: Based on the analysis performed by a physical anthropologist it is determined that the mandible is... the physical remains of one individual of Native American ancestry. Pursuant to 43 CFR 10.11(c)(1...

Occupational Analysis: Hospital Radiologic Technologist. The UCLA Allied Health Professions Project.

ERIC Educational Resources Information Center

Reeder, Glenn D.; And Others

In an effort to meet the growing demand for skilled radiologic technologists and other supportive personnel educated through the associate degree level, a national survey was conducted as part of the UCLA Allied Health Professions Project to determine the tasks performed by personnel in the field and lay the groundwork for development of…

On the methane opacity for Uranus and Neptune.

NASA Technical Reports Server (NTRS)

Trafton, L.

1972-01-01

The contribution of methane to the thermal opacity in the atmospheres of Uranus and Neptune is shown to be negligible. The relevance of this finding lies in the importance of knowing all the sources of thermal opacity to include in models of these atmospheres, for only then may it be possible to deduce their atmospheric structure and composition correctly.

Performance of three-way data types during Voyager's encounter with Neptune

NASA Technical Reports Server (NTRS)

Roth, D. C.; Taylor, T. H.; Jacobson, R. A.; Lewis, G. D.

1990-01-01

Voyager's flyby of Neptune in August of 1989 was the most distant planetary encounter ever achieved. Round trip light travel time was more than eight hours, exceeding view periods at two of the three tracking station sites. Consequently, the majority of radiometric tracking was accomplished by transmitting the uplink from one station, and receiving the downlink at a different station. This procedure defines three-way data. Dependence on three-way data for orbit determination is one distinguishing element of Voyager's successful encounter with Neptune. This paper addresses the performance of three-way range and Doppler data supporting pre-encounter orbit determination and post-encounter orbit reconstruction. Also, calibrations which reduce systematic errors inherent to three-way data are described and analyzed.

Infrared radiometry of Uranus and Neptune at 21 and 32 microns

NASA Technical Reports Server (NTRS)

Orton, Glenn S.; Baines, Kelvin H.; Bergstralh, Jay T.; Brown, Robert H.; Caldwell, John

1987-01-01

Mauna Kea's NASA IRTF has been used to obtain 21- and 32-cm radiometric measurements of Uranus and Neptune; brightness temperatures of 54.1 + or - 0.3 K for Uranus and 58.1 + or 0.3 K for Neptune were obtained by calibrating the 21-cm data against Alpha Boo. A calibration of the 32-cm data against Callisto and Ganymede yielded respective temperatures of 51.8 + or - 1.5 K and 55.6 + or - 1.2 K. The general decrease of brightness temperatures with wavelength from 20 to 30 microns is confirmed. The two planets are noted to appear as bodies sufficiently different to depart from the hypothesis of smooth planetary bulk property variation as a function of heliocentric distance.

Temperature and thermal emissivity of the surface of Neptune's satellite Triton

NASA Technical Reports Server (NTRS)

Nelson, Robert M.; Smythe, William D.; Wallis, Brad D.; Horn, Linda J.; Lane, Arthur L.; Mayo, Marvin J.

1990-01-01

Analysis of the preliminary results from the Voyager mission to the Neptune system has provided the scientific community with several methods by which the temperature of Neptune's satellite Triton may be determined. If the 37.5 K surface temperature reported by several Voyager investigations is correct, then the photometry reported by the imaging experiment on Voyager requires that Triton's surface have a remarkably low emissivity. Such a low emissivity is not required in order to explain the photometry from the photopolarimeter experiment on Voyager. A low emissivity would be inconsistent with Triton having a rough surface at the about 100-micron scale as might be expected given the active renewal processes which appear to dominate Triton's surface.

Laboratory Simulations on Haze Formation in Cool Exoplanet Atmospheres

NASA Astrophysics Data System (ADS)

He, Chao; Horst, Sarah; Lewis, Nikole; Yu, Xinting; McGuiggan, Patricia; Moses, Julianne I.

2017-10-01

The Kepler mission has shown that the most abundant types of planets are super-Earths and mini-Neptunes among ~3500 confirmed exoplanets, and these types of exoplanets are expected to exhibit a wide variety of atmospheric compositions. Recent transit spectra have demonstrated that clouds and/or hazes could play a significant role in these planetary atmospheres (Deming et al. 2013, Knutson et al. 2014, Kreidberg et al. 2014, Pont, et al. 2013). However, very little laboratory work has been done to understand the formation of haze over a broad range of atmospheric compositions. Here we conducted a series of laboratory simulations to investigate haze formation in a range of planetary atmospheres using our newly built Planetary HAZE Research (PHAZER) chamber (He et al. 2017). We ran experimental simulations for nine different atmospheres: three temperatures (300 K, 400 K, and 600 K) and three metallicities (100, 1000, and 10000 times solar metallicity) using AC glow discharge as an energy source to irradiate gas mixtures. We found that haze particles are formed in all nine experiments, but the haze production rates are dramatically different for different cases. We investigated the particle sizes of the haze particles deposited on quartz discs using atomic force microscopy (AFM). The AFM images show that the particle size varies from 30 nm to 200 nm. The haze particles are more uniform for 100x solar metallicity experiments (30 nm to 40 nm) while the particles sizes for 1000x and 10000x solar metallicity experiments have wider distributions (30 nm to 200 nm). The particle size affects the scattering of light, and thus the temperature structure of planetary atmospheres. The haze production rates and particle size distributions obtained here can serve as critical inputs to atmospheric physical and chemical tools to understand the exoplanetary atmospheres and help guide future TESS and JWST observations of super-Earths and mini-Neptunes.Ref:Deming, D., et al. 2013, ApJ, 774, 95.He, C., et al. 2017, APJL, 841, L31.Knutson, H. A., et al. 2014, Nat. 505, 66.Kreidberg, L., et al. 2014, Nat. 505, 69.Pont, F., et al. 2013, MNRAS, 432, 2917.

Dynamic compression of water to 700 GPa: single- and double shock experiments on Sandia's Z machine, first principles simulations, and structure of water planets

NASA Astrophysics Data System (ADS)

Mattsson, Thomas R.

2011-11-01

Significant progress has over the last few years been made in high energy density physics (HEDP) by executing high-precision multi-Mbar experiments and performing first-principles simulations for elements ranging from carbon [1] to xenon [2]. The properties of water under HEDP conditions are of particular importance in planetary science due to the existence of ice-giants like Neptune and Uranus. Modeling the two planets, as well as water-rich exoplanets, requires knowing the equation of state (EOS), the pressure as a function of density and temperature, of water with high accuracy. Although extensive density functional theory (DFT) simulations have been performed for water under planetary conditions [3] experimental validation has been lacking. Accessing thermodynamic states along planetary isentropes in dynamic compression experiments is challenging because the principal Hugoniot follows a significantly different path in the phase diagram. In this talk, we present experimental data for dynamic compression of water up to 700 GPa, including in a regime of the phase-diagram intersected by the Neptune isentrope and water-rich models for the exoplanet GJ436b. The data was obtained on the Z-accelerator at Sandia National Laboratories by performing magnetically accelerated flyer plate impact experiments measuring both the shock and re-shock in the sample. The high accuracy makes it possible for the data to be used for detailed model validation: the results validate first principles based thermodynamics as a reliable foundation for planetary modeling and confirm the fine effect of including nuclear quantum effects on the shock pressure. Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under Contract No. DE-AC04-94AL85000. [4pt] [1] M.D. Knudson, D.H. Dolan, and M.P. Desjarlais, SCIENCE 322, 1822 (2008).[0pt] [2] S. Root, et al., Phys. Rev. Lett. 105, 085501 (2010).[0pt] [3] M. French, et al., Phys. Rev. B 79, 054107 (2009).

Binaries in Transneptunian Resonances: Evidence for Slow Migration of Neptune?

NASA Technical Reports Server (NTRS)

Noll, Keith

2012-01-01

A distinguishing feature of trans neptunian objects (TNO) is the high fraction that arc binary. This is particularly true for the Cold Classicals (CC), objects in lowe and low i orbits concentrated between the 3:2 and 2: 1 mean-motion resonances. CCs have other physical markers: red colors, high albedos, and equal-mass binaries. The CCs appear to be a coherent and physically distinct population of planetesimals that has survived to the present with their physical properties relatively unaltered. Their spatial concentration between 39.4 and 47.7 AU has made identification of the CCs as a physical group possible. However, objects that started out as CCs arc almost certainly 1101 limited to this one dynamical niche. We can, therefore, use the measurable physical properties of CCs as tracers of Neptune-driven dynamical mixing in the Kuiper Belt. As Neptune migrated, its mean-motion resonances preceded it into the planetesimal disk. The efficiency of capture into mean motion resonances depends on the smoothness of Neptune's migration and the local population available to be captured. The two strongest resonances, the 3:2 at 39.4 AU and 2: 1 at 47.7 AU, straddle the core repository of the physically distinct CCs, providing a unique opportunity to test the details of Neptune's migration. Smooth migration should result in a measurable difference between the 3:2 and 2:1 with low inclination 2:1s having a red, binary population mirroring that of the CC itself while the 3:2 will be less contaminated. Alternative models with rapid migration would generate a more homogeneous result.

Neptune's Discovery: Le Verrier, Adams, and the Assignment of Credit

NASA Astrophysics Data System (ADS)

Sheehan, William

2011-01-01

As one of the most significant achievements of 19th century astronomy, the discovery of Neptune has been the subject of a vast literature. A large part of this literature--beginning with the period immediately after the optical discovery in Berlin--has been the obsession with assigning credit to the two men who attempted to calculate the planet's position (and initially this played out against the international rivalry between France and England). Le Verrier and Adams occupied much different positions in the Scientific Establishments of their respective countries; had markedly different personalities; and approached the investigation using different methods. A psychiatrist and historian of astronomy tries to provide some new contexts to the familiar story of the discovery of Neptune, and argues that the personalities of these two men played crucial roles in their approaches to the problem they set themselves and the way others reacted to their stimuli. Adams had features of high-functioning autism, while Le Verrier's domineering, obsessive, orderly personality--though it allowed him to be immensely productive--eventually led to serious difficulties with his peers (and an outright revolt). Though it took extraordinary smarts to calculate the position of Neptune, the discovery required social skills that these men lacked--and thus the process to discovery was more bumbling and adventitious than it might have been. The discovery of Neptune occurred at a moment when astronomy was changing from that of heroic individuals to team collaborations involving multiple experts, and remains an object lesson in the sociological aspects of scientific endeavor.

Dynamics of the Trans-Neptune Region: Apsidal Waves in the Kuiper Belt

NASA Technical Reports Server (NTRS)

Ward, William R.; Hahn, Joseph M.

1998-01-01

The role of apsidal density waves propagating in a primordial trans-Neptune disk (i.e., Kuiper belt) is investigated. It is shown that Neptune launches apsidal waves at its secular resonance near 40 AU that propagate radially outward, deeper into the particle disk. The wavelength of apsidal waves is considerably longer than waves that might be launched at Lindblad resonances, because the pattern speed, g(sub s), resulting from the apsis precession of Neptune is much slower than its mean motion, Omega(sub s). If the early Kuiper belt had a sufficient surface density, sigma, the disk's wave response to Neptune's secular perturbation would have spread the disturbing torque radially over a collective scale lambda(sub *) approx. = r(2(mu)(sub d)Omega/ absolute value of r dg/dr)(sup 1/2), where mu(sub d)equivalent pi(sigma)r(exp 2)/(1 solar mass) and Omega(r) and g(r) are respectively the mean motion and precession frequency of the disk particles. This results in considerably smaller eccentricities at resonance than had the disk particles been treated as noninteracting test particles. Consequently, particles are less apt to be excited into planet-crossing orbits, implying that the erosion timescales reported by earlier test-particle simulations of the Kuiper belt may be underestimated. It is also shown that the torque the disk exerts upon the planet (due to its gravitational attraction for the disk's spiral wave pattern) damps the planet's eccentricity and further inhibits the planet's ability to erode the disk. Key words: celestial mechanics, stellar dynamics - comets: general minor planets, asteroids

Spectroscopic Characterization of a Newborn Neptune-Sized Planet

NASA Astrophysics Data System (ADS)

Benneke, Bjoern

2016-10-01

The study of planet formation as it occurs has remained an elusive frontier, until now. Our team recently identified a newly-born planet orbiting a young, 5-10 Myr old, pre-main-sequence M star in the Upper Scorpius star-forming region. In its early stage, the close-in planet is about 50% larger than Neptune. Models predict that it will contract over the coming 100-1000 Myr to become a member of the intriguingly abundant class of close-in sub-Neptunes. Spectroscopic observations of this newborn planet will give us the unprecedented opportunity to probe the formation and evolution of low-mass, close-in planets at this early stage. Here, we propose to a reconnaissance study to probe the adolescent state of the gravitationally-bound atmosphere using near-infrared transit spectroscopy and the planet's hydrogen loss rate using far-UV transit spectroscopy. Together, our observations will give us unparalleled insights into the initial state of a young close-in planet as well as into the competing timescales of Kelvin-Helmholtz contraction and envelope mass-loss involved in the early evolution of close-in sub-Neptunes and Neptunes. If the proposed reconnaissance observations detect that molecular absorption in the atmosphere of USco 1610-1919b, then USco 1610-1919b will be one of the prime targets for the 200-hour JWST/NIRISS GTO program to probe the formation and evolution of exoplanets. Mid-cycle observations are required because the final target list for JWST/GTO programs must be locked in by June 2017 before the beginning of HST Cycle 25.

Performance Analysis and Optimization on the UCLA Parallel Atmospheric General Circulation Model Code

NASA Technical Reports Server (NTRS)

Lou, John; Ferraro, Robert; Farrara, John; Mechoso, Carlos

1996-01-01

An analysis is presented of several factors influencing the performance of a parallel implementation of the UCLA atmospheric general circulation model (AGCM) on massively parallel computer systems. Several modificaitons to the original parallel AGCM code aimed at improving its numerical efficiency, interprocessor communication cost, load-balance and issues affecting single-node code performance are discussed.

The Effects of Positively and Negatively Worded Items on the Factor Structure of the UCLA Loneliness Scale

ERIC Educational Resources Information Center

Dodeen, Hamzeh

2015-01-01

The purpose of this study was to evaluate the factor structure of the University of California, Los Angeles (UCLA) Loneliness Scale and examine possible wording effects on a sample of 1,429 students from the United Arab Emirates University. Correlated traits-correlated uniqueness as well as correlated traits-correlated methods were used to examine…

Twelve-year planetary ephemeris: 1995-2006

NASA Technical Reports Server (NTRS)

Espenak, Fred

1994-01-01

Accurate geocentric positions and physical ephemerides are tabulated for the Sun, Moon, Mercury, Venus, Mars, Jupiter, Saturn, Uranus, Neptune, and Pluto for the 12-year period 1995 through 2006. The frequency interval is 2 days for the Sun and classical planets. Uranus, Neptune, and Pluto are tabulated at 4-day intervals. Because of its rapid apparent motion, the Moon's ephemeris is given daily.

On the unique structure of the magnetic fields of Uranus and Neptune

NASA Technical Reports Server (NTRS)

Dolginov, Sh. SH.

1993-01-01

The magnetic fields of Uranus and Neptune, which have comparable dipole, quadrupole, and octupole harmonics, are unique in the present-day solar system, but they resemble the geomagnetic field at the epochs of excursions and reversals known from paleomagnetic data. The precession dynamo model, in which the dominant role in the generation of the planetary magnetic fields is played by external gravitational forces, allows us to propose two scenarios for the formation of the unique topology of the magnetic fields of Uranus and Neptune. In the first case, tidal flows in the 'oceans' of these two planets extend down to the depths where the matter has a noticeable electric conductivity and velocity. A hydromagnetic interaction of the moving conducting fluid with the planetary magnetic field outside the generation region results in the deformation of the field and the deceleration of the motion under the action of the radial magnetic field. In the second case, the deformation of the field facilitates drastic changes in cyclonic cells within the generation region causing instabilities that result in a multi-polar field structure, excursions, and inversions. This paper considers this problem in greater detail by using the Neptune-Triton system as an example.

AxIOM: Amphipod crustaceans from insular Posidonia oceanica seagrass meadows

PubMed Central

Heughebaert, André; Lepoint, Gilles

2016-01-01

Abstract Background The Neptune grass, Posidonia oceanica (L.) Delile, 1813, is the most widespread seagrass of the Mediterranean Sea. This foundation species forms large meadows that, through habitat and trophic services, act as biodiversity hotspots. In Neptune grass meadows, amphipod crustaceans are one of the dominant groups of vagile invertebrates, forming an abundant and diverse taxocenosis. They are key ecological components of the complex, pivotal, yet critically endangered Neptune grass ecosystems. Nevertheless, comprehensive qualitative and quantitative data about amphipod fauna found in Mediterranean Neptune grass meadows remain scarce, especially in insular locations. New information Here, we provide in-depth metadata about AxIOM, a sample-based dataset published on the GBIF portal. AxIOM is based on an extensive and spatially hierarchized sampling design with multiple years, seasons, day periods, and methods. Samples were taken along the coasts of Calvi Bay (Corsica, France) and of the Tavolara-Punta Coda Cavallo Marine Protected Area (Sardinia, Italy). In total, AxIOM contains 187 samples documenting occurrence (1775 records) and abundance (10720 specimens) of amphipod crustaceans belonging to 72 species spanning 29 families. The dataset is available at http://ipt.biodiversity.be/resource?r=axiom. PMID:27660521

Dynamical evolution of a fictitious population of binary Neptune Trojans

NASA Astrophysics Data System (ADS)

Brunini, Adrián

2018-03-01

We present numerical simulations of the evolution of a synthetic population of Binary Neptune Trojans, under the influence of the solar perturbations and tidal friction (the so-called Kozai cycles and tidal friction evolution). Our model includes the dynamical influence of the four giant planets on the heliocentric orbit of the binary centre of mass. In this paper, we explore the evolution of initially tight binaries around the Neptune L4 Lagrange point. We found that the variation of the heliocentric orbital elements due to the libration around the Lagrange point introduces significant changes in the orbital evolution of the binaries. Collisional processes would not play a significant role in the dynamical evolution of Neptune Trojans. After 4.5 × 109 yr of evolution, ˜50 per cent of the synthetic systems end up separated as single objects, most of them with slow diurnal rotation rate. The final orbital distribution of the surviving binary systems is statistically similar to the one found for Kuiper Belt Binaries when collisional evolution is not included in the model. Systems composed by a primary and a small satellite are more fragile than the ones composed by components of similar sizes.

High quality single shot diffraction patterns using ultrashort megaelectron volt electron beams from a radio frequency photoinjector.

PubMed

Musumeci, P; Moody, J T; Scoby, C M; Gutierrez, M S; Bender, H A; Wilcox, N S

2010-01-01

Single shot diffraction patterns using a 250-fs-long electron beam have been obtained at the UCLA Pegasus laboratory. High quality images with spatial resolution sufficient to distinguish closely spaced peaks in the Debye-Scherrer ring pattern have been recorded by scattering the 1.6 pC 3.5 MeV electron beam generated in the rf photoinjector off a 100-nm-thick Au foil. Dark current and high emittance particles are removed from the beam before sending it onto the diffraction target using a 1 mm diameter collimating hole. These results open the door to the study of irreversible phase transformations by single shot MeV electron diffraction.

Observation of two new L4 Neptune Trojans in the Dark Energy Survey supernova fields

DOE PAGES

Gerdes, D. W.

2016-01-28

We report the discovery of the eighth and ninth known Trojans in stable orbits around Neptune's leading Lagrange point, L4. The objects 2014 QO 441 and 2014 QP 441 were detected in data obtained during the 2013-14 and 2014-15 observing seasons by the Dark Energy Survey, using the Dark Energy Camera (DECam) on the 4-meter Blanco telescope at Cerro Tololo Inter- American Observatory. Both are in high-inclination orbits (18.8° and 19.4° respectively). Furthermore, with an eccentricity of 0.104, 2014 QO 441 has the most eccentric orbit of the eleven known stable Neptune Trojans. We describe the search procedure and investigatemore » the objects' long-term dynamical stability and physical properties.« less

Neptune's small dark spot (D2)

NASA Technical Reports Server (NTRS)

1999-01-01

This bulls-eye view of Neptune's small dark spot (D2) was obtained by Voyager 2's narrow-angle camera. Banding surrounding the feature indicates unseen strong winds, while structures within the bright spot suggest both active upwelling of clouds and rotation about the center. A rotation rate has not yet been measured, but the V-shaped structure near the right edge of the bright area indicates that the spot rotates clockwise. Unlike the Great Red Spot on Jupiter, which rotates counterclockwise, if the D2 spot on Neptune rotates clockwise, the material will be descending in the dark oval region. The fact that infrared data will yield temperature information about the region above the clouds makes this observation especially valuable. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

User Language Specification

DTIC Science & Technology

1977-06-30

Digital System Design based on Structural and Function Modeling. Computer Science Dept., UCLA, (UCLA-ENG-7488), 1975. [7] Hamlet, R. G. High-level...of libaries of pro- grams where each library represents a coherent set of data types and parameterized nodes which operate on those types. * Allow...following form: an optional minus sign, concatenated with an optional sequence of digits the first of which is nonzero, concatenated with a single

The Function of Neuroendocrine Cells in Prostate Cancer

DTIC Science & Technology

2015-06-20

Comprehensive Cancer Center and 4Broad Center for Regenerative Medicine and Stem Cell Biology, David Geffen School of Medicine at UCLA, 10833 Le Conte... Regenerative Medicine and Stem Cell Research, UCLA David Geffen School of Medicine , Los Angeles, California. 2Department of Urology, The First...progress in prostate cancer. Soochou University Annual Translational Medicine Meeting, Suzhou, China, November 2013 21. Prostate Cancer Stem Cells

Vector Fluxgate Magnetometer (VMAG) Development for DSX

DTIC Science & Technology

2008-05-19

AFRL-RV-HA-TR-2008-1108 Vector Fluxgate Magnetometer (VMAG) Development for DSX Mark B. Moldwin Q. O O O I- UCLA Q Institute of...for Public Release; Distribution Unlimited. 13. SUPPLEMENTARY NOTES 14. ABSTRACT UCLA is building a three-axis fluxgate magnetometer for the Air... fluxgate magnetometer provides the necessary data to support both the Space Weather (SWx) specification and mapping requirements and the WPIx

Educating European Corporate Communication Professionals for Senior Management Positions: A Collaboration between UCLA's Anderson School of Management and the University of Lugano

ERIC Educational Resources Information Center

Forman, Janis

2005-01-01

UCLA's program in strategic management for European corporate communication professionals provides participants with a concentrated, yet selective, immersion in those management disciplines taught at U.S. business schools, topics that are essential to their work as senior advisors to CEOs and as leaders in the field. The choice of topics…

Identifying Therapeutics for Platinum-Resistant Ovarian Cancer by Next Generation Mechanotyping

DTIC Science & Technology

2017-09-01

period, we have successfully advanced and integrated the PMF technology into the Molecular Shared Screening Resource at UCLA, thereby establishing the...will validate the effects of the lead compounds on cisplatin- resistant ovarian cancer cells, including cellular and molecular analyses. 15. SUBJECT...throughput screening facility at UCLA, the Molecular Shared Screening Resource (MSSR). Due to technical hurdles in the integration process, and reduced

Why Race and Culture Matter in Schools, and Why We Need to "Get This Right": A Conversation with Dr. Tyrone Howard

ERIC Educational Resources Information Center

Clark, Pat; Zygmunt, Eva; Howard, Tyrone

2016-01-01

Tyrone Howard is Professor of Education at UCLA; Associate Dean of Equity, Diversity, and Inclusion; and former Director of Center X, which is where UCLA's teacher education program is housed. Center X provides a unique setting where researchers and practitioners collaborate to design and conduct programs that prepare and support K-12 teachers and…

Exploring Your Universe at UCLA: Steps to Developing and Sustaining a Large STEM Event

NASA Astrophysics Data System (ADS)

Curren, I. S.; Vican, L.; Sitarski, B.; Jewitt, D. C.

2015-12-01

Public STEM events are an excellent method to implement informal education and for scientists and educators to interact with their community. The benefits of such events are twofold. First and foremost, science enthusiasts and students both young and old, in particular, are exposed to STEM in a way that is accessible, fun, and not as stringent as may be presented in classrooms where testing is an underlying goal. Second, scientists and educators are given the opportunity to engage with the public and share their science to an audience who may not have a scientific background, thereby encouraging scientists to develop good communication practices and skills. In 2009 graduate student members of Astronomy Live!, an outreach organization in the UCLA Department of Physics and Astronomy, started a free and public event on the campus that featured a dozen hands-on outreach activities. The event, though small at the time, was a success and it was decided to make it an annual occurrence. Thus, Exploring Your Universe (EYU) was born. Primarily through word of mouth, the event has grown every year, both in number of attendees and number of volunteers. In 2009, approximately 1000 people attended and 20 students volunteered over the course of an eight-hour day. In 2014, participation was at an all-time high with close to 6000 attendees and over 400 volunteers from all departments in the Division of Physical Sciences (plus many non-divisional departments and institutes, as well as non-UCLA organizations). The event, which is the largest STEM event at UCLA and one of the largest in Los Angeles, now features near 100 hands-on activities that span many STEM fields. EYU has been featured by the UCLA news outlets, Daily Bruin and UCLA Today, and is often lauded as their favorite event of the year by attendees and volunteers alike. The event is entirely student-run, though volunteers include faculty, staff, researchers and students alike. As the event has grown, new systems for managing its many aspects have been adopted. Here, we will present the details of how the event was created and has remained successful, and sustainable.

Map refinement of locus RP13 to human chromosome 17p13.3 in a second family with autosomal dominant retinitis pigmentosa

DOE Office of Scientific and Technical Information (OSTI.GOV)

Kojis, T.L.; Heinzmann, C.; Ngo, J.T.

1996-02-01

In order to elucidate the genetic basis of autosomal dominant retinitis pigmentosa (adRP) in a large eight-generation family (UCLA-RP09) of British descent, we assessed linkage between the UCLA-RP09 adRP gene and numerous genetic loci, including eight adRP candidate genes, five anonymous adRP-linked DNA loci, and 20 phenotypic markers. Linkage to the UCLA-RP09 disease gene was excluded for all eight candidate genes analyzed, including rhodopsin (RP4) and peripherin/RDS (RP7), for the four adRP loci RP1, RP9, RP10 and RP11, as well as for 17 phenotypic markers. The anonymous DNA marker locus D17S938, linked to adRP locus RP13 on chromosome 17p13.1, yieldedmore » a suggestive but not statistically significant positive lod score. Linkage was confirmed between the UCLA-RP09 adRP gene and markers distal to D17S938 in the chromosomal region 17p13.3. A reanalysis of the original RP13 data from a South African adRP family of British descent, in conjunction with our UCLA-RP09 data, suggests that only one adRP locus exists on 17p but that it maps to a more telomeric position, at band 17p13.3, than previously reported. Confirmation of the involvement of RP13 in two presumably unrelated adRP families, both of British descent, suggests that this locus is a distinct adRP gene in a proportion of British, and possibly other, adRP families. 39 refs., 4 figs., 3 tabs.« less

[Validation of the UCLA loneliness scale in an elderly population that live alone].

PubMed

Velarde-Mayol, C; Fragua-Gil, S; García-de-Cecilia, J M

2016-04-01

This article examines the growing social phenomenon of elderly people living alone from 2 points of view: the objective loneliness of living alone and the subjective loneliness of feeling lonely. To validate the UCLA loneliness scale as a tool for the overall measurement of loneliness and to determine the social profile in elderly people living alone. Observational study carried out over 2 years (2012-2013) to identify elderly people living alone; case-control study to validate the UCLA loneliness scale. The sample was taken from 3 surgeries belonging to 2 Primary Care health centres from urban and rural areas. We studied construct validity, discriminant validity and sensitivity analysis were analysed. Of the elderly population studied 22.3% live alone, 61.7% due to loss of spouse, with a mean age of 70.7 years, and 82.7% women; 17.3% have no family ties and 63.2% feel lonely. UCLA loneliness scale has a construct validity with a high correlation between items. The discriminant validity was confirmed in relation to the elderly who do not live alone, with Cronbach alpha of 0.95, and it is sensitive to change. One in 4-5 elderly live alone, mainly due to the loss of spouse. There are 3 times as many women as men who live alone. Two out of 3 experience the feeling of loneliness. The UCLA loneliness scale has proved to be a useful and sensitive tool to measure loneliness in the elderly population. Copyright © 2015 Sociedad Española de Médicos de Atención Primaria (SEMERGEN). Publicado por Elsevier España, S.L.U. All rights reserved.

Italian cross-cultural adaptation and validation of three different scales for the evaluation of shoulder pain and dysfunction after neck dissection: University of California - Los Angeles (UCLA) Shoulder Scale, Shoulder Pain and Disability Index (SPADI) and Simple Shoulder Test (SST).

PubMed

Marchese, C; Cristalli, G; Pichi, B; Manciocco, V; Mercante, G; Pellini, R; Marchesi, P; Sperduti, I; Ruscito, P; Spriano, G

2012-02-01

Shoulder syndrome after neck dissection is a well known entity, but its incidence and prognostic factors influencing recovery have not been clearly assessed due to the heterogeneity of possible evaluations. The University of California - Los Angeles (UCLA) Shoulder Scale, the Shoulder Pain and Disability Index (SPADI) and the Simple Shoulder Test (SST) are three English-language questionnaires commonly used to test shoulder impairment. An Italian version of these scales is not available. The aim of the present study was to translate, culturally adapt and validate an Italian version of UCLA Shoulder Scale, SPADI and SST. Translation and cross-cultural adaptation of the SPADI, the UCLA shoulder scale and the SST was performed according to the international guidelines. Sixty-six patients treated with neck dissection for head and neck cancer were called to draw up these scales. Forty patients completed the same questionnaires a second time one week after the first to test the reproducibility of the Italian versions. All the English-speaking Italian patients (n = 11) were asked to complete both the English and the Italian versions of the three questionnaires to validate the scales. No major problems regarding the content or the language were found during the translation of the 3 questionnaires. For all three scales, Cronbach's α was > 0.89. The Pearson correlation coefficient was r > 0.91. With respect to validity, there was a significant correlation between the Italian and the English versions of all three scales. This study shows that the Italian versions of UCLA Shoulder Scale, SPADI and SST are valid instruments for the evaluation of shoulder dysfunction after neck dissection in Italian patients.

HIV-1 subtype C unproductively infects human cardiomyocytes in vitro and induces apoptosis mitigated by an anti-Gp120 aptamer.

PubMed

Lopes de Campos, Walter R; Chirwa, Nthato; London, Grace; Rotherham, Lia S; Morris, Lynn; Mayosi, Bongani M; Khati, Makobetsa

2014-01-01

HIV-associated cardiomyopathy (HIVCM) is of clinical concern in developing countries because of a high HIV-1 prevalence, especially subtype C, and limited access to highly active antiretroviral therapy (HAART). For these reasons, we investigated the direct and indirect effects of HIV-1 subtype C infection of cultured human cardiomyocytes and the mechanisms leading to cardiomyocytes damage; as well as a way to mitigate the damage. We evaluated a novel approach to mitigate HIVCM using a previously reported gp120 binding and HIV-1 neutralizing aptamer called UCLA1. We established a cell-based model of HIVCM by infecting human cardiomyocytes with cell-free HIV-1 or co-culturing human cardiomyocytes with HIV-infected monocyte derived macrophages (MDM). We discovered that HIV-1 subtype C unproductively (i.e. its life cycle is arrested after reverse transcription) infects cardiomyocytes. Furthermore, we found that HIV-1 initiates apoptosis of cardiomyocytes through caspase-9 activation, preferentially via the intrinsic or mitochondrial initiated pathway. CXCR4 receptor-using viruses were stronger inducers of apoptosis than CCR5 utilizing variants. Importantly, we discovered that HIV-1 induced apoptosis of cardiomyocytes was mitigated by UCLA1. However, UCLA1 had no protective effective on cardiomyocytes when apoptosis was triggered by HIV-infected MDM. When HIV-1 was treated with UCLA1 prior to infection of MDM, it failed to induce apoptosis of cardiomyocytes. These data suggest that HIV-1 causes a mitochondrial initiated apoptotic cascade, which signal through caspase-9, whereas HIV-1 infected MDM causes apoptosis predominantly via the death-receptor pathway, mediated by caspase-8. Furthermore the data suggest that UCLA1 protects cardiomyocytes from caspase-mediated apoptosis, directly by binding to HIV-1 and indirectly by preventing infection of MDM.

Comparison of implant-abutment interface misfits after casting and soldering procedures.

PubMed

Neves, Flávio Domingues das; Elias, Gisele Araújo; da Silva-Neto, João Paulo; de Medeiros Dantas, Lucas Costa; da Mota, Adérito Soares; Neto, Alfredo Júlio Fernandes

2014-04-01

The aim of this study was to compare vertical and horizontal adjustments of castable abutments after conducting casting and soldering procedures. Twelve external hexagonal implants (3.75 × 10 mm) and their UCLA abutments were divided according their manufacturer and abutment type: PUN (plastic UCLA, Neodent), PUC (plastic UCLA, Conexão), PU3i (plastic UCLA, Biomet 3i), and PUTN (plastic UCLA with Tilite milled base, Neodent). Three infrastructures of a fixed partial implant-supported bridge with 3 elements were produced for each group. The measurements of vertical (VM) and horizontal (HM) misfits were obtained via scanning electron microscopy after completion of casting and soldering. The corresponding values were determined to be biomechanically acceptable to the system, and the results were rated as a percentage. Statistical analysis establishes differences between groups by chi-square after procedures, and McNeman's test was applied to analyze the influence of soldering over casting (α ≤ .05). For the values of VM and HM, respectively, when the casting process was complete, it was observed that 83.25% and 100% (PUTN), 33.3% and 27.75% (PUN), 33.3% and 88.8% (PUC), 33.3% and 94.35% (PU3i) represented acceptable values. After completing the requisite soldering, acceptable values were 50% and 94.35% (PUTN), 16.6% and 77.7% (PUN), 38.55% and 77.7% (PUC), and 27.75% and 94.35% (PU3i). Within the limitations of this study, it can be concluded that the premachined abutments presented more acceptable VM values. The HM values were within acceptable limits before and after the soldering procedure for most groups. Further, the soldering procedure resulted in an increase of VM in all groups.

Ion beam generated modes in the lower hybrid frequency range in a laboratory magnetoplasma

NASA Astrophysics Data System (ADS)

Van Compernolle, B.; Tripathi, S.; Gekelman, W. N.; Colestock, P. L.; Pribyl, P.

2012-12-01

The generation of waves by ion ring distributions is of great importance in many instances in space plasmas. They occur naturally in the magnetosphere through the interaction with substorms, or they can be man-made in ionospheric experiments by photo-ionization of neutral atoms injected perpendicular to the earth's magnetic field. The interaction of a fast ion beam with a low β plasma has been studied in the laboratory. Experiments were performed at the LArge Plasma Device (LAPD) at UCLA. The experiments were done in a Helium plasma (n ≃ 1012 \\ cm-3, B0 = 1000 G - 1800 G, fpe}/f{ce ≃ 1 - 5, Te = 0.25\\ eV, vte ≤ vA). The ion beam \\cite{Tripathi_ionbeam} is a Helium beam with energies ranging from 5 keV to 18 keV. The fast ion velocity is on the order of the Alfvén velocity. The beam is injected from the end of the machine, and spirals down the linear device. Waves were observed below fci in the shear Alfvén wave regime, and in a broad spectrum above fci in the lower hybrid frequency range, the focus of this paper. The wave spectra have distinct peaks close to ion cyclotron harmonics, extending out to the 100th harmonic in some cases. The wave generation was studied for various magnetic fields and background plasma densities, as well as for different beam energies and pitch angles. The waves were measured with 3-axis electric and magnetic probes. Detailed measurements of the perpendicular mode structure will be shown. Langmuir probes were used to measure density and temperature evolution due to the beam-plasma interaction. Retarding field energy analyzers captured the ion beam profiles. The work was performed at the LArge Plasma Device at the Basic Plasma Science Facility (BaPSF) at UCLA, funded by DOE/NSF.

Neptune: An astrophysical smooth particle hydrodynamics code for massively parallel computer architectures

NASA Astrophysics Data System (ADS)

Sandalski, Stou

Smooth particle hydrodynamics is an efficient method for modeling the dynamics of fluids. It is commonly used to simulate astrophysical processes such as binary mergers. We present a newly developed GPU accelerated smooth particle hydrodynamics code for astrophysical simulations. The code is named neptune after the Roman god of water. It is written in OpenMP parallelized C++ and OpenCL and includes octree based hydrodynamic and gravitational acceleration. The design relies on object-oriented methodologies in order to provide a flexible and modular framework that can be easily extended and modified by the user. Several pre-built scenarios for simulating collisions of polytropes and black-hole accretion are provided. The code is released under the MIT Open Source license and publicly available at http://code.google.com/p/neptune-sph/.

No evidence of rings around Neptune

NASA Technical Reports Server (NTRS)

Elliot, J. L.; Mink, D. J.; Baron, R. L.; Dunham, E.; Pingree, J. E.; French, R. G.; Elias, J. H.; Liller, W.; Nicholson, P. D.; Jones, T. J.

1981-01-01

The results of two observations of stellar occultations of Neptune to determine if the planet has a ring system are reported. The sightings were made from Mt. Stromlo, Mauna Kea, and Cerro Tololo, noting that an equatorial ring would subtend only two arcsec of view. An upper accretion limit was defined to set the region around Neptune where rings, rather than satellites, could form. The intensities of the starlight from the two selected stars were recorded by photometers on magnetic tape during the occultation period. One of the stars did not occult, but passed through the entire region where a ring system might be present. No definitive evidence for rings was found, although an optical depth for a Neptunian ring was calculated at 0.07, with a width of more than 5 km and a radius of 31,400 km.

Cameras on the NEPTUNE Canada seafloor observatory: Towards monitoring hydrothermal vent ecosystem dynamics

NASA Astrophysics Data System (ADS)

Robert, K.; Matabos, M.; Sarrazin, J.; Sarradin, P.; Lee, R. W.; Juniper, K.

2010-12-01

Hydrothermal vent environments are among the most dynamic benthic habitats in the ocean. The relative roles of physical and biological factors in shaping vent community structure remain unclear. Undersea cabled observatories offer the power and bandwidth required for high-resolution, time-series study of the dynamics of vent communities and the physico-chemical forces that influence them. The NEPTUNE Canada cabled instrument array at the Endeavour hydrothermal vents provides a unique laboratory for researchers to conduct long-term, integrated studies of hydrothermal vent ecosystem dynamics in relation to environmental variability. Beginning in September-October 2010, NEPTUNE Canada (NC) will be deploying a multi-disciplinary suite of instruments on the Endeavour Segment of the Juan de Fuca Ridge. Two camera and sensor systems will be used to study ecosystem dynamics in relation to hydrothermal discharge. These studies will make use of new experimental protocols for time-series observations that we have been developing since 2008 at other observatory sites connected to the VENUS and NC networks. These protocols include sampling design, camera calibration (i.e. structure, position, light, settings) and image analysis methodologies (see communication by Aron et al.). The camera systems to be deployed in the Main Endeavour vent field include a Sidus high definition video camera (2010) and the TEMPO-mini system (2011), designed by IFREMER (France). Real-time data from three sensors (O2, dissolved Fe, temperature) integrated with the TEMPO-mini system will enhance interpretation of imagery. For the first year of observations, a suite of internally recording temperature probes will be strategically placed in the field of view of the Sidus camera. These installations aim at monitoring variations in vent community structure and dynamics (species composition and abundances, interactions within and among species) in response to changes in environmental conditions at different temporal scales. High-resolution time-series studies also provide a mean of studying population dynamics, biological rhythms, organism growth and faunal succession. In addition to programmed time-series monitoring, the NC infrastructure will also permit manual and automated modification of observational protocols in response to natural events. This will enhance our ability to document potentially critical but short-lived environmental forces affecting vent communities.

Gravity-assist trajectories to Venus, Mars, and the ice giants: Mission design with human and robotic applications

NASA Astrophysics Data System (ADS)

Hughes, Kyle M.

Gravity-assist trajectories to Uranus and Neptune are found (with the allowance of impulsive maneuvers using chemical propulsion) for launch dates ranging from 2024 to 2038 for Uranus and 2020 to 2070 for Neptune. Solutions are found using a patched conic model with analytical ephemeris via the Satellite Tour Design Program (STOUR), originally developed at the Jet Propulsion Laboratory (JPL). Delivered payload mass is computed for all solutions for select launch vehicles, and attractive solutions are identified as those that deliver a specified amount of payload mass into orbit at the target body in minimum time. The best cases for each launch year are cataloged for orbiter missions to Uranus and Neptune. Solutions with sufficient delivered payload for a multi-planet mission (e.g. sending a probe to Saturn on the way to delivering an orbiter at Uranus) become available when the Space Launch System (SLS) launch vehicle is employed. A set of possible approach trajectories are modeled at the target planet to assess what (if any) adjustments are needed for ring avoidance, and to determine the probe entry conditions. Mars free-return trajectories are found with an emphasis on short flight times for application to near-term human flyby missions (similar to that of Inspiration Mars). Venus free-returns are also investigated and proposed as an alternative to a human Mars flyby mission. Attractive Earth-Mars free-return opportunities are identified that use an intermediate Venus flyby. One such opportunity, in 2021, has been adopted by the Inspiration Mars Foundation as a backup to the currently considered 2018 Mars free-return opportunity. Methods to establish spacecraft into Earth-Mars cycler trajectories are also investigated to reduce the propellant cost required to inject a 95-metric ton spacecraft into a cycler orbit. The establishment trajectories considered use either a V-infinity leveraging maneuver or low thrust. The V-infinity leveraging establishment trajectories are validated using patched conics via the STOUR program. Establishment trajectories that use low-thrust were investigated with particular focus on validating the patched-conic based solutions at instances where Earth encounter times are not negligible.

Vector Fluxgate Magnetometer (VMAG) Development for DSX

DTIC Science & Technology

2007-07-02

AFRL-RV-HA-TR-2007-1077 Vector Fluxgate Magnetometer (VMAG) Development for DSX -- Mark B. Moldwin 0 UCLA Institute of Geophysics and Planetary...02-07-2007IScientific Report No. 2 April 2006 - April 2007 4. TITLE AND SUBTITLE S. CONTRACT NUMBER Vector Fluxgate Magnetometer (VMAG) Development...SUPPLEMENTARY NOTES 14. ABSTRACT UCLA is building a three-axis fluxgate magnetometer for the AFRL-mission. The instrument is designed to measure the medium

Proceedings of the 2016 Workshop on the Physics and Applications of High Brightness Beams

NASA Astrophysics Data System (ADS)

Cianchi, Alessandro; Ferrario, Massimo; Musumeci, Pietro; Rosenzweig, James

2017-09-01

We are proud to present the proceedings of the latest in the series of International Committee on Future Accelerators (ICFA)-endorsed workshops on the Physics and Applications of High Brightness Beams, which has been held at the Hotel Nacional in Havana, Cuba between March 28 and April 1, 2016. In total, 135 participants coming from 14 different countries attended this historic conference. In recognition of its pioneering role in the significant blossoming of relations between Cuba and the larger scientific community, this workshop also received the endorsement of UNESCO. The workshop organization was headed by co-chairs Massimo Ferrario (INFN-LNF) and James Rosenzweig (UCLA), with the essential and energetic contributions of local organizing committee chair Fidel Antonio Castro Smirnov (InSTEC, Havana). The workshop scientific agenda was developed under the care of program committee co-chairs Pietro Musumeci (UCLA) and Luca Serafini (INFN-Milano). The publication of the proceedings we present here was led by Alessandro Cianchi (Tor Vergata). Tangible contributions to the workshop infrastructure were received from UCLA, INFN-LNF, InSTEC, EuroNNAC2, and the US National Science Foundation. The workshop web site, which contains detailed information on the scientific agenda of the meeting, is found at https://conferences.pa.ucla.edu/hbb/.

P - ρ - T data for H2O up to 260 GPa under laser-driven shock loading

NASA Astrophysics Data System (ADS)

Kimura, T.; Ozaki, N.; Sano, T.; Okuchi, T.; Shimizu, K.; Miyanishi, K.; Terai, T.; Kakeshita, T.; Sakawa, Y.; Kodama, R.

2014-12-01

H2O is believed to be one of the most abundant compounds in ice giants including Neptune and Uranus1. Therefore, equation of state (EOS) for H2O is critical for understanding the formation and evolution of these planets. Various EOS models have been suggested for modeling the interior structure of the ice giants2-4. The recent shock experiments reported that their P - ρ data of H2O are in agreement with those of the QMD based EOS model5, indicating that this model is most suitable for modeling H2O in the ice giants. Whether H2O is in the solid or liquid state in the planetary interior has a great importance to understand their internal structures6. While the QMD model predicted that the solid H2O is present in deep interior of their planets above ~100 GPa4, the recent measurements revealed that H2O remains in the liquid state even at the deep interior conditions7. This discrepancy between experimental and theoretical studies suggests that the QMD based EOS model is disputable for modeling the planetary interior. Indeed, the comparison between data obtained from the shock experiments and the QMD based EOS did not cover the temperature5. We have obtained P - ρ - T data for H2O up to 260 GPa by using laser-driven shock compression technique. The diamond cell applied for the laser shock experiments was used as the sample container in order to achieve temperature conditions lower than the principal Hugoniot states. This shock technique combined with the cell can be used for an assessment the EOS models because it is possible to compare the states under the conditions that the contrast between the models clearly appears. Our data covering P - ρ - T on both the principal and the off Hugoniot curves agree with those of the QMD model, indicating this model to be adopted as the standard for modeling the interior structures of Neptune, Uranus, and exoplanets. References 1W. B. Hubbard et al., The interior of Neptune: Neptune and Triton(Univ. Arizona Press, Tucson, 1995) p.109-138. 2S. P. Lyon and J. D. Johnson, Los Alamos Technical Report No. LA-UR-92-3407, 1992. 3F. H. Ree, Lawrence Livemore Laboratory Technical Report No. UCRL-52190, 1976. 4M. French et al., Phys. Rev. B 79, 054107 (2009). 5M. D. Knudson et al., Phys. Rev. Lett. 108, 091102 (2012). 6 R. Redmer et al., Icarus 211, 798 (2011). 7T. Kimura et al., J. Chem. Phys. 140, 074501 (2014).

Generation and Amplification of Coherent Radiation with Optical Orbital Angular Momentum in a Free-Electron Laser

NASA Astrophysics Data System (ADS)

Hemsing, Erik Willard

The object of this work is to examine how coherent light that carries orbital angular momentum (OAM) can be generated and amplified in a single pass, high-gain free-electron laser (FEL) at the fundamental operating frequency. This concept unites two rapidly expanding, but at present largely non-overlapping fields of study: high-order OAM light modes, which interact in new ways with matter, and FELs, in which a relativistically energetic electron beam emits coherent, ultra high-brightness, highly frequency-tunable light. The ability to generate OAM light in an FEL enables new regimes of laser interaction physics to be explored at wavelengths down to hard x-rays. The theoretical portion of this dissertation attempts to provide a new predictive mathematical framework. It builds on existing work, and describes the three-dimensional electromagnetic field of the high-gain FEL as a sum of OAM modes such that the amplification properties of individual modes can be characterized. The effects of uncorrelated energy spread, longitudinal space charge, energy detuning, and transverse emittance in the electron beam are included, as is the diffraction of the laser light. Theoretical predictions are corroborated by detailed numerical Genesis 1.3 simulations. When the theory is extended to frequency harmonics, a novel interaction is uncovered that generates a helical electron beam density distribution. These predictions are also supported by numerical Tredi simulations. This type of highly correlated structure is shown to naturally emit OAM light, and forms the basis of a new high-gain, high-mode generation (HGHMG) scheme proposed in its entirety here. The experimental section examines the helical microbunching concept in a proof-of-principle experiment dubbed HELIX, performed at the UCLA Neptune laboratory. We present detailed measurement of the coherent transition radiation emitted by the 12.5 MeV electron beam that is microbunched in a second harmonic interaction with an input laser and helical undulator. The predicted dependence of the CTR signal on the input laser polarization is observed, and is consistent with microbunching that has a periodicity near the 10.6 mum wavelength of the 30 MW CO2 laser pulse. Scans of the interaction energy bandwidth are consistent with predictions that indicate a dominant azimuthal density mode with a bunching factor of 10%, and thus provide indication of the first experimental evidence of helical microbunching. This result offers support for future successful realization of the proposed HGHMG scheme to generate OAM modes in high-gain FELs.

Career Guidance Lesson Plans for Grades K-12. Developed as Part of New Jersey Comprehensive Career Development Guidelines Program in Neptune Township Public Schools.

ERIC Educational Resources Information Center

Neptune Township Public Schools, NJ.

This document contains the career development scope and sequence and 39 lesson plans for career guidance activities, for grades K-5, 6-8, and 9-12, developed for use in the Neptune Township Public Schools (New Jersey). Each one-to-two-page lesson plan includes information on subject area, competency, indicators, lesson objectives, resources, time…

A Search for Small Distant Moons of Neptune

NASA Astrophysics Data System (ADS)

Holman, Matthew; Kavelaars, Jj; Gladman, Brett; Petit, Jean-Marc; Grav, Tommy; Nicholson, Philip

2002-08-01

With many new jovian, saturnian, and uranian irregular satellites having been discovered in the last few years, our attention naturally falls upon Neptune. In 1999, we conducted a search for neptunian satellites covering about 8 square degrees (almost the entire stable region around the planet). This survey yielded no new satellites down to R magnitude 24. We interpreted this as supporting a violent destruction of the Neptunian outer satellite system as Triton was captured. However, there were good reasons to believe that the largest un-discovered Neptune satellites lay just beyond the previous survey's magnitude limit. In August 2001, we used the mosaic camera on the Blanco 4-m to push down to m_R~eq25.5, to test this hypothesis. We discovered two neptunian satellites candidates. Using the time available after Neptune had set, we also discovered four faint uranian satellite candidates. However, poor weather at Palomar and Magellan in September 2001 and instrumental problems on the VLT in November 2001 prevented the tracking these candidates to conclusively prove that they are moons. We request time to repeat last summer's search and "re- discover" these moons, armed with the knowledge that they are there as well as having assured access to large-aperture southern hemisphere tracking time (on VLT and Magellan).

Haze production in the atmospheres of super-Earths and mini-Neptunes: Insight from PHAZER lab

NASA Astrophysics Data System (ADS)

Horst, Sarah; He, Chao; Kempton, Eliza; Moses, Julianne I.; Vuitton, Veronique; Lewis, Nikole

2017-10-01

Super-Earths and mini-Neptunes (~1.2-3 Earth radii) comprise a large fraction of planets in the universe and TESS (Transiting Exoplanet Survey Satellite) will increase the number that are amenable to atmospheric characterization with observatories like JWST (James Webb Space Telescope). These atmospheres should span a large range of temperature and atmospheric composition phase space, with no solar system analogues. Interpretation of current and future atmospheric observations of super-Earths and mini-Neptunes requires additional knowledge about atmospheric chemistry and photochemical haze production. We have experimentally investigated haze formation for H2, H2O, and CO2 dominated atmospheres (100x, 1000x, and 10000x solar metallicity) for a range of temperatures (300 K, 400 K, and 600 K) using the PHAZER (Planetary Haze Research) experiment at Johns Hopkins University. This is a necessary step in understanding which, if any, super-Earths and mini-Neptunes possess the conditions required for efficient production of photochemical haze in their atmospheres. We find that the production rates vary over a few orders of magnitudes with some higher than our nominal Titan experiments. We therefore expect that planets in this temperature and atmospheric composition phase space will exhibit a range of particle concentrations and some may be as hazy as Titan.

Resonant and Secular Families of the Kuiper Belt

NASA Astrophysics Data System (ADS)

Chiang, E. I.; Lovering, J. R.; Millis, R. L.; Buie, M. W.; Wasserman, L. H.; Meech, K. J.

2003-06-01

We review ongoing efforts to identify occupants of mean-motion resonances (MMRs) and collisional families in the Edgeworth-Kuiper belt. Direct integrations of trajectories of Kuiper belt objects (KBOs) reveal the 1:1 (Trojan), 5:4, 4:3, 3:2 (Plutino), 5:3, 7:4, 9:5, 2:1 (Twotino), and 5:2 MMRs to be inhabited. Apart from the Trojan, resonant KBOs typically have large orbital eccentricities and inclinations. The observed pattern of resonance occupation is consistent with resonant capture and adiabatic excitation by a migratory Neptune; however, the dynamically cold initial conditions prior to resonance sweeping that are typically assumed by migration simulations are probably inadequate. Given the dynamically hot residents of the 5:2 MMR and the substantial inclinations observed in all exterior MMRs, a fraction of the primordial belt was likely dynamically pre-heated prior to resonance sweeping. A pre-heated population may have arisen as Neptune gravitationally scattered objects into trans-Neptunian space. The spatial distribution of Twotinos offers a unique diagnostic of Neptune's migration history. The Neptunian Trojan population may rival the Jovian Trojan population, and the former's existence is argued to rule out violent orbital histories for Neptune. Finally, lowest-order secular theory is applied to several hundred non-resonant KBOs with well-measured orbits to update proposals of collisional families. No convincing family is detected.

On The Detachment of Massive Trans-Neptunian Objects

NASA Astrophysics Data System (ADS)

Fleisig, Jacob; Madigan, Ann-Marie; Zderic, Alexander

2018-06-01

Our Solar System contains a large population of icy bodies stretching well beyond the orbit of Neptune. These objects, known collectively as the Scattered Disk, are remnants from the early formation of the Solar System that were scattered outward from their birth location by Neptune. But not all fit the bill.Sedna, one particularly massive Trans-Neptunian Object (TNO), does not conform to the scattering pattern. Its orbital eccentricity (e) is much lower than expected for a scattered object. This means its perihelion distance (proportional to 1-e) is much larger than the orbit of Neptune, or that it is “detached” from the main Solar System. Many more TNOs share similarities with Sedna. These observations suggest that there is a large population of detached TNOs that have a dynamical history different than that of the objects scattered by Neptune.The physical mechanism by which these massive minor planets become detached is currently unknown. However, we have discovered a phenomenon, driven by differential precession between TNOs of different masses and mutual secular gravitational torques, that naturally detach massive minor planets. This mechanism could have notable consequences for the outer Solar System and may shed some light on the origin of the detached population of minor planets near the Scattered Disk.

The Origin of Pluto's Orbit: Implications for the Solar System Beyond Neptune

NASA Technical Reports Server (NTRS)

Malhotra, Renu

1995-01-01

The origin of the highly eccentric, inclined, and resonance-locked orbit of Pluto has long been a puzzle. A possible explanation has been proposed recently which suggests that these extraordinary orbital properties may be a natural consequence of the formation and early dynamical evolution of the outer solar system. A resonance capture mechanism is possible during the clearing of the residual planetesimal debris and the formation of the Oort Cloud of comets by planetesimal mass loss from the vicinity of the giant planets. If this mechanism were in operation during the early history of the planetary system, the entire region between the orbit of Neptune and approximately 50 AU would have been swept by first-order mean motion resonances. Thus, resonance capture could occur not only for Pluto, but quite generally for other trans-Neptunian small bodies. Some consequences of this evolution for the present-day dynamical structure of the trans-Neptunian region are (1) most of the objects in the region beyond Neptune and up to approximately 50 AU exist in very narrow zones located at orbital resonances with Neptune (particularly the 3:2 and the 2:1 resonances); and (2) these resonant objects would have significantly large eccentricities. The distribution of objects in the Kuiper Belt as predicted by this theory is presented here.

Uranus' and Neptune's Clouds as Revealed by UKIRT/UIST Observations

NASA Astrophysics Data System (ADS)

Irwin, Patrick G. J.; Teanby, N. A.; Davis, G. R.

2009-09-01

In 2006, 2007 and 2008 observations of the near-infrared spectrum of Uranus were made with the UIST instrument of the UK Infrared Telescope, covering the period of Uranus’ Northern Spring Equinox. A significant change in the visible appearance of Uranus occurred during this time with the southern polar zone at 45°S fading, while a corresponding zone at 45°N began to form. In addition the visibility of the equatorial zone increased. The observed spectra were fitted using the NEMESIS optimal estimation retrieval model to determine the variation in the latitudinal and vertical cloud structure during this time. Retrievals were conducted using both the methane absorption coefficients used in our previous analyses and also a newly available revised set of methane coefficients and significant differences were seen, which will be reported. During the Uranus observations in 2007, corresponding observations were also made of Neptune's near-infrared spectrum, albeit with substantially less spatial resolution. The spectra were nevertheless sufficient to retrieve the gross variation in Neptune's latitudinal-vertical cloud structure using both sets of methane absorption coefficients. The retrieved vertical-latitudinal cloud structure on Uranus and Neptune, observed with identical instrument setups, are directly compared and the similarities and differences will be presented and discussed.

The quest for H_3^+ at Neptune: deep burn observations with NASA IRTF iSHELL

NASA Astrophysics Data System (ADS)

Melin, H.; Fletcher, L. N.; Stallard, T. S.; Johnson, R. E.; O'Donoghue, J.; Moore, L.; Donnelly, P. T.

2018-03-01

Emission from the molecular ion H_3^+ is a powerful diagnostic of the upper atmosphere of Jupiter, Saturn, and Uranus, but it remains undetected at Neptune. In search of this emission, we present near-infrared spectral observations of Neptune between 3.93 and 4.00 μm taken with the newly commissioned iSHELL instrument on the NASA Infrared Telescope Facility in Hawaii, obtained 2017 August 17-20. We spent 15.4 h integrating across the disc of the planet, yet were unable to unambiguously identify any H_3^+ line emissions. Assuming a temperature of 550 K, we derive an upper limit on the column integrated density of 1.0^{+1.2}_{-0.8}× 10^{13} m-2, which is an improvement of 30 per cent on the best previous observational constraint. This result means that models are overestimating the density by at least a factor of 5, highlighting the need for renewed modelling efforts. A potential solution is strong vertical mixing of polyatomic neutral species from Neptune's upper stratosphere to the thermosphere, reacting with H_3^+, thus greatly reducing the column integrated H_3^+ densities. This upper limit also provide constraints on future attempts at detecting H_3^+ using the James Webb Space Telescope.

Fine Collimator Grids Using Silicon Metering Structure

NASA Technical Reports Server (NTRS)

Eberhard, Carol

1998-01-01

The project Fine Collimator Grids Using Silicon Metering Structure was managed by Dr. Carol Eberhard of the Electromagnetic Systems & Technology Department (Space & Technology Division) of TRW who also wrote this final report. The KOH chemical etching of the silicon wafers was primarily done by Dr. Simon Prussin of the Electrical Engineering Department of UCLA at the laboratory on campus. Moshe Sergant of the Superconductor Electronics Technology Department (Electronics Systems & Technology Division) of TRW and Dr. Prussin were instrumental in developing the low temperature silicon etching processes. Moshe Sergant and George G. Pinneo of the Microelectronics Production Department (Electronics Systems & Technology Division) of TRW were instrumental in developing the processes for filling the slots etched in the silicon wafers with metal-filled materials. Their work was carried out in the laboratories at the Space Park facility. Moshe Sergant is also responsible for the impressive array of Scanning Electron Microscope images with which the various processes were monitored. Many others also contributed their time and expertise to the project. I wish to thank them all.

Modular Digital Course in Undergraduate Neuroscience Education (MDCUNE): A Website Offering Free Digital Tools for Neuroscience Educators.

PubMed

Grisham, William

2009-01-01

We are providing free digital resources for teaching neuroscience labs at http://mdcune.psych.ucla.edu/. These resources will ultimately include materials for teaching laboratories in electrophysiology of neuronal circuits (SWIMMY), a Neuroinformatics/Bioinformatics module, and two modules for investigating the effects of hormones on early CNS development-one focusing on the development of the song system and one focusing on sex differences in spinal cord motor neurons. All of these modules are inquiry based-students gain from genuine experiences in doing actual studies rather than just simulations. These materials should provide instructors the ability to provide good quality laboratory experiences regardless of resource limitations. Currently, modules on sex differences in the spinal cord and virtual neural circuits (SWIMMY) are available on our website. More will be available in summer 2009 and 2010. SWIMMY was demonstrated at the Faculty for Undergraduate Neuroscience (FUN) Workshop-The Undergraduate Neuroscience Education: Interactions, interdisciplines, and curricular best practices at Macalester College in July 2008.

Parallel collisionless shocks forming in simulations of the LAPD experiment

NASA Astrophysics Data System (ADS)

Weidl, Martin S.; Jenko, Frank; Niemann, Chris; Winske, Dan

2016-10-01

Research on parallel collisionless shocks, most prominently occurring in the Earth's bow shock region, has so far been limited to satellite measurements and simulations. However, the formation of collisionless shocks depends on a wide range of parameters and scales, which can be accessed more easily in a laboratory experiment. Using a kJ-class laser, an ongoing experimental campaign at the Large Plasma Device (LAPD) at UCLA is expected to produce the first laboratory measurements of the formation of a parallel collisionless shock. We present hybrid kinetic/MHD simulations that show how beam instabilities in the background plasma can be driven by ablating carbon ions from a target, causing non-linear density oscillations which develop into a propagating shock front. The free-streaming carbon ions can excite both the resonant right-hand instability and the non-resonant firehose mode. We analyze their respective roles and discuss optimizing their growth rates to speed up the process of shock formation.

Posttest analysis of the 1:6-scale reinforced concrete containment

DOE Office of Scientific and Technical Information (OSTI.GOV)

Pfeiffer, P.A.; Kennedy, J.M.; Marchertas, A.H.

A prediction of the response of the Sandia National Laboratories 1:6- scale reinforced concrete containment model test was made by Argonne National Laboratory. ANL along with nine other organizations performed a detailed nonlinear response analysis of the 1:6-scale model containment subjected to overpressurization in the fall of 1986. The two-dimensional code TEMP-STRESS and the three-dimensional NEPTUNE code were utilized (1) to predict the global response of the structure, (2) to identify global failure sites and the corresponding failure pressures and (3) to identify some local failure sites and pressure levels. A series of axisymmetric models was studied with the two-dimensionalmore » computer program TEMP-STRESS. The comparison of these pretest computations with test data from the containment model has provided a test for the capability of the respective finite element codes to predict global failure modes, and hence serves as a validation of these codes. Only the two-dimensional analyses will be discussed in this paper. 3 refs., 10 figs.« less

Generation of high quality electron beams via ionization injection in a plasma wakefield accelerator

NASA Astrophysics Data System (ADS)

Vafaei-Najafabadi, Navid; Joshi, Chan; E217 SLAC Collaboration

2016-10-01

Ionization injection in a beam driven plasma wakefield accelerator has been used to generate electron beams with over 30 GeV of energy in a 130 cm of lithium plasma. The experiments were performed using the 3 nC, 20.35 GeV electron beam at the FACET facility of the SLAC National Accelerator Laboratory as the driver of the wakefield. The ionization of helium atoms in the up ramp of a lithium plasma were injected into the wake and over the length of acceleration maintained an emittance on the order of 30 mm-mrad, which was an order of magnitude smaller than the drive beam, albeit with an energy spread of 10-20%. The process of ionization injection occurs due to an increase in the electric field of the drive beam as it pinches through its betatron oscillations. Thus, this energy spread is attributed to the injection region encompassing multiple betatron oscillations. In this poster, we will present evidence through OSIRIS simulations of producing an injected beam with percent level energy spread and low emittance by designing the plasma parameters appropriately, such that the ionization injection occurs over a very limited distance of one betatron cycle. Work at UCLA was supported by the NSF Grant Number PHY-1415386 and DOE Grant Number DE-SC0010064. Work at SLAC was supported by DOE contract number DE-AC02-76SF00515. Simulations used the Hoffman cluster at UCLA.

Experimental Evaluation of the New Automated Team Composition System (ATCS) by Formation of Optimal Teams for an Engineering Research Task

DTIC Science & Technology

2010-12-24

Los Angeles Police Department ) 3. LACSD ( Los Angeles County Sheriff’ Department ) 4. USDHS (US Department of Homeland Security) Candidate Roster... The present study used archival data from a UCLA (University of California Los Angeles ) engineering course in which nominally student teams prepare...psychological literature. The present study used archival data from a UCLA (University of California Los Angeles ) engineering course

UCLA-LANL Reanalysis Project

NASA Astrophysics Data System (ADS)

Shprits, Y.; Chen, Y.; Friedel, R.; Kondrashov, D.; Ni, B.; Subbotin, D.; Reeves, G.; Ghil, M.

2009-04-01

We present first results of the UCLA-LANL Reanalysis Project. Radiation belt relativistic electron Phase Space Density is obtained using the data assimilative VERB code combined with observations from GEO, CRRES, and Akebono data. Reanalysis of data shows the pronounced peaks in the phase space density and pronounced dropouts of fluxes during the main phase of a storm. The results of the reanalysis are discussed and compared to the simulations with the recently developed VERB 3D code.

Leon Knopoff (1926-2011)

NASA Astrophysics Data System (ADS)

Davis, Paul; Jackson, David; Gilbert, Freeman

2011-06-01

Leon Knopoff died at his home in Sherman Oaks, Calif., on 20 January 2011 at the age of 85. A man of wide-ranging talents, he had the rare distinction of being simultaneously a professor of physics, a professor of geophysics, and a research musicologist at the University of California, Los Angeles (UCLA). As an undergraduate he studied electrical engineering and obtained his Ph.D. in physics and mathematics at the California Institute of Technology (Caltech) in 1949. He was recruited to the Institute of Geophysics (now the Institute of Geophysics and Planetary Physics) at UCLA in 1950 by Louis Slichter, where he became a professor of geophysics in 1957 and of geophysics and physics in 1961. He became a research musicologist in the UCLA Institute of Ethnomusicology soon after it was formed in 1960. Other appointments included faculty positions at Miami University in Ohio (1948-1950) and Caltech (1962-1963) and visiting appointments at Cambridge, Karlsruhe, Harvard, Santiago, Trieste, and Venice.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Buchanan, Charles D.; Cline, David B.; Byers, N.

Progress in the various components of the UCLA High-Energy Physics Research program is summarized, including some representative figures and lists of resulting presentations and published papers. Principal efforts were directed at the following: (I) UCLA hadronization model, PEP4/9 e{sup +}e{sup {minus}} analysis, {bar P} decay; (II) ICARUS and astroparticle physics (physics goals, technical progress on electronics, data acquisition, and detector performance, long baseline neutrino beam from CERN to the Gran Sasso and ICARUS, future ICARUS program, and WIMP experiment with xenon), B physics with hadron beams and colliders, high-energy collider physics, and the {phi} factory project; (III) theoretical high-energy physics;more » (IV) H dibaryon search, search for K{sub L}{sup 0} {yields} {pi}{sup 0}{gamma}{gamma} and {pi}{sup 0}{nu}{bar {nu}}, and detector design and construction for the FNAL-KTeV project; (V) UCLA participation in the experiment CDF at Fermilab; and (VI) VLPC/scintillating fiber R D.« less

DOE Office of Scientific and Technical Information (OSTI.GOV)

Not Available

Progress in the various components of the UCLA High-Energy Physics Research program is summarized, including some representative figures and lists of resulting presentations and published papers. Principal efforts were directed at the following: (I) UCLA hadronization model, PEP4/9 e{sup +}e{sup {minus}} analysis, {bar P} decay; (II) ICARUS and astroparticle physics (physics goals, technical progress on electronics, data acquisition, and detector performance, long baseline neutrino beam from CERN to the Gran Sasso and ICARUS, future ICARUS program, and WIMP experiment with xenon), B physics with hadron beams and colliders, high-energy collider physics, and the {phi} factory project; (III) theoretical high-energy physics;more » (IV) H dibaryon search, search for K{sub L}{sup 0} {yields} {pi}{sup 0}{gamma}{gamma} and {pi}{sup 0}{nu}{bar {nu}}, and detector design and construction for the FNAL-KTeV project; (V) UCLA participation in the experiment CDF at Fermilab; and (VI) VLPC/scintillating fiber R & D.« less

The LCLS Project

NASA Astrophysics Data System (ADS)

Paterson, James M.

2000-04-01

The Linac Coherent Light Source (LCLS) is a linac driven FEL which uses a 1km electron linac (the last third of the SLAC linac) and a 100m long undulator to produce 1.5 angstrom X-rays of extremely high peak brightness. This radiation is fully tranversely coherent and is in sub-picosecond long pulses. The LCLS Project is a four year R&D program to solidify the design, to develop required technologies, to optimize the cost and performance and to study the potential experimental programs using these unique beam characteristics. The program is conducted by a multi-institutional collaboration consisting of SLAC as the lead laboratory, along with ANL, BNL, LLNL, LANL and UCLA.The LCLS design and the R&D programs are described.

Atmospheric Models for Aerocapture

NASA Technical Reports Server (NTRS)

Justus, C. G.; Duvall, Aleta L.; Keller, Vernon W.

2004-01-01

There are eight destinations in the solar System with sufficient atmosphere for aerocapture to be a viable aeroassist option - Venus, Earth, Mars, Jupiter, Saturn and its moon Titan, Uranus, and Neptune. Engineering-level atmospheric models for four of these targets (Earth, Mars, Titan, and Neptune) have been developed for NASA to support systems analysis studies of potential future aerocapture missions. Development of a similar atmospheric model for Venus has recently commenced. An important capability of all of these models is their ability to simulate quasi-random density perturbations for Monte Carlo analyses in developing guidance, navigation and control algorithm, and for thermal systems design. Similarities and differences among these atmospheric models are presented, with emphasis on the recently developed Neptune model and on planned characteristics of the Venus model. Example applications for aerocapture are also presented and illustrated. Recent updates to the Titan atmospheric model are discussed, in anticipation of applications for trajectory and atmospheric reconstruct of Huygens Probe entry at Titan.

The Voyager Neptune travel guide

NASA Technical Reports Server (NTRS)

Kohlhase, Charles (Editor)

1989-01-01

The Voyager mission to the giant outer planets of our solar system is described. Scientific highlights include interplanetary cruise, Jupiter, Saturn, Uranus, and their vast satellite and ring systems. Detailed plans are provided for the August 1989 Neptune encounter and subsequent interstellar journey to reach the heliopause. As background, the elements of an unmanned space mission are explained, with emphasis on the capabilities of the spacecraft and the scientific sensors. Other topics include the Voyager Grand Tour trajectory design, deep-space navigation, and gravity-assist concepts. The Neptune flyby is animated through the use of computer-generated, flip-page movie frames that appear in the corners of the publication. Useful historical information is also presented, including facts associated with the Voyager mission. Finally, short summaries are provided to describe the major objectives and schedules for several space missions planned for the remainder of the 20th century.

ARC-1989-A89-7050

NASA Image and Video Library

1989-08-27

P-34715 Range: 900,000 kilometers (560,000 miles) This post-encounter view of the south pole of Neptune was obtained after Voyager 2 passed the planet and sped away on a southward-trending trajectory. Voyager's wide-angle camera saw features as small as 120 km (75 mi) in diameter. The angle between the Sun, the center of the planet, and the spacecraft is 137 °, so the entire south polar region is illuminated. Near the bright limb, clouds located at 71 and 42 degrees south latitude rotate eastward onto Neptune's night side. A bright cloud (bottom center) lies within 1.5 ° of Neptune's south pole, which has been determined from the orbits of the planet's rings and satellites. The feature is believed to be created by an organized circulation around the pole that forms a clear 'eye' at the center of the system.

An extrasolar planetary system with three Neptune-mass planets.

PubMed

Lovis, Christophe; Mayor, Michel; Pepe, Francesco; Alibert, Yann; Benz, Willy; Bouchy, François; Correia, Alexandre C M; Laskar, Jacques; Mordasini, Christoph; Queloz, Didier; Santos, Nuno C; Udry, Stéphane; Bertaux, Jean-Loup; Sivan, Jean-Pierre

2006-05-18

Over the past two years, the search for low-mass extrasolar planets has led to the detection of seven so-called 'hot Neptunes' or 'super-Earths' around Sun-like stars. These planets have masses 5-20 times larger than the Earth and are mainly found on close-in orbits with periods of 2-15 days. Here we report a system of three Neptune-mass planets with periods of 8.67, 31.6 and 197 days, orbiting the nearby star HD 69830. This star was already known to show an infrared excess possibly caused by an asteroid belt within 1 au (the Sun-Earth distance). Simulations show that the system is in a dynamically stable configuration. Theoretical calculations favour a mainly rocky composition for both inner planets, while the outer planet probably has a significant gaseous envelope surrounding its rocky/icy core; the outer planet orbits within the habitable zone of this star.

Outer planet entry probe system study. Volume 2: Supporting technical studies

NASA Technical Reports Server (NTRS)

1972-01-01

The environment, science investigations, and general mission analysis considerations are given first. These data are followed by discussions of the studies pertaining to the planets Jupiter, Saturn, Uranus, and Neptune. Except for Neptune, each planet discussion is divided into two parts: (1) parametric activities and (2) probe definition for that planet, or the application of a given probe for that planet. The Neptune discussion is limited to parametrics in the area of science and mission analysis. Each of the probe system definitions consists of system and subsystem details including telecommunications, data handling, power pyrotechnics, attitude control, structures, propulsion, thermal control, and probe to spacecraft integration. The first configuration is discussed in detail and the subsequent configuration discussions are limited to the differences. Finally, the hardware availability to support a probe system and commonality of science, missions, and subsystems for use at the various planets are considered.

A disk of scattered icy objects and the origin of Jupiter-family comets.

PubMed

Duncan, M J; Levison, H F

1997-06-13

Orbital integrations carried out for 4 billion years produced a disk of scattered objects beyond the orbit of Neptune. Objects in this disk can be distinguished from Kuiper belt objects by a greater range of eccentricities and inclinations. This disk was formed in the simulations by encounters with Neptune during the early evolution of the outer solar system. After particles first encountered Neptune, the simulations show that about 1 percent of the particles survive in this disk for the age of the solar system. A disk currently containing as few as approximately 6 x 10(8) objects could supply all of the observed Jupiter-family comets. Two recently discovered objects, 1996 RQ20 and 1996 TL66, have orbital elements similar to those predicted for objects in this disk, suggesting that they are thus far the only members of this disk to be identified.

Using the Sandia Z Machine to Probe Water at Planetary Conditions: Redefining the Properties of Water in the Ice Giants

NASA Astrophysics Data System (ADS)

Knudson, M. D.; Desjarlais, M.; Lemke, R.; Mattsson, T.; French, M.; Nettelmann, N.; Redmer, R.

2012-12-01

Recently, there has been a tremendous increase in the number of identified extrasolar planetary systems. Our understanding of their formation is tied to exoplanet internal structure models, which rely upon equation of state (EOS) models of light elements and compounds such as water at multi-Mbar pressure conditions. For the past decade, a large, interdisciplinary team at Sandia National Laboratories has been refining the Z Machine (20+ MA and 10+ MGauss) into a mature, robust, and precise platform for material dynamics experiments in the multi-Mbar pressure regime. In particular, significant effort has gone into effectively coupling condensed matter theory, magneto-hydrodynamic simulation, and electromagnetic modeling to produce a fully self-consistent simulation capability able to very accurately predict the performance of the Z machine and various experimental load configurations. This capability has been instrumental in the ability to develop experimental platforms to routinely perform magnetic ramp compression experiments to over 4 Mbar, and magnetically accelerate flyer plates to over 40 km/s, creating over 20 Mbar impact pressures. Furthermore, a strong tie has been developed between the condensed matter theory and the experimental program. This coupling has been proven time and again to be extremely fruitful, with the capability of both theory and experiment being challenged and advanced through this close interrelationship. This presentation will provide a short overview of the material dynamics platform and discuss in more detail the use of Z to perform extreme material dynamics studies with unprecedented accuracy on water in support of basic science, planetary astrophysics, and the emerging field of high energy density laboratory physics. It was found that widely used EOSs for water are much too compressible (up to 30 percent) at pressures and temperatures relevant to planetary interiors. Furthermore, it is shown that the behavior of water at these conditions, including its reflectivity and isentropic response, is well-described by an EOS for water based on recent first-principles calculations. These findings advocate that this water model be used as the standard for modeling Neptune, Uranus, and "hot Neptune" exoplanets, and should improve our understanding of these types of planetary systems. Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under Contract No. DE-AC04-94AL85000.

Project NEPTUNE: an innovative, powered, fibre-optic cabled deep ocean observatory spanning the Juan de Fuca plate, NE Pacific

NASA Astrophysics Data System (ADS)

Barnes, C.; Delaney, J.

2003-04-01

NEPTUNE is an innovative facility, a deep-water cabled observatory, that will transform marine science. MARS and VENUS are deep and shallow-water test bed facilities for NEPTUNE located in Monterey Canyon, California and in southern British Columbia, respectively; both were funded in 2002. NEPTUNE will be a network of over 30 subsea observatories covering the 200,000 sq. km Juan de Fuca tectonic plate, Northeast Pacific. It will draw power via two shore stations and receive and exchange data with scientists through 3000 km of submarine fiber-optic cables. Each observatory, and cabled extensions, will host and power many scientific instruments on the surrounding seafloor, in seafloor boreholes and buoyed through the water column. Remotely operated and autonomous vehicles will reside at depth, recharge at observatories, and respond to distant labs. Continuous near-real-time multidisciplinary measurement series will extend over 30 years. Free from the limitations of battery life, ship schedules/ accommodations, bad weather and delayed access to data, scientists will monitor remotely their deep-sea experiments in real time on the Internet, and routinely command instruments to respond to storms, plankton blooms, earthquakes, eruptions, slope slides and other events. Scientists will be able to pose entirely new sets of questions and experiments to understand complex, interacting Earth System processes such as the structure and seismic behavior of the ocean crust; dynamics of hot and cold fluids and gas hydrates in the upper ocean crust and overlying sediments; ocean climate change and its effect on the ocean biota at all depths; and the barely known deep-sea ecosystem dynamics and biodiversity. NEPTUNE is a US/Canada (70/30) partnership to design, test, build and operate the network on behalf of a wide scientific community. The total cost of the project is estimated at about U.S. 250 million from concept to operation. Over U.S. 50 million has already been funded for design, development, and the test beds. NEPTUNE will be among the first of many such cabled ocean observatories. Much is to be gained by being among the scientific and industrial pioneers. The multidisciplinary data archive will be an amazing, expanding resource for scientists and students. The public will share in the research discoveries of one of the last unexplored places on earth through an extensive education/outreach program.

Impact of electronic health records on the patient experience in a hospital setting.

PubMed

Migdal, Christopher W; Namavar, Aram A; Mosley, Virgie N; Afsar-manesh, Nasim

2014-10-01

The impact of electronic health records (EHRs) and their effects on optimizing the patient experience has been debated nationally. Currently, there is a paucity of data in this area, and existing research offers conflicting results. Since 2006, the Assessing Residents' CI-CARE (ARC) program has evaluated the physician-patient interaction of resident physicians at University of California, Los Angeles (UCLA) Health utilizing a 20-item questionnaire administered through facilitator-patient interviews. To evaluate the impact of EHR implementation on the patient experience. Retrospective cohort study. Two academic medical campuses: Ronald Reagan UCLA Medical Center and UCLA Medical Center, Santa Monica. A total of 3417 surveys, spanning December 1, 2012 to May 30, 2013, were assessed. This included patient representation from 9 departments within UCLA Health. Surveys were analyzed to assess physician-patient communication. Statistical comparisons were made using χ analysis. All 16 questions assessing physician-patient communication received better responses in the 3 months following EHR implementation, compared to the 3 months prior to implementation. Of these, 9 questions illustrated statistically significant improvement, whereas the improvement in the remaining 7 questions was not statistically significant. These results suggest that EHRs may improve physician-patient communication. The ARC infrastructure allowed for observation of this trend; however, future research should aim to further validate and understand the etiologies of this improvement. © 2014 Society of Hospital Medicine.

Discovery of the candidate Kuiper belt object 1992 QB1

NASA Astrophysics Data System (ADS)

Jewitt, D.; Luu, J.

1993-04-01

The discovery of a new faint object in the outer solar system, 1992 QB1, moving beyond the orbit of Neptune is reported. It is suggested that the 1992 QB1 may represent the first detection of a member of the Kuiper belt (Edgworth, 1949; Kuiper, 1951), the hypothesized population of objects beyond Neptune and a possible source of the short-period comets, as suggested by Whipple (1964), Fernandez (1980), and Duncan et al. (1988).

ARC-1989-A89-7058

NASA Image and Video Library

1989-08-24

Voyager II Imagery; Neptune. This bulls-eye view of Neptune's small dark spot (D2) was obtained by Voyager 2's narrow-angle camera , when Neptune was within 1.1 million km (680,000 miles) of the planet. The smallest structures that can be seen are 20 km (12 miles) across. This unplanned photograph was obtained when the infrared spectrograph was mapping the the highest-resolution view of the feature taken during the flyby. Banding surrounding the feature indicates unseen strong winds, while structues within the bright spot suggest both active upwelling of clouds and rotation about the center. A rotation rate has not yet been measured, but the v-shaped structure near the right edge of the bright area indicates that the spot rotates clockwise. Unlike the Great Red Spot on Jupiter, which rotates counterclockwise, if the D2 spot on Neptune rotates clockwise, the material will be descending in the dark oval region. The fact that infrared data will yield temperature information about the region above the clouds makes this observation especially valuable. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applicaitons. (JPL ref: P-34749 Voyager N-71) taken during the flyby. Banding surrounding the feature indicates unseen strong winds, while structures within the bright spot suggest both active upwelling of clouds and rotation about the center. A rotation rate has not yest been measured, but the Vv-sphped

The weaker effects of First-order mean motion resonances in intermediate inclinations

NASA Astrophysics Data System (ADS)

Chen, YuanYuan; Quillen, Alice C.; Ma, Yuehua; Chinese Scholar Council, the National Natural Science Foundation of China, the Natural Science Foundation of Jiangsu Province, the Minor Planet Foundation of the Purple Mountain Observatory

2017-10-01

During planetary migration, a planet or planetesimal can be captured into a low-order mean motion resonance with another planet. Using a second-order expansion of the disturbing function in eccentricity and inclination, we explore the sensitivity of the capture probability of first-order mean motion resonances to orbital inclination. We find that second-order inclination contributions affect the resonance strengths, reducing them at intermediate inclinations of around 10-40° for major first-order resonances. We also integrated the Hamilton's equations with arbitrary initial arguments, and provided the varying tendencies of resonance capture probabilities versus orbital inclinations for different resonances and different particle or planetary eccentricities. Resonance-weaker ranges in inclinations generally appear at the places where resonance strengths are low, around 10-40° in general. The weaker ranges disappear with a higher particle eccentricity (≳0.05) or planetary eccentricity (≳0.05). These resonance-weaker ranges in inclinations implies that intermediate-inclination objects are less likely to be disturbed or captured into the first-order resonances, which would make them entering into the chaotic area around Neptune with a larger fraction than those with low inclinations, during the epoch of Neptune's outward migration. The privilege of high-inclination particles leave them to be more likely captured into Neptune Trojans, which might be responsible for the unexpected high fraction of high-inclination Neptune Trojans.

Fostering K-12 Inquiry-based Lesson Development on Regional Water Resource Issues in Los Angeles Urban Schools through the NSF UCLA SEE-LA GK-12 program

NASA Astrophysics Data System (ADS)

Hogue, T. S.; Burke, M. P.; Thulsirag, V.; Daniel, J.; Moldwin, M.; Nonacs, P.

2010-12-01

A National Science Foundation Graduate Teaching Fellows in K- 12 Education program at UCLA (SEE-LA; http://measure.igpp.ucla.edu/GK12-SEE-LA/ ) partners UCLA faculty and graduate students (fellows) with urban middle and high school science teachers and their students to foster programs of science and engineering exploration that bring the environment of Los Angeles into the classroom. UCLA graduate fellows serve as scientists-in-residence at four partner schools to integrate inquiry-based science lessons, facilitate advancements in science content teaching, and ultimately, to improve their own science communication skills. As part of their fellowship, graduate students are required to develop inquiry-based lessons in their partner classroom. During the first two years of the project, the SEE-LA fellows have developed a range of inquiry-based activities, from invertebrate observations in an urban stream system, to water and home energy consumption surveys, to a school biodiversity investigation, to a school-wide alternative energy fair, to engineering the cleanup of environmental disasters, such as the recent oil spill in the Gulf of Mexico. Several of the current fellows have dissertation research in water resource related fields and are specifically integrating lessons specific to their research into their partner classrooms, including urban stream water quality, post-fire watershed behavior, beach water quality assessment and E. coli source tracking. This presentation will provide an overview of goals of the SEE-LA GK-12 program, development of inquiry-based water resource lessons and resulting engagement in the partner classrooms. University and local pre-college school partnerships provide an excellent opportunity to support the development of graduate student communication and teaching skills while also contributing significantly to the integration of science education into K-12 curriculum.

Integrating long-term science projects into K-12 curriculum: Fostering teacher-student engagement in urban environmental research through an NSF UCLA GK-12 program

NASA Astrophysics Data System (ADS)

Hogue, T. S.; Moldwin, M.; Nonacs, P.; Daniel, J.; Shope, R.

2009-12-01

A National Science Foundation Graduate Teaching Fellows in K- 12 Education program at UCLA (SEE-LA; http://measure.igpp.ucla.edu/GK12-SEE-LA) has just completed its first year (of a five-year program) and has greatly expanded UCLA’s science and engineering partnerships with LA Unified and Culver City Unified School Districts. The SEE-LA program partners UCLA faculty, graduate students (fellows), middle and high school science teachers and their students into a program of science and engineering exploration that brings the environment of Los Angeles into the classroom. UCLA graduate fellows serve as scientists-in-residence at the four partner schools to integrate inquiry-based science and engineering lessons, facilitate advancements in science content teaching, and ultimately, to improve their own science communication skills. As part of their fellowship, graduate students are required to develop three inquiry-based lessons in their partner classroom, including a lesson focused on their dissertation research, a lesson focused on the environmental/watershed theme of the project, and a lesson that involves longer-term data collection and synthesis with the grade 6-12 teachers and students. The developed long-term projects ideally involve continued observations and analysis through the five-year project and beyond. During the first year of the project, the ten SEE-LA fellows developed a range of long-term research projects, from seasonal invertebrate observations in an urban stream system, to home energy consumption surveys, to a school bioblitz (quantification of campus animals and insects). Examples of lesson development and integration in the classroom setting will be highlighted as well as tools required for sustainability of the projects. University and local pre-college school partnerships provide an excellent opportunity to support the development of graduate student communication skills while also contributing significantly to the integration of sustainable research projects into K-12 curriculum.

Neptune's New Dark Vortex: Aerosol Properties from Optical Data

NASA Astrophysics Data System (ADS)

Tollefson, J.; Luszcz-Cook, S.; Wong, M. H.; De Pater, I.

2016-12-01

Over the past year, amateur and professional astronomers alike have monitored the appearance of a new dark vortex on Neptune, dubbed SDS-2015 for "southern dark spot discovered in 2015" (Wong et al. 2016; CBET 4278). The discovery of SDS-2015 is fortuitous, being one of only five dark spots observed on Neptune since Voyager 2 imaged the Great Dark Spot (Smith et al. 1989, Science 246, 1422). A companion abstract (Wong et al., this meeting) will present Hubble Space Telescope images of SDS-2015, showcasing the discovery of the vortex in September 2015 and subsequent observations in May 2016. These observations span the optical regime. Longer wavelengths track bright companion clouds thought to form as air is diverted around SDS-2015. Shorter wavelengths reveal the dark spot itself. Combined, these data probe the vertical extent of the dark spot and Neptune's surrounding upper atmosphere. We present preliminary radiative transfer analyses of SDS-2015 using our multispectral data. Our model is the same as that in Luszcz-Cook et al. (2016, Icarus 276, 52) but extended to optical wavelengths. Prior to this work, little was known about the composition and vertical extent of Neptune's dark spots. Only data at optical wavelengths reveal these vortices, suggesting they consist of clearings in the background of fine, evenly-distributed haze particle. Alternatively, the spots may consist of low-albedo aerosols, causing their apparent darkness. Radiative transfer modeling is also one way to determine the vortex top altitude. Simulations of the Great Dark Spot by Stratman et al. (2001, Icarus 151, 275) found that the vortex top altitude is coupled to the brightness of companion clouds, where cloud opacity weakened as the top of the vortex reached higher into the tropopause region. The modeling presented here will compare these hypotheses and provide the first glimpses into the vertical structure of SDS-2015.

Mid-Infrared Ethane Emission on Neptune: 2005-2009

NASA Astrophysics Data System (ADS)

Hammel, Heidi B.; Sitko, M. L.; Russell, R. W.; Lynch, D. K.; Bernstein, L. S.; Perry, R. B.

2009-09-01

Hammel et al. (2006, ApJ 644, 1326) reported 8- to 13-micron spectral observations of Neptune spanning more than a decade. Those data indicated a steady increase in Neptune's 12-micron atmospheric ethane emission from 1985 to 2003, followed by a slight decrease in 2004. The simplest explanation for the intensity variation was an increase in stratospheric effective temperature from 155 K in 1985 to 176 K in 2003 (an average rate of 1.2 K/year), and subsequent decrease to 165 K in 2004 (uncertainties +/- 3 K). Later disk-resolved 12-micron images (Hammel et al. 2007, AJ 134, 637; Orton et al. 2007, AA 473, L5) showed Neptune's ethane emission arose mainly from two regions: emission distributed nearly uniformly around the planet's limb and emission near the south pole. Because much of the non-limb emission was confined to the near-polar region, seasonal variation may play some role in the long-term mid-infrared brightness variations: i.e., more of that region was revealed as Neptune neared solstice in 2005. We will report the results of an additional half decade of mid-infrared spectroscopic observations, from 2005 through 2009, using the Broadband Array Spectrograph System on the NASA Infrared Telescope Facility (IRTF). These post-solstice data should elucidate whether the variations are intrinsic, or due to changes in viewing angle. HBH acknowledges support from NASA grants NNX06AD12G and NNA07CN65A. This work was supported at The Aerospace Corporation by the Independent Research and Development Program. LSB acknowledges the support of Spectral Sciences, Inc. IR and D funding. We also gratefully acknowledge D. Kim (The Aerospace Corporation) for BASS technical support, as well as the support of IRTF staff and telescope operators. We recognize the significant cultural role of Mauna Kea within the indigenous Hawaiian community, and we appreciate the opportunity to conduct observations from this revered site.

The NEPTUNE Canada Seismograph Network

NASA Astrophysics Data System (ADS)

Rogers, G. C.; Meldrum, R.; Baldwin, R.; Rosenberger, A.; Mulder, T.

2009-12-01

NEPTUNE Canada is the world’s first large regional cable-linked, multi-disciplinary scientific seafloor observatory. In the fall of 2007 an 800 kilometer ring of powered fibre optic cable was laid on the seafloor over the northern part of the Juan de Fuca plate and connected to a shore facility near Port Alberni on Vancouver Island. Five nodes were attached to the cable in the early in the summer of 2009 paving the way for junction boxes and scientific instruments installed in the late summer and fall. The NEPTUNE Canada Seismograph Network will consist initially of four broadband and four short period seismic systems. In the summer of 2009, three broadband OBS packages were deployed forming a large triangle with apexes at ODP 1027 in mid plate and two sites on the continental slope, ODP 889 and Barkley Canyon. In summer 2010 an additional broadband package will be installed on the Endeavour segment of the Juan de Fuca Ridge, and four short period instruments will be installed nearby forming a small array, 6 km in maximum dimension, to record earthquake activity in the vicinity of the many multidisciplinary ridge experiments. The broadband systems comprise a broadband seismometer and strong motion accelerometer in a surficially buried spherical titanium case, with a current meter, hydrophone and differential pressure gauge deployed nearby. The short period systems will include 3-component corehole seismometers on long term loan from the Monterey Bay Aquarium Research Institute (MBARI). All systems will have backup capacity for modest cable outages. The NEPTUNE Canada Seismograph Network relies heavily on knowledge gained from the previous seismographs temporarily deployed in the region by MBARI and the University of Washington and will re-occupy the broadband site and three short period sites at the ridge. NEPTUNE Canada seismic data will be archived by, and available from, both the Geological Survey of Canada and IRIS.

Possible occulations by satellites of Uranus and Neptune - 1983-1985

NASA Technical Reports Server (NTRS)

Mink, D. J.; Klemola, A.

1982-01-01

Predictions are presented for 15 possible occulations by the satellites of Uranus and Neptune from 1983 through 1985. Umbriel, the third satellite of Uranus, might occult a 10.4-mag star (Hyd-20 deg 51699) on 25 March 1983 which will be occulted by Uranus 14 hr earlier. Uncertainties in star positions and ephemerides of planets and satellites are quite large in comparison to the size of these bodies, and these predictions are to be taken as possibilities only.

Chairmanship of the Neptune/Pluto Outer Planets Science Working Group

NASA Technical Reports Server (NTRS)

Stern, S. Alan

1992-01-01

The Outer Planets Science Working Group (OPSWG) is the NASA Solar System Exploration Division (SSED) scientific steering committee for the Outer Solar Systems missions. The FY92 activities of OPSWG are summarized. A set of objectives for OPSWG over FY93 are described. OPSWG's activities for subsequent years are outlined. A paper which examines scientific questions motivating renewed exploration of the Neptune/Triton system and which reviews the technical results of the mission studies completed to date is included in the appendix.

An Evaluation of NEPTUNE - A Program for Estimating Life-Cycle Cost of Oily Waste/Waste Oil Collection, Transportation and Treatment Systems.

DTIC Science & Technology

1981-04-01

are listed in Appendix B. There was a significant problem with the formal auditing of the NEPTUNE predictions since a complete manual checking effort...WRSE R. Z. ien BROKLY ! ACcA BSTON SATH CROTON SAT VALJLJO OUZ~A 5.3. NW AD AX A’s AMS AOFT AG! AZ AOSS AD "’s A AS& ASI AT! A’S AVM cc C"~ Cv DC OD963

Retrieving Neptune's aerosol properties from Keck OSIRIS observations. I. Dark regions

NASA Astrophysics Data System (ADS)

Luszcz-Cook, S. H.; de Kleer, K.; de Pater, I.; Adamkovics, M.; Hammel, H. B.

2016-09-01

We present and analyze three-dimensional data cubes of Neptune from the OSIRIS integral-field spectrograph on the 10-m W.M. Keck II telescope, from 26 July 2009. These data have a spatial resolution of 0.035/pixel and spectral resolution of R ∼3800 in the H (1.47-1.80 μm) and K (1.97-2.38 μm) broad bands. We focus our analysis on regions of Neptune's atmosphere that are near-infrared dark - that is, free of discrete bright cloud features. We use a forward model coupled to a Markov chain Monte Carlo algorithm to retrieve properties of Neptune's aerosol structure and methane profile above ∼4 bar in these near-infrared dark regions. We construct a set of high signal-to-noise spectra spanning a range of viewing geometries to constrain the vertical structure of Neptune's aerosols in a cloud-free latitude band from 2-12°N. We find that Neptune's cloud opacity at these wavelengths is dominated by a compact, optically thick cloud layer with a base near 3 bar. Using the pyDISORT algorithm for the radiative transfer and assuming a Henyey-Greenstein phase function, we observe this cloud to be composed of low albedo (single scattering albedo = 0.45-0.01+0.01), forward scattering (asymmetry parameter g = 0.50-0.02+0.02) particles, with an assumed characteristic size of ∼1μm. Above this cloud, we require an aerosol layer of smaller (∼0.1μm) particles forming a vertically extended haze, which reaches from the upper troposphere (0.59-0.03+0.04 bar) into the stratosphere. The particles in this haze are brighter (single scattering albedo = 0.91-0.05+0.06) and more isotropically scattering (asymmetry parameter g = 0.24-0.03+0.02) than those in the deep cloud. When we extend our analysis to 18 cloud-free locations from 20°N to 87°S, we observe that the optical depth in aerosols above 0.5 bar decreases by a factor of 2-3 or more at mid- and high-southern latitudes relative to low latitudes. We also consider Neptune's methane (CH4) profile, and find that our retrievals indicate a strong preference for a low methane relative humidity at pressures where methane is expected to condense. When we include in our fits a parameter for methane depletion below the CH4 condensation pressure, our preferred solution at most locations is for a methane relative humidity below 10% near the tropopause in addition to methane depletion down to 2.0-2.5 bar. We tentatively identify a trend of lower CH4 columns above 2.5 bar at mid- and high-southern latitudes over low latitudes, qualitatively consistent with what is found by Karkoschka and Tomasko (2011), and similar to, but weaker than, the trend observed for Uranus.

UCLA's outreach program of science education in the Los Angeles schools.

PubMed

Palacio-Cayetano, J; Kanowith-Klein, S; Stevens, R

1999-04-01

The UCLA School of Medicine's Interactive Multi-media Exercises (IMMEX) Project began its outreach into pre-college education in the Los Angeles area in 1993. The project provides a model in which software and technology are effectively intertwined with teaching, learning, and assessment (of both students' and teachers' performances) in the classroom. The project has evolved into a special collaboration between the medical school and Los Angeles teachers. UCLA faculty and staff work with science teachers and administrators from elementary, middle, and high schools. The program benefits ethnically and racially diverse groups of students in schools ranging from the inner city to the suburbs. The project's primary goal is to use technology to increase students' achievement and interest in science, including medicine, and thus move more students into the medical school pipeline. Evaluations from outside project evaluators (West Ed) as well as from teachers and IMMEX staff show that the project has already had a significant effect on teachers' professional development, classroom practice, and students' achievement in the Los Angeles area.

Uranus and Neptune: Refugees from the Jupiter-Saturn zone?

NASA Astrophysics Data System (ADS)

Thommes, E. W.; Duncan, M. J.; Levison, H. F.

1999-09-01

Plantesimal accretion models of planet formation have been quite successful at reproducing the terrestrial region of the Solar System. However, in the outer Solar System these models run into problems, and it becomes very difficult to grow bodies to the current mass of the ``ice giants," Uranus and Neptune. Here we present an alternative scenario to in-situ formation of the ice giants. In addition to the Jupiter and Saturn solid cores, several more bodies of mass ~ 10 MEarth or more are likely to have formed in the region between 4 and 10 AU. As Jupiter's core, and perhaps Saturn's, accreted nebular gas, the other nearby bodies must have been scattered outward. Dynamical friction with the trans-Saturnian part of the planetesimal disk would have acted to decouple these ``failed cores" from their scatterer, and to circularize their orbits. Numerical simulations presented here show that systems very similar to our outer Solar System (including Uranus, Neptune, the Kuiper belt, and the scattered disk) are a natural product of this process.

The Neptune/Triton Explorer Mission: A Concept Feasibility Study

NASA Technical Reports Server (NTRS)

Esper, Jaime

2003-01-01

Technological advances over the next 10 to 15 years promise to enable a number of smaller, more capable science missions to the outer planets. With the inception of miniaturized spacecraft for a wide range of applications, both in large clusters around Earth, and for deep space missions, NASA is currently in the process of redefining the way science is being gathered. Technologies such as 3-Dimensional Multi-Chip Modules, Micro-machined Electromechanical Devices, Multi Functional Structures, miniaturized transponders, miniaturized propulsion systems, variable emissivity thermal coatings, and artificial intelligence systems are currently in research and development, and are scheduled to fly (or have flown) in a number of missions. This study will leverage on these and other technologies in the design of a lightweight Neptune orbiter unlike any other that has been proposed to date. The Neptune/Triton Explorer (NExTEP) spacecraft uses solar electric earth gravity assist and aero capture maneuvers to achieve its intended target orbit. Either a Taurus or Delta-class launch vehicle may be used to accomplish the mission.

A Neptune-mass Free-floating Planet Candidate Discovered by Microlensing Surveys

NASA Astrophysics Data System (ADS)

Mróz, Przemek; Ryu, Y.-H.; Skowron, J.; Udalski, A.; Gould, A.; Szymański, M. K.; Soszyński, I.; Poleski, R.; Pietrukowicz, P.; Kozłowski, S.; Pawlak, M.; Ulaczyk, K.; OGLE Collaboration; Albrow, M. D.; Chung, S.-J.; Jung, Y. K.; Han, C.; Hwang, K.-H.; Shin, I.-G.; Yee, J. C.; Zhu, W.; Cha, S.-M.; Kim, D.-J.; Kim, H.-W.; Kim, S.-L.; Lee, C.-U.; Lee, D.-J.; Lee, Y.; Park, B.-G.; Pogge, R. W.; KMTNet Collaboration

2018-03-01

Current microlensing surveys are sensitive to free-floating planets down to Earth-mass objects. All published microlensing events attributed to unbound planets were identified based on their short timescale (below two days), but lacked an angular Einstein radius measurement (and hence lacked a significant constraint on the lens mass). Here, we present the discovery of a Neptune-mass free-floating planet candidate in the ultrashort (t E = 0.320 ± 0.003 days) microlensing event OGLE-2016-BLG-1540. The event exhibited strong finite-source effects, which allowed us to measure its angular Einstein radius of θ E = 9.2 ± 0.5 μas. There remains, however, a degeneracy between the lens mass and distance. The combination of the source proper motion and source-lens relative proper motion measurements favors a Neptune-mass lens located in the Galactic disk. However, we cannot rule out that the lens is a Saturn-mass object belonging to the bulge population. We exclude stellar companions up to ∼15 au.

CCC Observations of Pluto, Neptune and Triton with the San Fernando automatic meridian circle.

NASA Astrophysics Data System (ADS)

Muiños, J. L.; Belizón, F.; Vallejo, M.; Mallamaci, C. C.; Pérez, J. A.; Marmolejo, L. F.; Navarro, J. L.; Sedeño, J. A.

2003-11-01

The San Fernando automatic meridian circle (CMASF) is a meridian telescope built by Grubb-Parsons in 1948 fully automated between 1987 and 1995. In 1996 was moved from the Real Instituto y Observatorio de la Armada (ROA) in San Fernando to the Carlos U. Cesco (CUC) mountain observatory in San Juan (Argentine). The CUC is owned by the Observatorio Astronómico Félix Aguilar (OAFA) of National University of San Juan. In 1999 the telescope was provided with a CCD camera borrowed by the Copenhagen University Observatory (CUO). Between March and October of 2001 a campaign of observations of Pluto, Neptune and its satellite Triton was carried out with the CMASF. They were observed every five days while their transits through the CUC meridian happened during the night. In total 12 transits of Pluto, 15 of Neptune and 16 of Triton were got during that period. In this paper we present the results of the campaign.

Radio science ground data system for the Voyager-Neptune encounter, part 1

NASA Technical Reports Server (NTRS)

Kursinski, E. R.; Asmar, S. W.

1991-01-01

The Voyager radio science experiments at Neptune required the creation of a ground data system array that includes a Deep Space Network complex, the Parkes Radio Observatory, and the Usuda deep space tracking station. The performance requirements were based on experience with the previous Voyager encounters, as well as the scientific goals at Neptune. The requirements were stricter than those of the Uranus encounter because of the need to avoid the phase-stability problems experienced during that encounter and because the spacecraft flyby was faster and closer to the planet than previous encounters. The primary requirement on the instrument was to recover the phase and amplitude of the S- and X-band (2.3 and 8.4 GHz) signals under the dynamic conditions encountered during the occultations. The primary receiver type for the measurements was open loop with high phase-noise and frequency stability performance. The receiver filter bandwidth was predetermined based on the spacecraft's trajectory and frequency uncertainties.

Estimates of the Tropospheric Vertical Structure of Neptune Based on Microwave Radiative Transfer Studies

NASA Technical Reports Server (NTRS)

DeBoer, David R.; Steffes, Paul G.

1996-01-01

A radiative transfer model incorporating, among other things, the recently measured centimeter wavelength opacity of H2S, the full line catalog of PH3, and absorption due to CO has been developed to study the tropospheric vertical structure of Neptune. To match radio-telescope observations, subsolar amounts of NH3 and supersolar amounts of H2S are found to be needed, as has been previously noted. To match both the measured microwave emission and the measured opacity at 13 cm and 6.3 bars by Voyager 2, an H2S dominant atmosphere (H2S/NH3 approximately equals 40) with enhanced PH3 (15 x solar) or NH3 supersaturation with respect to the putative NH4SH cloud (400 ppbv) seems to be indicated. Due to the possible importance of PH3 opacity, it is suggested that measurements of its opacity could aid in resolving some of the outstanding ambiguities concerning Neptune's tropospheric structure.

A Binary System in the Hyades Cluster Hosting a Neptune-Sized Planet

NASA Astrophysics Data System (ADS)

Feinstein, Adina; Ciardi, David; Crossfield, Ian; Schlieder, Joshua; Petigura, Erik; David, Trevor J.; Bristow, Makennah; Patel, Rahul; Arnold, Lauren; Benneke, Björn; Christiansen, Jessie; Dressing, Courtney; Fulton, Benjamin; Howard, Andrew; Isaacson, Howard; Sinukoff, Evan; Thackeray, Beverly

2018-01-01

We report the discovery of a Neptune-size planet (Rp = 3.0Rearth) in the Hyades Cluster. The host star is in a binary system, comprising a K5V star and M7/8V star with a projected separation of 40 AU. The planet orbits the primary star with an orbital period of 17.3 days and a transit duration of 3 hours. The host star is bright (V = 11.2, J = 9.1) and so may be a good target for precise radial velocity measurements. The planet is the first Neptune-sized planet to be found orbiting in a binary system within an open cluster. The Hyades is the nearest star cluster to the Sun, has an age of 625-750 Myr, and forms one of the fundamental rungs in the distance ladder; understanding the planet population in such a well-studied cluster can help us understand and set contraints on the formation and evolution of planetary systems.

An Assessment of Aerocapture and Applications to Future Missions to Uranus and Neptune

NASA Astrophysics Data System (ADS)

Beauchamp, P. M.; Spilker, T. R.

2017-12-01

Our investigation examined the current state of readiness of aerocapture at several destinations of interest, including Uranus and Neptune, to identify what technologies are needed, and to determine if a technology demonstration mission is required, prior to the first use of aerocapture for a science mission. The study team concluded that the current state of readiness is destination dependent, with aerocaptured missions feasible at Venus, Mars, and Titan with current technologies. The use of aerocapture for orbit insertion at the ice giant planets Uranus and Neptune requires at least additional study to assess the expected performance of new guidance, navigation, and control algorithms, and possible development of new hardware, such as a mid-L/D entry vehicle shape or new thermal protection system materials. A variety of near-term activities could contribute to risk reduction for missions proposing use of aerocapture, but a system-level technology demonstration mission is not deemed necessary before the use of aerocapture for a NASA science mission.

Improved Bounds on Nonluminous Matter in Solar Orbit

NASA Technical Reports Server (NTRS)

Anderson, John D.; Lau, Eunice L.; Krisher, Timothy P.; Dicus, Duane A.; Rosenbaum, Doris C.; Teplitz, Vigdor L.

1995-01-01

We improve, using a larger set of observations including Voyager 2 Neptune flyby data, previous bounds on the amount of dark matter (DM) trapped in a spherically symmetric distribution about the Sun. We bound DM by noting that such a distribution would increase the effective mass of the Sun as seen by the outer planets and by finding the uncertainty in that effective mass for Uranus and Neptune in fits to the JPL developmental ephemeris residuals, including optical data and those two planets' Voyager 2 flybys. We extend our previous procedure by fitting more parameters of the developmental ephamerides. In addition, we present here the values for Pioneer 10, Pioneer 11, Voyager 1, and Voyager 2 Jupiter-ranging normal points (and incorporate these data as well). Our principal result is to limit DM in spherically symmetric distributions in orbit about the Sun interior to Neptune's orbit to less than Earth mass and interior to Uranus's orbit to about 1/6 of Earth's mass.

Magnetospheric Science at Uranus and Neptune

NASA Astrophysics Data System (ADS)

Hospodarsky, G. B.; Masters, A.; Soderlund, K. M.; Mandt, K. E.

2017-12-01

The magnetospheres of the Ice Giant planets Uranus and Neptune have only been sampled in-situ by the Voyager 2 spacecraft, which revealed a very complicated and dynamic system. In combination with the much weaker solar wind at these distances, the large diurnal and seasonal variability of the magnetospheres' orientation with respect to the solar wind, results in characteristics that are very different from the magnetospheres of Earth and the Gas Giants, Jupiter and Saturn. Studying these magnetospheres is important for furthering our understanding of fundamental physical and chemical processes in the Solar System, and may help in understanding the magnetic fields of exoplanets as well. A number of studies, proposals, and reports, including the recently completed "Ice Giants Pre-Decadal Survey Mission Study Report" have demonstrated the interest in a new mission to the Ice Giants. We will review the magnetospheric results from Voyager 2, summarize outstanding science questions, and discuss possible goals of a future mission to Uranus and/or Neptune.

Voyager planetary radio astronomy at neptune.

PubMed

Warwick, J W; Evans, D R; Peltzer, G R; Peltzer, R G; Romig, J H; Sawyer, C B; Riddle, A C; Schweitzer, A E; Desch, M D; Kaiser, M L; Farrell, W M; Carr, T D; de Pater, I; Staelin, D H; Gulkis, S; Poynter, R L; Boischot, A; Genova, F; Leblanc, Y; Lecacheux, A; Pedersen, B M; Zarka, P

1989-12-15

Detection of very intense short radio bursts from Neptune was possible as early as 30 days before closest approach and at least 22 days after closest approach. The bursts lay at frequencies in the range 100 to 1300 kilohertz, were narrowband and strongly polarized, and presumably originated in southern polar regions ofthe planet. Episodes of smooth emissions in the frequency range from 20 to 865 kilohertz were detected during an interval of at least 10 days around closest approach. The bursts and the smooth emissions can be described in terms of rotation in a period of 16.11 +/- 0.05 hours. The bursts came at regular intervals throughout the encounter, including episodes both before and after closest approach. The smooth emissions showed a half-cycle phase shift between the five episodes before and after closest approach. This experiment detected the foreshock of Neptune's magnetosphere and the impacts of dust at the times of ring-plane crossings and also near the time of closest approach. Finally, there is no evidence for Neptunian electrostatic discharges.

Non-invasive intravital imaging of cellular differentiation with a bright red-excitable fluorescent protein

PubMed Central

Chu, Jun; Haynes, Russell D; Corbel, Stéphane Y; Li, Pengpeng; González-González, Emilio; Burg, John S; Ataie, Niloufar J; Lam, Amy J; Cranfill, Paula J; Baird, Michelle A; Davidson, Michael W; Ng, Ho-Leung; Garcia, K Christopher; Contag, Christopher H; Shen, Kang; Blau, Helen M; Lin, Michael Z

2014-01-01

A method for non-invasive visualization of genetically labelled cells in animal disease models with micron-level resolution would greatly facilitate development of cell-based therapies. Imaging of fluorescent proteins (FPs) using red excitation light in the “optical window” above 600 nm is one potential method for visualizing implanted cells. However, previous efforts to engineer FPs with peak excitation beyond 600 nm have resulted in undesirable reductions in brightness. Here we report three new red-excitable monomeric FPs obtained by structure-guided mutagenesis of mNeptune, previously the brightest monomeric FP when excited beyond 600 nm. Two of these, mNeptune2 and mNeptune2.5, demonstrate improved maturation and brighter fluorescence, while the third, mCardinal, has a red-shifted excitation spectrum without reduction in brightness. We show that mCardinal can be used to non-invasively and longitudinally visualize the differentiation of myoblasts and stem cells into myocytes in living mice with high anatomical detail. PMID:24633408

Chaos in Kepler's Multiple Planet Systems and K2s Observations of the Atmospheres of Uranus Neptune

NASA Technical Reports Server (NTRS)

Lissauer, Jack J.

2016-01-01

More than one-third of the 4700 planet candidates found by NASA's Kepler spacecraft during its prime mission are associated with target stars that have more than one planet candidate, and such "multis" account for the vast majority of candidates that have been verified as true planets. The large number of multis tells us that flat multiplanet systems like our Solar System are common. Virtually all of the candidate planetary systems are stable, as tested by numerical integrations that assume a physically motivated mass-radius relationship, but some of the systems lie in chaotic regions close to instability. The characteristics of some of the most interesting confirmed Kepler multi-planet systems will be discussed. The Kepler spacecraft's 'second life' in theK2 mission has allowed it to obtain long time-series observations of Solar System targets, including the giant planets Uranus & Neptune. These observations show variability caused by the chaotic weather patterns on Uranus & Neptune.

Surgical and prosthetic considerations to rehabilitate an ocular defect using extraoral implants: a clinical report.

PubMed

de Negreiros, Wagner Araujo; Verde, Marcus Aurelio Rabelo Lima; da Silva, Antonio Materson; Pinto, Lecio Pitombeira

2012-04-01

This clinical report shows the use of extraoral implants to rehabilitate an ocular defect, focusing the surgical and prosthetic procedures. Using local anesthesia and a surgical template obtained from the diagnostic wax ocular pattern, two cylinder dental implants were strategically placed in the lateral aspect of the right infraorbital region. Four months later, an acrylic framework including two spherical magnets was made using plastic UCLA abutments. After casting laboratory steps, a customized silicon prosthetic appliance was fabricated from the diagnostic wax ocular pattern and attached to the Co-Cr framework, observing its profile and seating aspects. The patient was satisfied with the treatment result, due to the retention, esthetics, and adhesive-free method to anchor his ocular prostheses. © 2012 by the American College of Prosthodontists.

Properties of the ion-ion hybrid resonator in fusion plasmas

DOE Office of Scientific and Technical Information (OSTI.GOV)

Morales, George J.

2015-10-06

The project developed theoretical and numerical descriptions of the properties of ion-ion hybrid Alfvén resonators that are expected to arise in the operation of a fusion reactor. The methodology and theoretical concepts were successfully compared to observations made in basic experiments in the LAPD device at UCLA. An assessment was made of the excitation of resonator modes by energetic alpha particles for burning plasma conditions expected in the ITER device. The broader impacts included the generation of basic insight useful to magnetic fusion and space science researchers, defining new avenues for exploration in basic laboratory experiments, establishing broader contacts betweenmore » experimentalists and theoreticians, completion of a Ph.D. dissertation, and promotion of interest in science through community outreach events and classroom instruction.« less

Wind, sand, and Mars - The 1990 tests of the Mars balloon and SNAKE

NASA Astrophysics Data System (ADS)

Anderson, C. M.

1991-02-01

The observations of one member of the international team of Planetary Society members responsible for testing the Mars balloon and SNAKE are presented. The tests were held in the fall of 1990 in Indio, California, and concluded successfully. The test team was made up of scientists and technicians from CNES; observers from the Babakin Center; scientists from the Space Research Institute of the Soviet Academy of Sciences; engineers from the Jet Propulsion Laboratory; students from the University of Arizona, Utah State University, UCLA, and Caltech; and Planetary Society volunteers. The chosen sites of study in this desert area were selected to simulate as neary as possible Mars-like conditions and included smooth ancient lake beds, jagged frozen lava flows and gently rolling sand dunes.

Development of an HIV Postexposure Prophylaxis (PEP) Protocol for Trainees Engaging in Academic Global Health Experiences.

PubMed

Arora, Gitanjli; Hoffman, Risa M

2017-11-01

Global health (GH) education programs have become increasingly common in U.S. medical schools and graduate medical education programs, with growing numbers of medical students, residents, and fellows participating in clinical experiences in settings with high HIV prevalence and limited resources. However, there are no guidelines for provision of HIV postexposure prophylaxis (PEP) to trainees engaging in these academic GH experiences. Faculty of the Global Health Education Programs (GHEP) at the David Geffen School of Medicine at UCLA and GH partner institutions recognized the need for PEP access for trainees engaged in GH experiences. In 2013-2014, key UCLA faculty collaborated in the development of the UCLA GHEP PEP Protocol, which includes provision of PEP medications to trainees prior to departure, an on-call infectious disease/HIV specialist to advise trainees who have exposures, and a system for following up with exposed trainees while on the GH rotation and after their return. Between February 2014 and September 2016, 112 medical students and 110 residents received education on the PEP protocol during their predeparture orientation. The protocol was used for 28 exposures (27 occupational, 1 nonoccupational), with PEP recommended in 3 occupational cases (all needlesticks) and the single nonoccupational case. There were no reported HIV seroconversions. The authors plan to formally evaluate the PEP protocol, conduct a qualitative assessment with trainees and both UCLA and GH partner faculty, and discuss best practices with institutions across the United States and with GH partners.

Validating the 11-Item Revised University of California Los Angeles Scale to Assess Loneliness Among Older Adults: An Evaluation of Factor Structure and Other Measurement Properties.

PubMed

Lee, Joonyup; Cagle, John G

2017-11-01

To examine the measurement properties and factor structure of the short version of the Revised University of California Los Angeles (R-UCLA) loneliness scale from the Health and Retirement Study (HRS). Based on data from 3,706 HRS participants aged 65 + who completed the 2012 wave of the HRS and its Psychosocial Supplement, the measurement properties and factorability of the R-UCLA were examined by conducting an exploratory factor analysis (EFA) and the confirmatory factor analysis (CFA) on randomly split halves. The average score for the 11-item loneliness scale was 16.4 (standard deviation: 4.5). An evaluation of the internal consistency produced a Cronbach's α of 0.87. Results from the EFA showed that two- and three-factor models were appropriate. However, based on the results of the CFA, only a two-factor model was determined to be suitable because there was a very high correlation between two factors identified in the three-factor model, available social connections and sense of belonging. This study provides important data on the properties of the 11-item R-UCLA scale by identifying a two-factor model of loneliness: feeling isolated and available social connections. Our findings suggest the 11-item R-UCLA has good factorability and internal reliability. Copyright © 2017 American Association for Geriatric Psychiatry. Published by Elsevier Inc. All rights reserved.

The International Outer Planets Watch atmospheres node database of giant-planet images

NASA Astrophysics Data System (ADS)

Hueso, R.; Legarreta, J.; Sánchez-Lavega, A.; Rojas, J. F.; Gómez-Forrellad, J. M.

2011-10-01

The Atmospheres Node of the International Outer Planets Watch (IOPW) is aimed to encourage the observations and study of the atmospheres of the Giant Planets. One of its main activities is to provide an interaction between the professional and amateur astronomical communities maintaining an online and fully searchable database of images of the giant planets obtained from amateur astronomers and available to both professional and amateurs [1]. The IOPW database contains about 13,000 image observations of Jupiter and Saturn obtained in the visible range with a few contributions of Uranus and Neptune. We describe the organization and structure of the database as posted in the Internet and in particular the PVOL software (Planetary Virtual Observatory & Laboratory) designed to manage the site and based in concepts from Virtual Observatory projects.

SPITZER SPACE TELESCOPE MID-IR LIGHT CURVES OF NEPTUNE

DOE Office of Scientific and Technical Information (OSTI.GOV)

Stauffer, John; Rebull, Luisa; Carey, Sean J.

2016-11-01

We have used the Spitzer Space Telescope in 2016 February to obtain high cadence, high signal-to-noise, 17 hr duration light curves of Neptune at 3.6 and 4.5 μ m. The light curve duration was chosen to correspond to the rotation period of Neptune. Both light curves are slowly varying with time, with full amplitudes of 1.1 mag at 3.6 μ m and 0.6 mag at 4.5 μ m. We have also extracted sparsely sampled 18 hr light curves of Neptune at W1 (3.4 μ m) and W2 (4.6 μ m) from the Wide-feld Infrared Survey Explorer ( WISE )/ NEOWISEmore » archive at six epochs in 2010–2015. These light curves all show similar shapes and amplitudes compared to the Spitzer light curves but with considerable variation from epoch to epoch. These amplitudes are much larger than those observed with Kepler / K 2 in the visible (amplitude ∼0.02 mag) or at 845 nm with the Hubble Space Telescope ( HST ) in 2015 and at 763 nm in 2016 (amplitude ∼0.2 mag). We interpret the Spitzer and WISE light curves as arising entirely from reflected solar photons, from higher levels in Neptune’s atmosphere than for K 2. Methane gas is the dominant opacity source in Neptune’s atmosphere, and methane absorption bands are present in the HST 763 and 845 nm, WISE W1, and Spitzer 3.6 μ m filters.« less

Formation of diamonds in laser-compressed hydrocarbons at planetary interior conditions

DOE Office of Scientific and Technical Information (OSTI.GOV)

Kraus, D.; Vorberger, J.; Pak, A.

The effects of hydrocarbon reactions and diamond precipitation on the internal structure and evolution of icy giant planets such as Neptune and Uranus have been discussed for more than three decades. Inside these celestial bodies, simple hydrocarbons such as methane, which are highly abundant in the atmospheres, are believed to undergo structural transitions that release hydrogen from deeper layers and may lead to compact stratified cores. Indeed, from the surface towards the core, the isentropes of Uranus and Neptune intersect a temperature–pressure regime in which methane first transforms into a mixture of hydrocarbon polymers, whereas, in deeper layers, a phasemore » separation into diamond and hydrogen may be possible. Here in this paper, we show experimental evidence for this phase separation process obtained by in situ X-ray diffraction from polystyrene (C 8H 8) n samples dynamically compressed to conditions around 150 GPa and 5,000 K; these conditions resemble the environment around 10,000 km below the surfaces of Neptune and Uranus. Our findings demonstrate the necessity of high pressures for initiating carbon–hydrogen separation and imply that diamond precipitation may require pressures about ten times as high as previously indicated by static compression experiments. In conclusion, our results will inform mass–radius relationships of carbon-bearing exoplanets, provide constraints for their internal layer structure and improve evolutionary models of Uranus and Neptune, in which carbon–hydrogen separation could influence the convective heat transport.« less

Formation of diamonds in laser-compressed hydrocarbons at planetary interior conditions

DOE PAGES

Kraus, D.; Vorberger, J.; Pak, A.; ...

2017-08-21

The effects of hydrocarbon reactions and diamond precipitation on the internal structure and evolution of icy giant planets such as Neptune and Uranus have been discussed for more than three decades. Inside these celestial bodies, simple hydrocarbons such as methane, which are highly abundant in the atmospheres, are believed to undergo structural transitions that release hydrogen from deeper layers and may lead to compact stratified cores. Indeed, from the surface towards the core, the isentropes of Uranus and Neptune intersect a temperature–pressure regime in which methane first transforms into a mixture of hydrocarbon polymers, whereas, in deeper layers, a phasemore » separation into diamond and hydrogen may be possible. Here in this paper, we show experimental evidence for this phase separation process obtained by in situ X-ray diffraction from polystyrene (C 8H 8) n samples dynamically compressed to conditions around 150 GPa and 5,000 K; these conditions resemble the environment around 10,000 km below the surfaces of Neptune and Uranus. Our findings demonstrate the necessity of high pressures for initiating carbon–hydrogen separation and imply that diamond precipitation may require pressures about ten times as high as previously indicated by static compression experiments. In conclusion, our results will inform mass–radius relationships of carbon-bearing exoplanets, provide constraints for their internal layer structure and improve evolutionary models of Uranus and Neptune, in which carbon–hydrogen separation could influence the convective heat transport.« less

Dynamical implantation of objects in the Kuiper Belt

DOE Office of Scientific and Technical Information (OSTI.GOV)

Brasil, P. I. O.; Nesvorný, D.; Gomes, R. S., E-mail: pedro_brasil87@hotmail.com, E-mail: davidn@boulder.swri.edu, E-mail: rodney@on.br

Several models have been suggested in the past to describe the dynamical formation of hot Kuiper Belt objects (hereafter Hot Classicals or HCs for short). Here, we discuss a dynamical mechanism that allows orbits to evolve from the primordial planetesimal disk at ≲ 35 AU to reach the orbital region now occupied by HCs. We performed three different sets of numerical simulations to illustrate this mechanism. Two of these simulations were based on modern theories for the early evolution of the solar system (the Nice and jumping-Jupiter models). The third simulation was performed with the purpose of increasing the resolutionmore » at 41-46 AU. The common aspect of these simulations is that Neptune scatters planetesimals from ≲ 35 AU to >40 AU and then undergoes a long phase of slow residual migration. Our results show that to reach an HC orbit, a scattered planetesimal needs to be captured in a mean motion resonance (MMR) with Neptune where the perihelion distance rises due to the Kozai resonance (which occurs in MMRs even for moderate inclinations). Finally, while Neptune is still migrating, the planetesimal is released from the MMR on a stable HC orbit. We show that the orbital distribution of HCs expected from this process provides a reasonable match to observations. The capture efficiency and the mass deposited into the HC region appears to be sensitive to the maximum eccentricity reached by Neptune during the planetary instability phase. Additional work will be needed to resolve this dependency in detail.« less

Effect of core cooling on the radius of sub-Neptune planets

NASA Astrophysics Data System (ADS)

Vazan, A.; Ormel, C. W.; Dominik, C.

2018-02-01

Sub-Neptune planets are very common in our Galaxy and show a large diversity in their mass-radius relation. In sub-Neptunes most of the planet mass is in the rocky part (hereafter, core), which is surrounded by a modest hydrogen-helium envelope. As a result, the total initial heat content of such a planet is dominated by that of the core. Nonetheless, most studies contend that the core cooling only has a minor effect on the radius evolution of the gaseous envelope because the cooling of the core is in sync with the envelope; that is most of the initial heat is released early on timescales of 10-100 Myr. In this Letter we examined the importance of the core cooling rate for the thermal evolution of the envelope. Thus, we relaxed the early core cooling assumption and present a model in which the core is characterized by two parameters: the initial temperature and the cooling time. We find that core cooling can significantly enhance the radius of the planet when it operates on a timescale similar to the observed age, i.e. Gyr. Consequently, the interpretation of the mass-radius observations of sub-Neptunes depends on the assumed core thermal properties and the uncertainty therein. The degeneracy of composition and core thermal properties can be reduced by obtaining better estimates of the planet ages (in addition to their radii and masses) as envisioned by future observations.

Born dry in the photoevaporation desert: Kepler's ultra-short-period planets formed water-poor

NASA Astrophysics Data System (ADS)

Lopez, Eric D.

2017-11-01

Recent surveys have uncovered an exciting new population of ultra-short-period (USP) planets with orbital periods less than a day. These planets typically have radii ≲1.5 R⊕, indicating that they likely have rocky compositions. This stands in contrast to the overall distribution of planets out to ∼100 d, which is dominated by low-density sub-Neptunes above 2 R⊕, which must have gaseous envelopes to explain their size. However, on the USP orbits, planets are bombarded by intense levels of photoionizing radiation and consequently gaseous sub-Neptunes are extremely vulnerable to losing their envelopes to atmospheric photoevaporation. Using models of planet evolution, I show that the rocky USP planets can easily be produced as the evaporated remnants of sub-Neptunes with H/He envelopes and that we can therefore understand the observed dearth of USP sub-Neptunes as a natural consequence of photoevaporation. Critically however, planets on USP orbits could often retain their envelopes if they are formed with very high-metallicity water-dominated envelopes. Such water-rich planets would commonly be ≳2 R⊕ today, which is inconsistent with the observed evaporation desert, indicating that most USP planets likely formed from water-poor material within the snow-line. Finally, I examine the special case of 55 Cancri e and its possible composition in the light of recent observations, and discuss the prospects for further characterizing this population with future observations.

The Dynamics of Objects in the Inner Edgeworth Kuiper Belt

NASA Astrophysics Data System (ADS)

Jones, Daniel C.; Williams, Iwan P.; Melita, Mario D.

2005-12-01

Objects in 3:2 mean motion resonance with Neptune are protected from close encounters with Neptune by the resonance. Bodies in orbits with semi-major axis between 39.5 and about 42 AU are not protected by the resonance; indeed due to overlapping secular resonances, the eccentricities of orbits in this region are driven up so that a close encounter with Neptune becomes inevitable. It is thus expected that such orbits are unstable. The list of known Trans-Neptunian objects shows a deficiency in the number of objects in this gap compared to the 43 50 AU region, but the gap is not empty. We numerically integrate models for the initial population in the gap, and also all known objects over the age of the Solar System to determine what fraction can survive. We find that this fraction is significantly less than the ratio of the population in the gap to that in the main belt, suggesting that some mechanism must exist to introduce new members into the gap. By looking at the evolution of the test body orbits, we also determine the manner in which they are lost. Though all have close encounters with Neptune, in most cases this does not lead to ejection from the Solar System, but rather to a reduced perihelion distance causing close encounters with some or all of the other giant planets before being eventually lost from the system, with Saturn appearing to be the cause of the ejection of most of the objects.

Probing planetary interiors: Shock compression of water to 700 GPa and 3.8 g/cc, and recent high precision Hugoniot measurements of deuterium

NASA Astrophysics Data System (ADS)

Knudson, Marcus

2013-06-01

The past several years have seen tremendous increase in the number of identified extra-solar planetary systems. Our understanding of the formation of these systems is tied to our understanding of the internal structure of these exoplanets, which in turn rely upon equations of state of light elements and compounds such as water and hydrogen. Here we present shock compression data for water with unprecedented accuracy that shows commonly used models for water in planetary modeling significantly overestimate the compressibility at conditions relevant to planetary interiors. Furthermore, we show that its behavior at these conditions, including reflectivity and isentropic response, is well described by a recent first-principles based equation of state. These findings advocate the use of this model as the standard for modeling Neptune, Uranus, and ``hot Neptune'' exoplanets, and should contribute to improved understanding of the interior structure of these planets, and perhaps improved understanding of formation mechanisms of planetary systems. We also present very recent experiments on deuterium that have taken advantage of continued improvements in both experimental configuration and the understanding of the quartz shock standard to obtain Hugoniot data with a significant increase in precision. These data will prove to provide a stringent test for the equation of state of hydrogen and its isotopes. Sandia is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Company, for the US Department of Energy's National Nuclear Security Administration under Contract No. DE-ACO4-94AL85000.

Discovery, Orbit and Orbital Evolution of the Distant Object (463368) 2012 VU85

NASA Astrophysics Data System (ADS)

Wlodarczyk, I.; Černis, K.; Boyle, R. P.

2017-03-01

We present the discovery and time evolution of orbital elements of the distant Centaur-type object (463368) 2012 VU85. From all 2135 distant objects listed in the Minor Planet Center we select all 347 numbered distant object and integrate their equations of motion in the 1 Gyr forward and backward integration. The asteroid (463368) 2012 VU85 lies on the border of the group of 347 distant objects, which have a semimajor axis about 44 a.u., eccentricity 0.1 and inclination between 0° and 30°. We show that after 1 Gyr of forward integration, about half of the objects are expelled from the Solar System, \\ie their median lifetime is about 1 Gyr. We note that the long-lived distant objects are mainly located between the regions where Neptune controls aphelia of asteroids and the asteroids are in the mean motion resonance 2/3 with Neptune. We find eight almost regular approaches of clones of the asteroid (463368) 2012 VU85 to Neptune and several generally shorter in time regular approaches to Uranus. For other outer planets we did not detect any approaches below 5 a.u. for a period of 15 000 yr in forward and backward integrations. In our calculations we find eight episodes, each lasting about 3000 yr when the value of inclination oscillates around its average. These changes look similar to the changes of semimajor axis during the occurrence of orbital mean motion resonance with a planet. We find that half of the clones of the asteroid (463368) 2012 VU85 remain in the Solar System for a forward integration of 44 Myr, and for a backward integration of 34 Myr. This is a significantly shorter escape time as compared to the group of distant objects. Almost all long-lived clones have value of Tisserand parameter with respect to Neptune smaller than 3 during the whole 1 Gyr forward and backward integrations. This implies that there are several clones of the asteroid (463368) 2012 VU85 that cross the orbits of Neptune and Uranus. We find many orbital mean motion resonances lasting up to several Myr in the motion of the asteroid (463368) 2012 VU85. According to our computations the presence of the Kozai resonance protects the asteroid from the close approaches with Uranus and Neptune. The Lyapunov time for the asteroid (463368) 2012 VU85 is equal to 4260 years.

Liquid Water Oceans in Ice Giants

NASA Technical Reports Server (NTRS)

Wiktorowicz, Sloane J.; Ingersoll, Andrew P.

2007-01-01

Aptly named, ice giants such as Uranus and Neptune contain significant amounts of water. While this water cannot be present near the cloud tops, it must be abundant in the deep interior. We investigate the likelihood of a liquid water ocean existing in the hydrogen-rich region between the cloud tops and deep interior. Starting from an assumed temperature at a given upper tropospheric pressure (the photosphere), we follow a moist adiabat downward. The mixing ratio of water to hydrogen in the gas phase is small in the photosphere and increases with depth. The mixing ratio in the condensed phase is near unity in the photosphere and decreases with depth; this gives two possible outcomes. If at some pressure level the mixing ratio of water in the gas phase is equal to that in the deep interior, then that level is the cloud base. The gas below the cloud base has constant mixing ratio. Alternately, if the mixing ratio of water in the condensed phase reaches that in the deep interior, then the surface of a liquid ocean will occur. Below this ocean surface, the mixing ratio of water will be constant. A cloud base occurs when the photospheric temperature is high. For a family of ice giants with different photospheric temperatures, the cooler ice giants will have warmer cloud bases. For an ice giant with a cool enough photospheric temperature, the cloud base will exist at the critical temperature. For still cooler ice giants, ocean surfaces will result. A high mixing ratio of water in the deep interior favors a liquid ocean. We find that Neptune is both too warm (photospheric temperature too high) and too dry (mixing ratio of water in the deep interior too low) for liquid oceans to exist at present. To have a liquid ocean, Neptune s deep interior water to gas ratio would have to be higher than current models allow, and the density at 19 kbar would have to be approx. equal to 0.8 g/cu cm. Such a high density is inconsistent with gravitational data obtained during the Voyager flyby. In our model, Neptune s water cloud base occurs around 660 K and 11 kbar, and the density there is consistent with Voyager gravitational data. As Neptune cools, the probability of a liquid ocean increases. Extrasolar "hot Neptunes," which presumably migrate inward toward their parent stars, cannot harbor liquid water oceans unless they have lost almost all of the hydrogen and helium from their deep interiors.

Interaction of high-energy beams with magnetized plasma: feasibility study for laboratory experiments

NASA Astrophysics Data System (ADS)

Roytershteyn, V.; Delzanno, G. L.; Dorfman, S. E.; Cattell, C. A.; Van Compernolle, B.

2017-12-01

We discuss plans for an experiment that will investigate interaction of energetic electron beam with magnetized plasma. The planned experiment will be conducted on the Large Plasma Device (LAPD) at UCLA and will utilize a variable-energy (0.1-1) MeV electron beam. Such energetic beams have recently attracted renewed attention as a basis for a number of active experiments in space, largely due to possibility of overcoming limitations imposed by spacecraft charging in low-density (e.g. magnetospheric) plasma. In this talk, we will discuss theoretical and computation studies of the plasma modes excited by the beam and beam stability. Energetic beams radiate both whistler and high-frequency R-X mode via Cherenkov resonances, with the relative efficiency of coupling to R-X mode increasing with beam energy. The stability of a finite-size, modulated beam (as produced by the available beam sources) is investigated and relative significance of instabilities and direct radiation is discussed. Special attention will be paid to discussing how laboratory experiments relate to conditions in space.

A simple inertial model for Neptune's zonal circulation

NASA Technical Reports Server (NTRS)

Allison, Michael; Lumetta, James T.

1990-01-01

Voyager imaging observations of zonal cloud-tracked winds on Neptune revealed a strongly subrotational equatorial jet with a speed approaching 500 m/s and generally decreasing retrograde motion toward the poles. The wind data are interpreted with a speculative but revealingly simple model based on steady gradient flow balance and an assumed global homogenization of potential vorticity for shallow layer motion. The prescribed model flow profile relates the equatorial velocity to the mid-latitude shear, in reasonable agreement with the available data, and implies a global horizontal deformation scale L(D) of about 3000 km.

Variability of Neptune's 12.2-micron ethane emission feature

NASA Technical Reports Server (NTRS)

Hammel, H. B.; Young, Leslie A.; Hackwell, J.; Lynch, D. K.; Russell, R.; Orton, Glenn S.

1992-01-01

It is presently shown that the ratio of ethane emission to methane emission in Neptune's 7-14 micron spectrum increased by a factor of 1.47 +/- 0.11 in the period between 1985 and 1991, and that the 12.2-micron ethan feature (rather than that of methane at 7.7 microns) is implicated in the greater part of that change. It is speculated that this variation is due either to a nonuniform increase in stratospheric temperature, or (more likely) to an increase in the ethane concentration by over 15 percent.

Discrete cloud structure on Neptune

NASA Technical Reports Server (NTRS)

Hammel, H. B.

1989-01-01

Recent CCD imaging data for the discrete cloud structure of Neptune shows that while cloud features at CH4-band wavelengths are manifest in the southern hemisphere, they have not been encountered in the northern hemisphere since 1986. A literature search has shown the reflected CH4-band light from the planet to have come from a single discrete feature at least twice in the last 10 years. Disk-integrated photometry derived from the imaging has demonstrated that a bright cloud feature was responsible for the observed 8900 A diurnal variation in 1986 and 1987.

Lessons learned from the NEPTUNE power system, and other deep-sea adventures

NASA Astrophysics Data System (ADS)

Kirkham, Harold

2006-11-01

The development of underwater science systems presents some challenging technical issues. It seems that the best efforts of the engineers and scientists involved are sometimes inadequate, and projects that once seemed straightforward end up being late or over-budget, or cancelled. This paper will review some of the lessons that may be learned from the examples of three science projects in the deep ocean: the Deep Underwater Muon and Neutrino Detector neutrino detector, the H2O observatory, and the power system part of the NEPTUNE regional cabled observatory.

DSN radio science system design and testing for Voyager-Neptune encounter

NASA Technical Reports Server (NTRS)

Ham, N. C.; Rebold, T. A.; Weese, J. F.

1989-01-01

The Deep Space Network (DSN) Radio Science System presently implemented within the Deep Space Network was designed to meet stringent requirements imposed by the demands of the Voyager-Neptune encounter and future missions. One of the initial parameters related to frequency stability is discussed. The requirement, specification, design, and methodology for measuring this parameter are described. A description of special instrumentation that was developed for the test measurements and initial test data resulting from the system tests performed at Canberra, Australia and Usuda, Japan are given.

Methane absorption in the visible spectra of the outer planets and Titan

NASA Technical Reports Server (NTRS)

Owen, T.; Cess, R. D.

1975-01-01

New spectra of Jupiter, Saturn, and Titan show weak methane bands in the region below 6000 A which have been known for many years in the spectra of Uranus and Neptune. Adopting the known abundance of methane on Jupiter, we have used a band model to determine CH4 abundances and broadening pressures for the other objects. The results indicate high values of the CH4 to H2 concentration ratio for Uranus and Neptune; for Titan, a surface pressure in excess of 1 atm is implied.

Ring dynamics

NASA Technical Reports Server (NTRS)

Borderies, Nicole

1989-01-01

Theoretical models of planetary-ring dynamics are discussed in a detailed analytical review and illustrated with graphs and diagrams. The streamline concept is introduced, and the phenomena associated with the transport of angular momentum are described. Particular attention is then given to (1) broad rings like those of Saturn (shepherding, density-wave excitation, gaps, bending-wave excitation, multiringlet structures, inner-edge shepherding, and the possibility of polar rings around Neptune), (2) narrow rings like those of Uranus (shepherding, ring shapes, and a self-gravity model of rigid precession), and (3) ring arcs like those seen in stellar-occultation observations of Neptune.

Clinical islet transplantation experience of the University of California Islet Transplant Consortium.

PubMed

Brunicardi, F C; Atiya, A; Stock, P; Kenmochi, T; Une, S; Benhamou, P Y; Watt, P C; Miyamato, M; Wantanabe, Y; Nomura, Y

1995-12-01

The University of California Islet Transplant Consortium was formed to evaluate the feasibility of performing clinical islet transplantation at different transplant centers by using a single centralized islet isolation laboratory. From July 1992 through February 1995 seven adult islet transplantations were performed, six allografts and one autograft. Once procured, human pancreata were brought to the UCLA-VA Islet Core Laboratory for islet isolation and purification, which were then transported to different centers for transplantation. Patients 1 through 3 received their transplants in Los Angeles, patient 4 received her islet transplant in Torrance, and patients 5 through 7 received their transplants in San Francisco. Although none of these patients achieved insulin independence, four of seven had functioning grafts longer than 6 months as indicated by circulating C-peptide level greater than 0.7 ng/ml. Furthermore, improved glucose control as shown by a decreased insulin requirement was seen in 57% (four of seven patients) of these patients. The ability to isolate islets at a single laboratory and transport them long distances to different centers was shown in patients 4 through 7. Islet transplantation can be performed with improvements in blood glucose control, and islets can be isolated at a centralized location and successfully transported to different centers for transplantation.

Significance of large Neptune-crossing objects for terrestrial catastrophism

NASA Astrophysics Data System (ADS)

Steel, D.

2014-07-01

Over the past few decades a substantial number of objects have been discovered on orbits beyond Neptune (i.e. transneptunian objects, in various sub-classes), crossing Neptune's orbit (here: the Neptune-crossers of interest), and also others crossing the orbits of any or all of the jovian planets (i.e. Centaurs). These range in size from tens of kilometres across to hundreds of kilometres and more. Although formally classified as minor planets/asteroids, plus a few dwarf planets, the physical reality of these objects is that they are giant comets. That is, they seem to be composed largely of ices and if they were to enter the inner solar system then they would demonstrate the commonly-observed behaviour of comets such as outgassing, and the formation of ion and dust tails. Commonly-observed cometary behaviour, however, also includes fragmentation events and sometimes complete disintegration for no apparent cause (such as tidal disruption or thermal stresses). One might therefore wonder what the implications would be for life on Earth and terrestrial catastrophism if and when one of these objects, say 100 to 500 kilometres in size, dropped into a short-period orbit with perihelion distance (q) less than 1 au; or even q ˜ 5 au, given what Jupiter's gravity might do to it. How often might such events occur? One way to address that question would be to conduct numerical integrations of suitable test orbits and identify how often small-q orbits result, but this comes up against the problem of identifying very-infrequent events (with annual probabilities per object perhaps of order 10^{-12}-10^{-10}. For example, Emel'yanenko et al. [1] recently followed test orbits for approximately 5 × 10^{14} particle-years (8,925 objects with 200 clones of each, for 300 Myr) but because these were selected on the basis of initial values of q only below 36 (rather than ˜30) au many were not immediately Neptune-crossers; however, many test particles did eventually migrate into small-q orbits, including falling into the Sun. Instead of the demanding computational requirements of numerical integrations I have instead employed a statistical technique which involves: (i) The probability of some test orbit encountering a perturbing planet (Neptune, here); and (ii) The relative probabilities of new orbital elements (in particular q<1 au or q<5 au) resulting from such encounters. This technique I introduced in a paper presented at ACM III in Uppsala in 1989 [2] but I have not used it much in the quarter-century since then. I have presented elsewhere [3] some initial results from running this technique on a handful of known Neptune-crossing orbits, the results justifying the probabilities of order 10^{-12}-10^{-10} per annum that I mentioned above. Here I extend the range of computations and the variety of test orbits sampled in order to try to build a picture of how often the inner solar system might be subject to an incursion by a gigantic fragmenting comet, with obvious repercussions for all the terrestrial planets but especially for the evolution of life on Earth.

Quality of Care Provided by a Comprehensive Dementia Care Comanagement Program.

PubMed

Jennings, Lee A; Tan, Zaldy; Wenger, Neil S; Cook, Erin A; Han, Weijuan; McCreath, Heather E; Serrano, Katherine S; Roth, Carol P; Reuben, David B

2016-08-01

Multiple studies have shown that quality of care for dementia in primary care is poor, with physician adherence to dementia quality indicators (QIs) ranging from 18% to 42%. In response, the University of California at Los Angeles (UCLA) Health System created the UCLA Alzheimer's and Dementia Care (ADC) Program, a quality improvement program that uses a comanagement model with nurse practitioner dementia care managers (DCM) working with primary care physicians and community-based organizations to provide comprehensive dementia care. The objective was to measure the quality of dementia care that nurse practitioner DCMs provide using the Assessing Care of Vulnerable Elders (ACOVE-3) and Physician Consortium for Performance Improvement QIs. Participants included 797 community-dwelling adults with dementia referred to the UCLA ADC program over a 2-year period. UCLA is an urban academic medical center with primarily fee-for-service reimbursement. The percentage of recommended care received for 17 dementia QIs was measured. The primary outcome was aggregate quality of care for the UCLA ADC cohort, calculated as the total number of recommended care processes received divided by the total number of eligible quality indicators. Secondary outcomes included aggregate quality of care in three domains of dementia care: assessment and screening (7 QIs), treatment (6 QIs), and counseling (4 QIs). QIs were abstracted from DCM notes over a 3-month period from date of initial assessment. Individuals were eligible for 9,895 QIs, of which 92% were passed. Overall pass rates of DCMs were similar (90-96%). All counseling and assessment QIs had pass rates greater than 80%, with most exceeding 90%. Wider variation in adherence was found among QIs addressing treatments for dementia, which patient-specific criteria triggered, ranging from 27% for discontinuation of medications associated with mental status changes to 86% for discussion about acetylcholinesterase inhibitors. Comprehensive dementia care comanagement with a nurse practitioner can result in high quality of care for dementia, especially for assessment, screening, and counseling. The effect on treatment QIs is more variable but higher than previous reports of physician-provided dementia care. © 2016, Copyright the Authors Journal compilation © 2016, The American Geriatrics Society.

The UCLA Alzheimer’s and Dementia Care Program for Comprehensive, Coordinated, Patient-centered Care: Preliminary Data

PubMed Central

Reuben, David B.; Evertson, Leslie Chang; Wenger, Neil S.; Serrano, Katherine; Chodosh, Joshua; Ercoli, Linda; Tan, Zaldy S.

2013-01-01

Dementia is a chronic disease that requires both medical and social services to provide high quality of care and prevent complications. As a result of time constraints in practice, lack of systems-based approaches, and poor integration of community-based organizations (CBOs), the quality of care for dementia is poor compared to other diseases that affect older persons. The UCLA Alzheimer’s and Dementia Care (UCLA ADC) program partners with CBOs to provide comprehensive, coordinated, patient-centered care for patients with Alzheimer’s disease and other dementias. The goals of the program are to maximize patient function, independence and dignity, minimize caregiver strain and burnout and reduce unnecessary costs. The UCLA ADC program consists of five key components: patient recruitment and a dementia registry, structured needs assessments of patients in the registry and their caregivers, creation and implementation of individualized dementia care plans based on needs assessments and input from the primary care physicians, monitoring and revising care plans, as needed, and access 24/7, 365 days a year for assistance and advice. The program uses a co-management model with a nurse practitioner Dementia Care Manager working with primary care physicians and CBOs. Based on the first 150 patients served, the most common recommendations in the initial care plans were referrals to support groups (73%), Alzheimer’s Association Safe Return (73%), caregiver training (45%), and medication adjustment (41%). The program will be evaluated on its ability to achieve the triple aim of better care for individuals, better health for populations, and lower costs. PMID:24329821

A comparative study of gold UCLA-type and CAD/CAM titanium implant abutments

PubMed Central

Park, Ji-Man; Lee, Jai-Bong; Heo, Seong-Joo

2014-01-01

PURPOSE The aim of this study was to evaluate the interface accuracy of computer-assisted designed and manufactured (CAD/CAM) titanium abutments and implant fixture compared to gold-cast UCLA abutments. MATERIALS AND METHODS An external connection implant system (Mark III, n=10) and an internal connection implant system (Replace Select, n=10) were used, 5 of each group were connected to milled titanium abutment and the rest were connected to the gold-cast UCLA abutments. The implant fixture and abutment were tightened to torque of 35 Ncm using a digital torque gauge, and initial detorque values were measured 10 minutes after tightening. To mimic the mastication, a cyclic loading was applied at 14 Hz for one million cycles, with the stress amplitude range being within 0 N to 100 N. After the cyclic loading, detorque values were measured again. The fixture-abutment gaps were measured under a microscope and recorded with an accuracy of ±0.1 µm at 50 points. RESULTS Initial detorque values of milled abutment were significantly higher than those of cast abutment (P<.05). Detorque values after one million dynamic cyclic loadings were not significantly different (P>.05). After cyclic loading, detorque values of cast abutment increased, but those of milled abutment decreased (P<.05). There was no significant difference of gap dimension between the milled abutment group and the cast abutment group after cyclic loading. CONCLUSION In conclusion, CAD/CAM milled titanium abutment can be fabricated with sufficient accuracy to permit screw joint stability between abutment and fixture comparable to that of the traditional gold cast UCLA abutment. PMID:24605206

Predictors of participation in sports after hip and knee arthroplasty.

PubMed

Williams, Daniel H; Greidanus, Nelson V; Masri, Bassam A; Duncan, Clive P; Garbuz, Donald S

2012-02-01

While the primary objective of joint arthroplasty is to improve patient quality of life, pain, and function, younger active patients often demand a return to higher function that includes sporting activity. Knowledge of rates and predictors of return to sports will help inform expectations in patients anticipating return to sports after joint arthroplasty. We measured the rate of sports participation at 1 year using the UCLA activity score and explored 11 variables, including choice of procedure/prosthesis, that might predict return to a high level of sporting activity, when controlling for potential confounding variables. We retrospectively evaluated 736 patients who underwent primary metal-on-polyethylene THA, metal-on-metal THA, hip resurfacing arthroplasty, revision THA, primary TKA, unicompartmental knee arthroplasty, and revision TKA between May 2005 and June 2007. We obtained UCLA activity scores on all patients; we defined high activity as a UCLA score of 7 or more. We evaluated patient demographics (age, sex, BMI, comorbidity), quality of life (WOMAC score, Oxford Hip Score, SF-12 score), and surgeon- and procedural/implant-specific variables to identify factors associated with postoperative activity score. Minimum followup was 11 months (mean, 12.1 months; range, 11-13 months). Preoperative UCLA activity score, age, male sex, and BMI predicted high activity scores. The type of operation and implant characteristics did not predict return to high activity sports. Our data suggest patient-specific factors predict postoperative activity rather than factors specific to type of surgery, implant, or surgeon factors. Level II, prognostic study. See the Guidelines for Authors for a complete description of levels of evidence.

An overabundance of low-density Neptune-like planets

NASA Astrophysics Data System (ADS)

Cubillos, Patricio; Erkaev, Nikolai V.; Juvan, Ines; Fossati, Luca; Johnstone, Colin P.; Lammer, Helmut; Lendl, Monika; Odert, Petra; Kislyakova, Kristina G.

2017-04-01

We present a uniform analysis of the atmospheric escape rate of Neptune-like planets with estimated radius and mass (restricted to Mp < 30 M⊕). For each planet, we compute the restricted Jeans escape parameter, Λ, for a hydrogen atom evaluated at the planetary mass, radius, and equilibrium temperature. Values of Λ ≲ 20 suggest extremely high mass-loss rates. We identify 27 planets (out of 167) that are simultaneously consistent with hydrogen-dominated atmospheres and are expected to exhibit extreme mass-loss rates. We further estimate the mass-loss rates (Lhy) of these planets with tailored atmospheric hydrodynamic models. We compare Lhy to the energy-limited (maximum-possible high-energy driven) mass-loss rates. We confirm that 25 planets (15 per cent of the sample) exhibit extremely high mass-loss rates (Lhy > 0.1 M⌖ Gyr-1), well in excess of the energy-limited mass-loss rates. This constitutes a contradiction, since the hydrogen envelopes cannot be retained given the high mass-loss rates. We hypothesize that these planets are not truly under such high mass-loss rates. Instead, either hydrodynamic models overestimate the mass-loss rates, transit-timing-variation measurements underestimate the planetary masses, optical transit observations overestimate the planetary radii (due to high-altitude clouds), or Neptunes have consistently higher albedos than Jupiter planets. We conclude that at least one of these established estimations/techniques is consistently producing biased values for Neptune planets. Such an important fraction of exoplanets with misinterpreted parameters can significantly bias our view of populations studies, like the observed mass-radius distribution of exoplanets for example.

Neptune - Changes in Great Dark Spot

NASA Technical Reports Server (NTRS)

1989-01-01

These images show changes in the clouds around Neptune's Great Dark Spot (GDS) over a four and one-half-day period. From top to bottom the images show successive rotations of the planet an interval of about 18 hours. The GDS is at a mean latitude of 20 degrees south, and covers about 30 degrees of longitude. The violet filter of the Voyager narrow angle camera was used to produce these images at distances ranging from 17 million kilometers (10.5 million miles) at the top, to 10 million kilometers (6.2 million miles) at bottom. The images have been mapped on to a rectangular latitude longitude grid to remove the effects of changing viewing geometry and the changing distance to Neptune. The sequence shows a large change in the western end (left side) of the GDS, where a dark extension apparent in the earlier images converges into an extended string of small dark spots over the next five rotations. This 'string of beads' extends from the GDS at a surprisingly large angle relative to horizontal lines of constant latitude. The large bright cloud at the southern (bottom) border of the GDS is a more or less permanent companion of the GDS. The apparent motion of smaller clouds at the periphery of the GDS suggests a counterclockwise rotation of the GDS reminiscent of flow around the Great Red Spot in Jupiter's atmosphere. This activity of the GDS is surprising because the total energy flux from the sun and from Neptune's interior is only 5 percent as large as the total energy flux on Jupiter.

A New Dark Vortex

NASA Astrophysics Data System (ADS)

Wong, Michael

2015-10-01

A bright, unusually long-lived outburst of cloud activity on Neptune was observed in 2015. This led to speculation about whether the clouds were convective in nature, or bright companions to an unseen dark vortex (similar to the Great Dark Spot studied in detail by Voyager 2). HST OPAL images at blue wavelengths finally answered this question by discovering a new dark vortex at 45 deg S. We call this feature SDS-2015, for southern dark spot discovered in 2015.Dark vortices on Neptune are rare; SDS-2015 is only the fifth ever seen. All five were diverse in terms of size and shape, the distribution of bright companion clouds, and horizontal motions (oscillations and drifts). The drift of these vortices is highly sensitive to horizontal and vertical wind shear, making them valuable probes into the structure of Neptune's atmospheric jets. We have traced oscillations in the longitudinal positions of bright companion clouds of SDS-2015, but a second epoch of HST imaging is needed to measure latitudinal motion of the dark vortex itself.Only HST can image dark vortices on Neptune. Ground-based facilities lack the resolution to detect these low-contrast features at blue optical wavelengths, while infrared observations don't detect the dark spots themselves, only their bright companion features. We propose observations of SDS-2015, in order to measure its size, drift rate, and aerosol structure, and to trace its temporal evolution. The observations will improve our understanding of the life cycle of neptunian vortices, of their influence on the surrounding atmosphere, and of the structure of planetary jets.

Investigation of atmospheric waves on Neptune

NASA Technical Reports Server (NTRS)

Eshleman, Von R.; Hinson, David P.

1994-01-01

This document constitutes the final report for grant NAGW-2442 of the Neptune Data Analysis Program, which supported research concerning atmospheric dynamics on Neptune. Professor Von R. Eshleman was the principal investigator. David P. Hinson was a Co-Investigator. The grant covered the period 1 March 1991 through 31 August 1994, including a six month no-cost extension. Funding from this grant resulted in publication of one journal article and one book chapter as well as presentation of results at two conferences and in numerous seminars. A complete bibliography is given below. A copy of the journal article is attached along with abstracts from the book chapter and the conference presentations. With support from this grant we extended our analysis and interpretation of the Voyager Project. This research contributed to an improvement in our basic understanding of atmospheric dynamics on Neptune. The highlight was the discovery and characterization of inertio-gravity waves in the troposphere and stratosphere. Results include measures of basic wave properties, such as amplitudes and vertical wavelengths, as well as estimates of the effect of the waves on the photochemistry and momentum balance of the stratosphere. This investigation also yielded a better understanding of the potential of radio occultation experiments for studies of atmospheric waves. At the same time we developed new methods of data analysis for exploiting these capabilities. These are currently being applied to radio occultation data obtained with the Magellan spacecraft to study waves in the atmosphere of Venus. Future planetary missions, such as Mars Global Surveyor and Cassini, will benefit from these accomplishments.

Leveraging lean principles in creating a comprehensive quality program: The UCLA health readmission reduction initiative.

PubMed

Afsar-Manesh, Nasim; Lonowski, Sarah; Namavar, Aram A

2017-12-01

UCLA Health embarked to transform care by integrating lean methodology in a key clinical project, Readmission Reduction Initiative (RRI). The first step focused on assembling a leadership team to articulate system-wide priorities for quality improvement. The lean principle of creating a culture of change and accountability was established by: 1) engaging stakeholders, 2) managing the process with performance accountability, and, 3) delivering patient-centered care. The RRI utilized three major lean principles: 1) A3, 2) root cause analyses, 3) value stream mapping. Baseline readmission rate at UCLA from 9/2010-12/2011 illustrated a mean of 12.1%. After the start of the RRI program, for the period of 1/2012-6/2013, the readmission rate decreased to 11.3% (p<0.05). To impact readmissions, solutions must evolve from smaller service- and location-based interventions into strategies with broader approach. As elucidated, a systematic clinical approach grounded in lean methodologies is a viable solution to this complex problem. Copyright © 2017 Elsevier Inc. All rights reserved.

Atmospheric Models for Aerocapture

NASA Technical Reports Server (NTRS)

Justus, C. G.; Duval, Aleta; Keller, Vernon W.

2003-01-01

There are eight destinations in the Solar System with sufficient atmosphere for aerocapture to be a viable aeroassist option - Venus, Earth, Mars, Jupiter, Saturn and its moon Titan, Uranus, and Neptune. Engineering-level atmospheric models for four of these targets (Earth, Mars, Titan, and Neptune) have been developed for NASA to support systems analysis studies of potential future aerocapture missions. Development of a similar atmospheric model for Venus has recently commenced. An important capability of all of these models is their ability to simulate quasi-random density perturbations for Monte Carlo analyses in developing guidance, navigation and control algorithms, and for thermal systems design. Similarities and differences among these atmospheric models are presented, with emphasis on the recently developed Neptune model and on planned characteristics of the Venus model. Example applications for aerocapture are also presented and illustrated. Recent updates to the Titan atmospheric model, in anticipation of applications for trajectory and atmospheric reconstruct of Huygens Robe entry at Titan, are discussed. Recent updates to the Mars atmospheric model, in support of ongoing Mars aerocapture systems analysis studies, are also presented.

Possible formation pathways for the low-density Neptune-mass planet HAT-P-26b

NASA Astrophysics Data System (ADS)

Ali-Dib, Mohamad; Lakhlani, Gunjan

2018-01-01

We investigate possible pathways for the formation of the low-density Neptune-mass planet HAT-P-26b. We use two different formation models based on pebble and planetesimal accretion, and includes gas accretion, disc migration and simple photoevaporation. The models track the atmospheric oxygen abundance, in addition to the orbital period, and mass of the forming planets, which we compare to HAT-P-26b. We find that pebble accretion can explain this planet more naturally than planetesimal accretion that fails completely unless we artificially enhance the disc metallicity significantly. Pebble accretion models can reproduce HAT-P-26b with either a high initial core mass and low amount of envelope enrichment through core erosion or pebbles dissolution, or the opposite, with both scenarios being possible. Assuming a low envelope enrichment factor as expected from convection theory and comparable to the values we can infer from the D/H measurements in Uranus and Neptune, our most probable formation pathway for HAT-P-26b is through pebble accretion starting around 10 au early in the disc's lifetime.

A search for stellar occultations by Uranus, Neptune, Pluto, and their satellites: 1990-1999

NASA Technical Reports Server (NTRS)

Mink, Douglas J.

1991-01-01

A search for occultations of stars by Uranus, Neptune, and Pluto between 1990 and 1999 was carried out by combining ephemeris information and star positions using very accurate occultation modeling software. Stars from both the Space Telescope Guide Catalog and photographic plates taken by Arnold Klemola at Lick Observatory were compared with planet positions from the JPL DE-130 ephemeris, with local modifications for Pluto and Charon. Some 666 possible occultations by the Uranian ring, 143 possible occultations by Neptune, and 40 possible occultations by Pluto and/or Charon were found among stars with visual magnitudes as faint as 16. Before the star positions could be obtained, the occultation prediction software was used to aid many observers in observing the occultation of 28 Sagitarii by Saturn in July 1989. As a test on other outer solar system objects, 17 possible occultations were found in a search of the Guide Star Catalog for occultations by 2060 Chiron, and interesting object between Saturn and Uranus which shows both cometary and asteroidal properties.

Energetic particle signatures of satellites and rings in Neptune's magnetosphere

NASA Technical Reports Server (NTRS)

Selesnick, R. S.; Stone, E. C.

1992-01-01

The cosmic ray system on Voyager 2 found a trapped radiation environment in Neptune's inner magnetosphere which is controlled primarily by absorption at the rings and satellite surfaces. The intensity of electrons with kinetic energies approximately greater than 1 MeV shows particularly strong and narrow signatures associated with absorption by the satellite 1989N1 at an orbital radius of 4.75 Neptune radii. Closer to the planet are several signatures of the inner satellites and rings. Absorption limits the intensity of the inner radiation belt sufficiently for the maximum intensity to occur outside the orbit of 1989N1 at a magnetic L shell of about 7. Radial profiles of the electron phase space density show that electrons diffuse inward from a source in the outer magnetosphere. Many of the inward-diffusing electrons are absorbed upon reaching a satellite orbital radius, but the finite absorption efficiency allows some of the electrons to pass by unaffected. The locations of the satellite and ring signatures also provide constraints on the nondipolar components of the planetary magnetic field.

Neptune False Color Image of Haze

NASA Technical Reports Server (NTRS)

1989-01-01

This false color photograph of Neptune was made from Voyager 2 images taken through three filters: blue, green, and a filter that passes light at a wavelength that is absorbed by methane gas. Thus, regions that appear white or bright red are those that reflect sunlight before it passes through a large quantity of methane. The image reveals the presence of a ubiquitous haze that covers Neptune in a semitransparent layer. Near the center of the disk, sunlight passes through the haze and deeper into the atmosphere, where some wavelengths are absorbed by methane gas, causing the center of the image to appear less red. Near the edge of the planet, the haze scatters sunlight at higher altitude, above most of the methane, causing the bright red edge around the planet. By measuring haze brightness at several wavelengths, scientists are able to estimate the thickness of the haze and its ability to scatter sunlight. The image is among the last full disk photos that Voyager 2 took before beginning its endless journey into interstellar space. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

Captivating Broad Audiences with an Internet-connected Ocean

NASA Astrophysics Data System (ADS)

Moran, K.; Elliott, L.; Gervais, F.; Juniper, K.; Owens, D.; Pirenne, B.

2012-12-01

NEPTUNE Canada, a network of Ocean Networks Canada and the first deep water cabled ocean observatory, began operations in December 2009. Located offshore Canada's west coast, the network streams data from passive, active, and interactive sensors positioned at five nodes along its 800 km long looped cable to the Internet. This technically advanced system includes a sophisticated data management and archiving system, which enables the collection of real-time physical, chemical, geological, and biological oceanographic data, including video, at resolutions relevant for furthering our understanding of the dynamics of the earth-ocean system. Scientists in Canada and around the world comprise the primary audience for these data, but NEPTUNE Canada is also serving these data to broader audiences including K-16 students and teachers, informal educators, citizen scientists, the press, and the public. Here we present our engagement tools, approaches, and experiences including electronic books, personal phone apps, Internet-served video, social media, mini-observatory systems, print media, live broadcasting from sea, and a citizen scientist portal.NEPTUNE Canada's ibook available on Apple's iBook store.

A search for stellar occultations by Uranus, Neptune, Pluto, and their satellites: 1990-1999

NASA Astrophysics Data System (ADS)

Mink, Douglas J.

1991-03-01

A search for occultations of stars by Uranus, Neptune, and Pluto between 1990 and 1999 was carried out by combining ephemeris information and star positions using very accurate occultation modeling software. Stars from both the Space Telescope Guide Catalog and photographic plates taken by Arnold Klemola at Lick Observatory were compared with planet positions from the JPL DE-130 ephemeris, with local modifications for Pluto and Charon. Some 666 possible occultations by the Uranian ring, 143 possible occultations by Neptune, and 40 possible occultations by Pluto and/or Charon were found among stars with visual magnitudes as faint as 16. Before the star positions could be obtained, the occultation prediction software was used to aid many observers in observing the occultation of 28 Sagitarii by Saturn in July 1989. As a test on other outer solar system objects, 17 possible occultations were found in a search of the Guide Star Catalog for occultations by 2060 Chiron, and interesting object between Saturn and Uranus which shows both cometary and asteroidal properties.

Corrigendum.

PubMed

2018-01-01

Arenillas JF, Cortijo E, García-Bermejo P, et al. Relative cerebral blood volume is associated with collateral status and infarct growth in stroke patients in SWIFT PRIME. J Cereb Blood Flow Metab. Epub ahead of print 1 January 2017. DOI: 10.1177/0271678X17740293 . This article was published online with the sixth author, David Liebeskind (Neurovascular Imaging Research Core, Department of Neurology, UCLA, USA), omitted. The full list and order of authors on the article is as follows: Juan F Arenillas, Elisa Cortijo, Pablo García-Bermejo, Elad I Levy, Reza Jahan, David Liebeskind, Mayank Goyal, Jeffrey L Saver and Gregory W Albers Juan F Arenillas's affiliation should have read Neurovascular Research i3 Laboratory, Instituto de Biología y Genética Molecular, Consejo Superior de Investigaciones Científicas (CSIC), Universidad de Valladolid, Valladolid, Spain.

Simulation of Shear Alfvén Waves in LAPD using the BOUT++ code

NASA Astrophysics Data System (ADS)

Wei, Di; Friedman, B.; Carter, T. A.; Umansky, M. V.

2011-10-01

The linear and nonlinear physics of shear Alfvén waves is investigated using the 3D Braginskii fluid code BOUT++. The code has been verified against analytical calculations for the dispersion of kinetic and inertial Alfvén waves. Various mechanisms for forcing Alfvén waves in the code are explored, including introducing localized current sources similar to physical antennas used in experiments. Using this foundation, the code is used to model nonlinear interactions among shear Alfvén waves in a cylindrical magnetized plasma, such as that found in the Large Plasma Device (LAPD) at UCLA. In the future this investigation will allow for examination of the nonlinear interactions between shear Alfvén waves in both laboratory and space plasmas in order to compare to predictions of MHD turbulence.

SHARP: Automated monitoring of spacecraft health and status

NASA Technical Reports Server (NTRS)

Atkinson, David J.; James, Mark L.; Martin, R. Gaius

1991-01-01

Briefly discussed here are the spacecraft and ground systems monitoring process at the Jet Propulsion Laboratory (JPL). Some of the difficulties associated with the existing technology used in mission operations are highlighted. A new automated system based on artificial intelligence technology is described which seeks to overcome many of these limitations. The system, called the Spacecraft Health Automated Reasoning Prototype (SHARP), is designed to automate health and status analysis for multi-mission spacecraft and ground data systems operations. The system has proved to be effective for detecting and analyzing potential spacecraft and ground systems problems by performing real-time analysis of spacecraft and ground data systems engineering telemetry. Telecommunications link analysis of the Voyager 2 spacecraft was the initial focus for evaluation of the system in real-time operations during the Voyager spacecraft encounter with Neptune in August 1989.

SHARP - Automated monitoring of spacecraft health and status

NASA Technical Reports Server (NTRS)

Atkinson, David J.; James, Mark L.; Martin, R. G.

1990-01-01

Briefly discussed here are the spacecraft and ground systems monitoring process at the Jet Propulsion Laboratory (JPL). Some of the difficulties associated with the existing technology used in mission operations are highlighted. A new automated system based on artificial intelligence technology is described which seeks to overcome many of these limitations. The system, called the Spacecraft Health Automated Reasoning Prototype (SHARP), is designed to automate health and status analysis for multi-mission spacecraft and ground data systems operations. The system has proved to be effective for detecting and analyzing potential spacecraft and ground systems problems by performing real-time analysis of spacecraft and ground data systems engineering telemetry. Telecommunications link analysis of the Voyager 2 spacecraft was the initial focus for evaluation of the system in real-time operations during the Voyager spacecraft encounter with Neptune in August 1989.

Computational design of the basic dynamical processes of the UCLA general circulation model

NASA Technical Reports Server (NTRS)

Arakawa, A.; Lamb, V. R.

1977-01-01

The 12-layer UCLA general circulation model encompassing troposphere and stratosphere (and superjacent 'sponge layer') is described. Prognostic variables are: surface pressure, horizontal velocity, temperature, water vapor and ozone in each layer, planetary boundary layer (PBL) depth, temperature, moisture and momentum discontinuities at PBL top, ground temperature and water storage, and mass of snow on ground. Selection of space finite-difference schemes for homogeneous incompressible flow, with/without a free surface, nonlinear two-dimensional nondivergent flow, enstrophy conserving schemes, momentum advection schemes, vertical and horizontal difference schemes, and time differencing schemes are discussed.

Patient-reported Outcomes of Tarsal Coalitions Treated With Surgical Excision.

PubMed

Mahan, Susan T; Spencer, Samantha A; Vezeridis, Peter S; Kasser, James R

2015-09-01

There are little patient-reported data on functional outcomes of tarsal coalition resection in children and adolescents. The purpose of this study is to evaluate the medium-term (>2 y) outcomes in patients who have had surgical excision of their symptomatic tarsal coalition and to compare patient-based outcomes in patients who have calcaneonavicular (CN) coalitions to those with talocalcaneal (TC) coalitions. A billing query was conducted to identify patients who had surgical excision of their tarsal coalition between 2003 and 2008. Eligible patients were mailed questionnaires consisting of a modified American Orthopaedic Foot and Ankle Society (AOFAS) score and the University of California at Los Angeles (UCLA) activity scale. Patients were also specifically asked if their activity level was limited by their foot pain. Only patients who returned questionnaires were included. Demographics and diagnostic images were reviewed. A nonresponder analysis was completed. Complications such as infection and reoperation were reported. Sixty-three patients (22 females, 41 males) who returned questionnaires were included in the analysis. Twenty-four patients had bilateral surgery. TC coalitions were present in 20 patients (32%); CN coalitions were present in 43 patients (68%).Overall, mean modified AOFAS score was 88.3 and mean UCLA activity score was 8.33 at an average of 4.62 years after surgery. Patients who had TC coalitions had similar modified AOFAS scores (88.4) and UCLA activity scores (8.4) when compared with those with CN coalitions (88.0 and 8.3, both not significant).Of the 73% (46/63) patients who reported that their activity levels were not limited by their foot pain, the mean AOFAS score was 93.9 and the mean UCLA activity score was 8.9; 32 of these were CN and 14 were TC coalitions. Of the 27% (17/63) patients who reported that their activity levels were limited by their foot pain, the mean AOFAS score was 72.9 and the mean UCLA activity score was 6.9; 11 of these were CN and 6 were TC coalitions. There was a statistically significant difference in these groups both in modified AOFAS score (P<0.0001) and UCLA activity score (P=0.006). There was no difference in outcomes between those who were treated for a TC and CN coalition. Patient-reported outcomes after surgical excision of tarsal coalition reveal that >70% of patients' activities are not limited by pain and their functional outcome is terrific. A few patients continue to have problems with ongoing foot pain and activity limitations. The type of coalition does not seem to be an indicative factor in determining outcome.

Longitudinal Long-term Magnetic Resonance Imaging and Clinical Follow-up After Single-Row Arthroscopic Rotator Cuff Repair: Clinical Superiority of Structural Tendon Integrity.

PubMed

Heuberer, Philipp R; Smolen, Daniel; Pauzenberger, Leo; Plachel, Fabian; Salem, Sylvia; Laky, Brenda; Kriegleder, Bernhard; Anderl, Werner

2017-05-01

The number of arthroscopic rotator cuff surgeries is consistently increasing. Although generally considered successful, the reported number of retears after rotator cuff repair is substantial. Short-term clinical outcomes are reported to be rarely impaired by tendon retears, whereas to our knowledge, there is no study documenting long-term clinical outcomes and tendon integrity after arthroscopic rotator cuff repair. To investigate longitudinal long-term repair integrity and clinical outcomes after arthroscopic rotator cuff reconstruction. Case series; Level of evidence, 4. Thirty patients who underwent arthroscopic rotator cuff repair with suture anchors for a full-tendon full-thickness tear of the supraspinatus or a partial-tendon full-thickness tear of the infraspinatus were included. Two and 10 years after initial arthroscopic surgery, tendon integrity was analyzed using magnetic resonance imaging (MRI). The University of California, Los Angeles (UCLA) score and Constant score as well as subjective questions regarding satisfaction with the procedure and return to normal activity were used to evaluate short- and long-term outcomes. At the early MRI follow-up, 42% of patients showed a full-thickness rerupture, while 25% had a partial rerupture, and 33% of tendons remained intact. The 10-year MRI follow-up (129 ± 11 months) showed 50% with a total rerupture, while the other half of the tendons were partially reruptured (25%) or intact (25%). The UCLA and Constant scores significantly improved from preoperatively (UCLA total: 50.6% ± 20.2%; Constant total: 44.7 ± 10.5 points) to 2 years (UCLA total: 91.4% ± 16.0% [ P < .001]; Constant total: 87.8 ± 15.3 points [ P < .001]) and remained significantly higher after 10 years (UCLA total: 89.7% ± 15.9% [ P < .001]; Constant total: 77.5 ± 15.6 points [ P < .001]). The Constant total score and Constant strength subscore, but not the UCLA score, were also significantly better at 10 years postoperatively in patients with intact tendons compared with patients with retorn tendons (Constant total: 89.0 ± 7.8 points vs 75.7 ± 14.1 points, respectively [ P = .034]; Constant strength: 18.0 ± 4.9 points vs 9.2 ± 5.2 points, respectively [ P = .006]). The majority of patients rated their satisfaction with the procedure as "excellent" (83.3%), and 87.5% returned to their normal daily activities. Arthroscopic rotator cuff repair showed good clinical long-term results despite a high rate of retears. Nonetheless, intact tendons provided significantly superior clinical long-term outcomes, making the improvement of tendon healing and repair integrity important goals of future research efforts.

Patrick Moore's Data Book of Astronomy

NASA Astrophysics Data System (ADS)

Moore, Patrick; Rees, Robin

2014-01-01

1. The Solar System; 2. The Sun; 3. The Moon; 4. Mercury; 5. Venus; 6. Earth; 7. Mars; 8. The asteroid belt; 9. Jupiter; 10. Saturn; 11. Uranus; 12. Neptune; 13. Beyond Neptune: the Kuiper Belt; 14. Comets; 15. Meteors; 16. Meteorites; 17. Glows and atmospheric effects; 18. The stars; 19. Stellar spectra and evolution; 20. Extrasolar planets; 21. Double stars; 22. Variable stars; 23. Stellar clusters; 24. Nebulae; 25. The Galaxy; 26. The evolution of the Universe; 27. The constellations; 28. The star catalogue; 29. Telescopes and observatories; 30. Non-optical astronomy; 31. The history of astronomy; 32. Astronomers; 33. Glossary; Index.

Between history, art and medicine: the Dresden-Friedrichstadt hospital, its Neptune fountain and connections to Vienna.

PubMed

Wollina, Uwe; Hunger, Sabine; Koch, André; França, Katlein; Lotti, Torello; Fioranelli, Massimo; Roccia, Maria Grazia

2017-10-01

The Dresden-Friedrichstadt hospital originated from Marcolini's summer palace. It was founded in 1845 and opened in 1849. It is a place where history and art of European importance mixes with technical and medical innovations. We reflect on the meetings of Napoleon Bonaparte and Metternich in 1812, the creation of the famous Neptune fountain by Longuelune and Matielli and two outstanding physicians of the 19 th  century, the surgeon Eduard Zeis, who coined the medical term "plastic surgery", and Maximilian Nitze, inventor of the first "modern" cystoscope and the father of urology.

Clouds on Neptune: Motions, Evolution, and Structure

NASA Technical Reports Server (NTRS)

Sromovsky, Larry A.; Morgan, Thomas (Technical Monitor)

2001-01-01

The aims of our original proposal were these: (1) improving measurements of Neptune's circulation, (2) understanding the spatial distribution of cloud features, (3) discovery of new cloud features and understanding their evolutionary process, (4) understanding the vertical structure of zonal cloud patterns, (5) defining the structure of discrete cloud features, and (6) defining the near IR albedo and light curve of Triton. Towards these aims we proposed analysis of existing 1996 groundbased NSFCAM/IRTF observations and nearly simultaneous WFPC2 observations from the Hubble Space Telescope. We also proposed to acquire new observations from both HST and the IRTF.

Angle-of-Attack-Modulated Terminal Point Control for Neptune Aerocapture

NASA Technical Reports Server (NTRS)

Queen, Eric M.

2004-01-01

An aerocapture guidance algorithm based on a calculus of variations approach is developed, using angle of attack as the primary control variable. Bank angle is used as a secondary control to alleviate angle of attack extremes and to control inclination. The guidance equations are derived in detail. The controller has very small onboard computational requirements and is robust to atmospheric and aerodynamic dispersions. The algorithm is applied to aerocapture at Neptune. Three versions of the controller are considered with varying angle of attack authority. The three versions of the controller are evaluated using Monte Carlo simulations with expected dispersions.

Parkes radio science system design and testing for Voyager Neptune encounter

NASA Technical Reports Server (NTRS)

Rebold, T. A.; Weese, J. F.

1989-01-01

The Radio Science System installed at Parkes, Australia for the Voyager Neptune encounter was specified to meet the same stringent requirements that were imposed upon the Deep Space Network Radio Science System. The system design and test methodology employed to meet these requirements at Parkes are described, and data showing the measured performance of the system are presented. The results indicate that the system operates with a comfortable margin on the requirements. There was a minor problem with frequency-dependent spurious signals which could not be fixed before the encounter. Test results characterizing these spurious signals are included.

A model of Neptune according to the Savic-Kasanin theory

NASA Astrophysics Data System (ADS)

Celebonovic, V.

1983-10-01

The structure and the distributions of temperature, pressure and density in the interior of Neptune are calculated using the pressure-ionization model of Savic and Kasanin (1961-1965). The model input data comprise only the mass, radius and moment of inertia; the results are presented in a graph and a table. A four-zone structure is defined, and the parameter values and profiles are found to be in good agreement with those of more complex models. Differences can be attributed to the crudeness of the present model but also to possible errors in the assumptions required by other models.

Phone behaviour and its relationship to loneliness in older adults

PubMed Central

Petersen, Johanna; Thielke, Stephen; Austin, Daniel; Kaye, Jeffrey

2015-01-01

Objectives Loneliness and social isolation are two important health outcomes among older adults. Current assessment of these outcomes relies on self-report which is susceptible to bias. This paper reports on the relationship between loneliness and objective measures of isolation using a phone monitoring device. Method Phone monitors were installed in the homes of 26 independent elderly individuals from the ORCATECH Life Laboratory cohort (age 86 ± 4.5, 88% female) and used to monitor the daily phone usage for an average of 174 days. Loneliness was assessed using the 20-item University of California Los Angeles (UCLA) Loneliness scale. A mixed effects negative binomial regression was used to model the relationship between loneliness and social isolation, as assessed using the total number of calls, controlling for cognitive function, pain, age, gender, and weekday. A secondary analysis examined the differential effect of loneliness on incoming and outgoing calls. Results The average UCLA Loneliness score was 35.3 ± 7.6, and the median daily number of calls was 4. Loneliness was negatively associated with telephone use (IRR = 0.99, p < 0.05). Daily phone use was also associated with gender (IRR = 2.03, p < 0.001) and cognitive status (IRR = 1.51, p < 0.001). The secondary analysis revealed that loneliness was significantly related to incoming (IRR = 0.98, p < 0.01) but not outgoing calls. Conclusions These results demonstrate the close relationship between loneliness and social isolation, showing that phone behaviour is associated with emotional state and cognitive function. Because phone behaviour can be monitored unobtrusively, it may be possible to sense loneliness levels in older adults using objective assessments of key aspects of behaviour. PMID:26133745

Phone behaviour and its relationship to loneliness in older adults.

PubMed

Petersen, Johanna; Thielke, Stephen; Austin, Daniel; Kaye, Jeffrey

2016-10-01

Loneliness and social isolation are two important health outcomes among older adults. Current assessment of these outcomes relies on self-report which is susceptible to bias. This paper reports on the relationship between loneliness and objective measures of isolation using a phone monitoring device. Phone monitors were installed in the homes of 26 independent elderly individuals from the ORCATECH Life Laboratory cohort (age 86 ± 4.5, 88% female) and used to monitor the daily phone usage for an average of 174 days. Loneliness was assessed using the 20-item University of California Los Angeles (UCLA) Loneliness scale. A mixed effects negative binomial regression was used to model the relationship between loneliness and social isolation, as assessed using the total number of calls, controlling for cognitive function, pain, age, gender, and weekday. A secondary analysis examined the differential effect of loneliness on incoming and outgoing calls. The average UCLA Loneliness score was 35.3 ± 7.6, and the median daily number of calls was 4. Loneliness was negatively associated with telephone use (IRR = 0.99, p < 0.05). Daily phone use was also associated with gender (IRR = 2.03, p < 0.001) and cognitive status (IRR = 1.51, p < 0.001). The secondary analysis revealed that loneliness was significantly related to incoming (IRR = 0.98, p < 0.01) but not outgoing calls. These results demonstrate the close relationship between loneliness and social isolation, showing that phone behaviour is associated with emotional state and cognitive function. Because phone behaviour can be monitored unobtrusively, it may be possible to sense loneliness levels in older adults using objective assessments of key aspects of behaviour.

A High Mass & Low Envelope Fraction for the Warm Neptune K2-55b

NASA Astrophysics Data System (ADS)

Dressing, Courtney; Sinukoff, Evan; Fulton, Benjamin; Lopez, Eric; Beichman, Charles; Howard, Andrew; Knutson, Heather; Werner, Michael; Schlieder, Joshua; Benneke, Björn; Crossfield, Ian; Isaacson, Howard; Krick, Jessica; Gorjian, Varoujan; Livingston, John; Petigura, Erik; Akeson, Rachel; Batygin, Konstantin; Christiansen, Jessie; Ciardi, David; Crepp, Justin; Jasmine Gonzales, Erica; Hardegree-Ullman, Kevin; Hirsch, Lea; Kosiarek, Molly; Weiss, Lauren

2018-01-01

The NASA K2 mission is using the Kepler spacecraft to search for transiting planets in multiple fields along the ecliptic plane. One of the planets detected by K2 is K2-55b, a warm Neptune in a short-period orbit (2.8 days) around a late K dwarf. We previously obtained near-infrared spectra from IRTF/SpeX to characterize the system and found that the host star K2-55 has a radius of 0.715 (+0.043/-0.040) solar radii, a mass of 0.668 (+/- 0.069) solar masses, and an effective temperature of 4300K (+100/-107). We then combined our updated stellar properties with new fits to the K2 photometry to estimate a planet radius of 4.38 (+0.29/-0.25) Earth radii, confirmed the transit ephemeris using Spitzer/IRAC (GO 11026, PI Werner), and embarked on radial velocity observations with Keck/HIRES to measure the planet mass. Our RV data suggest that K2-55b is much more massive than expected, indicating that the planet has a high density despite having a relatively high mass. The lack of a significant volatile envelope tests current theories of gas giant formation and indicates that K2-55b may have avoided runaway accretion by migration, delayed formation, or inefficient core accretion. We gratefully acknowledge funding from the NASA Sagan Fellowship Program and the NASA K2 Guest Observer Program. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.

The influence of abutment angulation on screw loosening of implants in the anterior maxilla.

PubMed

Ha, Chun-Yeo; Lim, Yung-Jun; Kim, Myung-Joo; Choi, Jung-Han

2011-01-01

This study compared the removal torque values (RTVs) of different abutments (straight, angled, and gold premachined UCLA-type) in external- and internal-hex implants after dynamic cyclic loading with the clinical situation of the anterior maxilla simulated. An ideal cast of a maxilla with a missing right central incisor was fabricated in dental stone, and an implant analog was embedded in this model at a 15-degree angle labial to the long axis of the left central incisor. Thirty external-hex and 30 internal-hex implants were used. A total of 10 straight abutments, 10 angled abutments, and 10 gold premachined UCLA-type abutments of each system and 60 abutment screws were tested. Initial RTVs were measured after each assembly was tightened to 30 Ncm. Straight abutments and angled abutments were prepared and gold-premachined UCLA-type abutments were waxed and cast with low-fusing gold alloy for the central incisor. RTVs were then measured again. After each assembly was tightened, a metal crown was temporarily cemented. After cyclic loading of 20 to 200 N was applied 1 million times, RTVs were measured for a third time. Statistical analysis (alpha = .05) was performed to evaluate the results. The angled abutment group showed significantly higher RTVs than the straight abutment and gold premachined UCLA-type abutment groups in external-hex implants. However, no significant difference in RTVs was found among abutments in internal-hex implants. The time of analysis of RTV was found to significantly influence mean RTVs. Mean RTVs of external- and internal-hex implants showed significant differences. Within the limitations of this study, there were significant differences in RTVs among different abutment groups in external-hex implants. There were no significant differences in RTVs among different abutment groups in internal-hex implants.

The evolution of a Pluto-like system during the migration of the ice giants

NASA Astrophysics Data System (ADS)

Pires, Pryscilla; Giuliatti Winter, Silvia M.; Gomes, Rodney S.

2015-01-01

The planetary migration of the Solar System giant planets in the framework of the Nice model (Tsiganis, K., Gomes, R., Morbidelli, A., Levison, H.F. [2005]. Nature 435,459-461; Morbidelli, A., Levison, H.F., Tsiganis, K., Gomes, R. [2005]. Nature 435, 462-465; Gomes, R., Levison, H.F., Tsiganis, K., Morbidelli, A. [2005]. Nature 435, 466-469) creates a dynamical mechanism which can be used to explain the distribution of objects currently observed in the Kuiper belt (e.g., Levison, H.F., Morbidelli, A., Vanlaerhoven, C., Gomes, R., Tsiganis, K. [2008]. Icarus 196, 258-273). Through this mechanism the planetesimals within the disk, heliocentric distance ranging from beyond Neptune's orbit to approximately 34 AU, are delivered to the belt after a temporary eccentric phase of Uranus and Neptune's orbits. We reproduced the mechanism proposed by Levison et al. to implant bodies into the Kuiper belt. The capture of Pluto into the external 3:2 mean motion resonance with Neptune is associated with this gravitational scattering model. We verified the existence of several close encounters between the ice giants and the planetesimals during their outward radial migration, then we believe that the analysis of the dynamical history of the plutonian satellites during this kind of migration is important, and would provide some constrains about their place of formation - within the primordial planetesimal disk or in situ. We performed N-body simulations and recorded the trajectories of the planetesimals during close approaches with Uranus and Neptune. Close encounters with Neptune are the most common, reaching approximately 1200 in total. A Pluto similarly sized body assumed the hyperbolic trajectories of the former primordial planetesimal with respect to those giant planets. We assumed the current mutual orbital configuration and sizes for Pluto's satellites, then we found that the rate of destruction of systems similar to that of Pluto with closest approaches to Uranus or Neptune <0.10 AU is 40%, i.e. these close approaches can lead to ejections of satellites or to changes in the satellites eccentricities at least 1 order of magnitude larger than the currently observed. However, we also found that the number of closest approaches which the minimum separation to Uranus or Neptune <0.10 AU is negligible, reaching 6%. In the other 60% of close encounter histories with closest approaches >0.10 AU, none of the systems have been destroyed. The latter sample concentrates 94% of closest approaches with the ice giants. Recall that throughout the early history of the Solar System giant impacts were common (McKinnon, W.B. [1989]. Astrophys. J. 344, L41-L44; Stern, A. [1991]. Icarus 90; Canup, R.M. [2005]. Science 307, 546-550). Also, impacts capable of forming a binary like Pluto-Charon can occur possibly prior to 0.5-1 Gyr (Kenyon, S.J., Bromley, B.C. [2014]. Astron. J. 147, 8), and small satellites such as Nix and Hydra can grow in debris from the giant impact (e.g., Canup, R.M. [2011]. Astron. J. 141, 35). Thus, we conclude that if Pluto and its satellites were emplaced into the KB from lower heliocentric orbits, then the Pluto system could survive the encounters that may have happened for emplacement of the Plutinos through the mechanism proposed by Levison et al.

An interpretation of a mysterious 3.0- to 4.6-kHz emission band observed on Voyager 2 near Neptune

NASA Technical Reports Server (NTRS)

Sonwalkar, Vikas S.; Inan, Umran S.; Bell, Timothy F.

1995-01-01

A whistler mode interpretation is provided for the narrowband signal (f approx. 3 - 4.6 kHz, Delta f approx. 200 - 800 Hz) detected by the plasma wave instrument on Voyager 2 during its encounter with Neptune. Our analysis indicates that this signal may have been generated in a limited spatial region and that it propagated to other regions of the Neptunian magnetosphere in the nonducted whistler mode with wave normal vectors lying close to the whistler mode resonance cone. The observed frequency variation of the emission along the Voyager 2 trajectory is consistent with this interpretation. The source location is estimated to be near the magnetic equator at L approx. 4 and dipole longitude of 111 deg W (260 deg W longitude in Neptune coordinate system). The source frequency and bandwidth are estimated to be 3.6 kHz and 300 Hz, respectively. The waves most likely would have been generated by energetic electrons with 2- to 20-keV parallel energy via a gyroresonance mechanism. Our interpretation of the narrowband emissions places the following limits on the Neptunian thermal plasma density and temperature: (1) N(sub e, min) greater than 0.16 el/cu cm for 1.2 R(sub N) less than R less than 5 R(sub N), (2) N(sub e, max) = 597.5/cu cm at R - 1.3 R(sub N), (3) T(sub e, max) less than 500-1000 K at R approx. 5 R(sub N). It is also possible that the weak UV aurora observed near Neptune could have been caused by the precipitation of energetic particles by the narrowband emission as a result of wave particle interactions.

Monitoring Active Atmospheres on Uranus and Neptune

NASA Astrophysics Data System (ADS)

Rages, Kathy

2009-07-01

We propose Snapshot observations of Uranus and Neptune to monitor changes in their atmospheres on time scales of weeks and months, as we have been doing for the past seven years. Previous Hubble Space Telescope observations {including previous Snapshot programs 8634, 10170, 10534, and 11156}, together with near-IR images obtained using adaptive optics on the Keck Telescope, reveal both planets to be dynamic worlds which change on time scales ranging from hours to {terrestrial} years. Uranus equinox occurred in December 2007, and the northern hemisphere is becoming fully visible for the first time since the early 1960s. HST observations during the past several years {Hammel et al. 2005, Icarus 175, 284 and references therein} have revealed strongly wavelength-dependent latitudinal structure, the presence of numerous visible-wavelength cloud features in the northern hemisphere, at least one very long-lived discrete cloud in the southern hemisphere, and in 2006 the first clearly defined dark spot seen on Uranus. Long-term ground-based observations {Lockwood and Jerzekiewicz, 2006, Icarus 180, 442; Hammel and Lockwood 2007, Icarus 186, 291} reveal seasonal brightness changes that seem to demand the appearance of a bright northern polar cap within the next few years. Recent HST and Keck observations of Neptune {Sromovsky et al. 2003, Icarus 163, 256 and references therein} show a general increase in activity at south temperate latitudes until 2004, when Neptune returned to a rather Voyager-like appearance with discrete bright spots rather than active latitude bands. Further Snapshot observations of these two dynamic planets will elucidate the nature of long-term changes in their zonal atmospheric bands and clarify the processes of formation, evolution, and dissipation of discrete albedo features.

Why is it so difficult to tilt Uranus?

NASA Astrophysics Data System (ADS)

Rogoszinski, Zeeve; Hamilton, Douglas

2018-04-01

The leading hypothesis for the origin of Uranus' large obliquity (98°) is a polar strike from an Earth sized object, but to tilt Saturn similarly would require an impactor roughly 10x as massive. A more likely cause for Saturn's tilt (27°) is a spin-orbit resonance with Neptune (Ward & Hamilton, 2004; Hamilton & Ward, 2004); might the same process work for Uranus? It initially seems unlikely, as at its current location Uranus' axial precession period is too long to resonate with any of the giant planets' orbital precession frequencies. If we place Uranus between Jupiter and Saturn, however, then Uranus' spin axis would precess much more quickly. Thommes et al. (1999, 2002, 2003) first postulated that Uranus and Neptune were formed between Jupiter and Saturn because the conditions there allow the ice giants to be built rapidly. A resonance for our closer Uranus still requires a distant planet, nevertheless, a condition that can be satisfied if Neptune is ejected from Jupiter and Saturn first with Uranus following significantly later. This scenario, while contrived, is consistent with at least some versions of the Nice model and allows us to fully test the resonance hypothesis. We discovered that even with these optimistic assumptions, i) a resonance capture requires a migration timescale on the order of 100 Myr, and ii) it is impossible to tilt Uranus past 90°. Increasing Neptune's migration speed precludes resonant capture, and instead results in a resonance kick. In the most favorable cases, a resonance kick could raise Uranus' obliquity by 40° on a time span of about 50 Myr. We conclude that even in our best scenario, a resonance cannot fully account for Uranus' tilt. We have investigated some scenarios that include both resonances and collisions, and will report on our findings.

Scientific rationale for Uranus and Neptune in situ explorations

NASA Astrophysics Data System (ADS)

Mousis, O.; Atkinson, D. H.; Cavalié, T.; Fletcher, L. N.; Amato, M. J.; Aslam, S.; Ferri, F.; Renard, J.-B.; Spilker, T.; Venkatapathy, E.; Wurz, P.; Aplin, K.; Coustenis, A.; Deleuil, M.; Dobrijevic, M.; Fouchet, T.; Guillot, T.; Hartogh, P.; Hewagama, T.; Hofstadter, M. D.; Hue, V.; Hueso, R.; Lebreton, J.-P.; Lellouch, E.; Moses, J.; Orton, G. S.; Pearl, J. C.; Sánchez-Lavega, A.; Simon, A.; Venot, O.; Waite, J. H.; Achterberg, R. K.; Atreya, S.; Billebaud, F.; Blanc, M.; Borget, F.; Brugger, B.; Charnoz, S.; Chiavassa, T.; Cottini, V.; d'Hendecourt, L.; Danger, G.; Encrenaz, T.; Gorius, N. J. P.; Jorda, L.; Marty, B.; Moreno, R.; Morse, A.; Nixon, C.; Reh, K.; Ronnet, T.; Schmider, F.-X.; Sheridan, S.; Sotin, C.; Vernazza, P.; Villanueva, G. L.

2018-06-01

The ice giants Uranus and Neptune are the least understood class of planets in our solar system but the most frequently observed type of exoplanets. Presumed to have a small rocky core, a deep interior comprising ∼70% heavy elements surrounded by a more dilute outer envelope of H2 and He, Uranus and Neptune are fundamentally different from the better-explored gas giants Jupiter and Saturn. Because of the lack of dedicated exploration missions, our knowledge of the composition and atmospheric processes of these distant worlds is primarily derived from remote sensing from Earth-based observatories and space telescopes. As a result, Uranus's and Neptune's physical and atmospheric properties remain poorly constrained and their roles in the evolution of the Solar System not well understood. Exploration of an ice giant system is therefore a high-priority science objective as these systems (including the magnetosphere, satellites, rings, atmosphere, and interior) challenge our understanding of planetary formation and evolution. Here we describe the main scientific goals to be addressed by a future in situ exploration of an ice giant. An atmospheric entry probe targeting the 10-bar level, about 5 scale heights beneath the tropopause, would yield insight into two broad themes: i) the formation history of the ice giants and, in a broader extent, that of the Solar System, and ii) the processes at play in planetary atmospheres. The probe would descend under parachute to measure composition, structure, and dynamics, with data returned to Earth using a Carrier Relay Spacecraft as a relay station. In addition, possible mission concepts and partnerships are presented, and a strawman ice-giant probe payload is described. An ice-giant atmospheric probe could represent a significant ESA contribution to a future NASA ice-giant flagship mission.

Parametric Simulations of the Great Dark Spots of Neptune

NASA Astrophysics Data System (ADS)

Deng, Xiaolong; Le Beau, R.

2006-09-01

Observations by Voyager II and the Hubble Space Telescope of the Great Dark Spots (GDS) of Neptune suggest that large vortices with lifespans of years are not uncommon occurrences in the atmosphere of Neptune. The variability of these features over time, in particular the complex motions of GDS-89, make them challenging candidates to simulate in atmospheric models. Previously, using the Explicit Planetary Isentropic-Coordinate (EPIC) General Circulation Model, LeBeau and Dowling (1998) simulated the GDS-like vortex features. Qualitatively, the drift, oscillation, and tail-like features of GDS-89 were recreated, although precise numerical matches were only achieved for the meridional drift rate. In 2001, Stratman et al. applied EPIC to simulate the formation of bright companion clouds to the Great Dark Spots. In 2006, Dowling et al. presented a new version of EPIC, which includes hybrid vertical coordinate, cloud physics, advanced chemistry, and new turbulence models. With the new version of EPIC, more observation results, and more powerful computers, it is the time to revisit CFD simulations of the Neptune's atmosphere and do more detailed work on GDS-like vortices. In this presentation, we apply the new version of EPIC to simulate GDS-89. We test the influences of different parameters in the EPIC model: potential vorticity gradient, wind profile, initial latitude, vortex shape, and vertical structure. The observed motions, especially the latitudinal drift and oscillations in orientation angle and aspect ratio, are used as diagnostics of these unobserved atmospheric conditions. Increased computing power allows for more refined and longer simulations and greater coverage of the parameter space than previous efforts. Improved quantitative results have been achieved, including voritices with near eight-day oscillations and comparable variations in shape to GDS-89. This research has been supported by Kentucky NASA EPSCoR.

Atmospheric Dynamics of the Outer Planets

NASA Technical Reports Server (NTRS)

Ingersoll, Andrew P.

2002-01-01

The giant planets-Jupiter, Saturn, Uranus, and Neptune-are fluid objects. The winds are powered by absorbed sunlight, as on earth, and by internal heat left over from planetary formation. The main constituents of the atmospheres are hydrogen and helium. The clouds are made of ammonia, hydrogen sulphide, and water. All four giant planets are banded, with multiple zonal jet streams. Even Uranus, whose spin axis is tipped by 98deg relative to the orbit axis, shows latitudinal banding and zonal jets. Equator-to-pole temperature differences are close to zero. Wind speeds are larger than on earth and do not decrease with distance from the sun. Although the power/area at Neptune is only 1/20 that at Jupiter, the winds at Neptune are three times stronger. Stable vortices like the Great Red Spot of Jupiter and similar spots on Neptune come in all size ranges and exhibit a variety of behaviours including merging, orbiting, filament ejection, and oscillating in both shape and position. At least at cloud-top levels, 90% of the long-lived vortices are anticyclonic and sit in anticyclonic shear zones. Features in the cyclonic zones tend to be chaotic, with lifetimes of several days or less. These mesoscale eddies tend to have lightning in them, which suggests that they get their energy from moist convection. The rate of conversion of eddy kinetic energy into kinetic energy of the zonal jets is more than 10% of the power/area radiated by Jupiter. This fraction is more than an order of magnitude larger than on earth. Several lines of evidence now indicate that the winds at cloud-top levels are the surface manifestation of deep-rooted motions that extend into the interior and are presumably driven by internal heat.

Aerocapture Performance Analysis for a Neptune-Triton Exploration Mission

NASA Technical Reports Server (NTRS)

Starr, Brett R.; Westhelle, Carlos H.; Masciarelli, James P.

2004-01-01

A systems analysis has been conducted for a Neptune-Triton Exploration Mission in which aerocapture is used to capture a spacecraft at Neptune. Aerocapture uses aerodynamic drag instead of propulsion to decelerate from the interplanetary approach trajectory to a captured orbit during a single pass through the atmosphere. After capture, propulsion is used to move the spacecraft from the initial captured orbit to the desired science orbit. A preliminary assessment identified that a spacecraft with a lift to drag ratio of 0.8 was required for aerocapture. Performance analyses of the 0.8 L/D vehicle were performed using a high fidelity flight simulation within a Monte Carlo executive to determine mission success statistics. The simulation was the Program to Optimize Simulated Trajectories (POST) modified to include Neptune specific atmospheric and planet models, spacecraft aerodynamic characteristics, and interplanetary trajectory models. To these were added autonomous guidance and pseudo flight controller models. The Monte Carlo analyses incorporated approach trajectory delivery errors, aerodynamic characteristics uncertainties, and atmospheric density variations. Monte Carlo analyses were performed for a reference set of uncertainties and sets of uncertainties modified to produce increased and reduced atmospheric variability. For the reference uncertainties, the 0.8 L/D flatbottom ellipsled vehicle achieves 100% successful capture and has a 99.87 probability of attaining the science orbit with a 360 m/s V budget for apoapsis and periapsis adjustment. Monte Carlo analyses were also performed for a guidance system that modulates both bank angle and angle of attack with the reference set of uncertainties. An alpha and bank modulation guidance system reduces the 99.87 percentile DELTA V 173 m/s (48%) to 187 m/s for the reference set of uncertainties.

UCLA Demodulation Engine,

DTIC Science & Technology

1983-03-01

36*13.2 Implementation .................................................................................. 36 3.3 Cells ...46 4.2 Cells ...56 5.1 Implementation .................................................................................. 57 5.3 Cells

SAPS simulation with GITM/UCLA-RCM coupled model

NASA Astrophysics Data System (ADS)

Lu, Y.; Deng, Y.; Guo, J.; Zhang, D.; Wang, C. P.; Sheng, C.

2017-12-01

Abstract: SAPS simulation with GITM/UCLA-RCM coupled model Author: Yang Lu, Yue Deng, Jiapeng Guo, Donghe Zhang, Chih-Ping Wang, Cheng Sheng Ion velocity in the Sub Aurora region observed by Satellites in storm time often shows a significant westward component. The high speed westward stream is distinguished with convection pattern. These kind of events are called Sub Aurora Polarization Stream (SAPS). In March 17th 2013 storm, DMSP F18 satellite observed several SAPS cases when crossing Sub Aurora region. In this study, Global Ionosphere Thermosphere Model (GITM) has been coupled to UCLA-RCM model to simulate the impact of SAPS during March 2013 event on the ionosphere/thermosphere. The particle precipitation and electric field from RCM has been used to drive GITM. The conductance calculated from GITM has feedback to RCM to make the coupling to be self-consistent. The comparison of GITM simulations with different SAPS specifications will be conducted. The neutral wind from simulation will be compared with GOCE satellite. The comparison between runs with SAPS and without SAPS will separate the effect of SAPS from others and illustrate the impact on the TIDS/TADS propagating to both poleward and equatorward directions.

Tracking and sustaining improvement initiatives: leveraging quality dashboards to lead change in a neurosurgical department.

PubMed

McLaughlin, Nancy; Afsar-Manesh, Nasim; Ragland, Victoria; Buxey, Farzad; Martin, Neil A

2014-03-01

Increasingly, hospitals and physicians are becoming acquainted with business intelligence strategies and tools to improve quality of care. In 2007, the University of California Los Angeles (UCLA) Department of Neurosurgery created a quality dashboard to help manage process measures and outcomes and ultimately to enhance clinical performance and patient care. At that time, the dashboard was in a platform that required data to be entered manually. It was then reviewed monthly to allow the department to make informed decisions. In 2009, the department leadership worked with the UCLA Medical Center to align mutual quality-improvement priorities. The content of the dashboard was redesigned to include 3 areas of priorities: quality and safety, patient satisfaction, and efficiency and use. Throughout time, the neurosurgery quality dashboard has been recognized for its clarity and its success in helping management direct improvement strategies and monitor impact. We describe the creation and design of the neurosurgery quality dashboard at UCLA, summarize the evolution of its assembly process, and illustrate how it can be used as a powerful tool of improvement and change. The potential challenges and future directions of this business intelligence tool are also discussed.

Ethane abundance on Neptune

NASA Technical Reports Server (NTRS)

Kostiuk, Theodor; Espenak, Fred; Romani, Paul; Zipoy, David; Goldstein, Jeff

1990-01-01

IR spectroscopic measurements of the C2H6 RR (4,5) emission line at 840.9764/cm have been used to infer Neptune's ethane mole fractions; while the resulting value is lower than that obtained by Orton et al. (1987), it lies within their 2-sigma error bounds. The present results are also found to require 2.0-5.8 times more ethane in the 0.02-2 mbar pressure region than predicted by the Romani and Atreya (1989) photochemical model. Better agreement is obtainable through a reduction of eddy mixing in the lower stratosphere and/or an increase of stratospheric temperature by more than 10 K above the 6-mbar level.

Interagency telemetry arraying for Voyager-Neptune encounter

NASA Technical Reports Server (NTRS)

Brown, D. W.; Brundage, W. D.; Ulvestad, J. S.; Kent, S. S.; Bartos, K. P.

1990-01-01

The reception capability of the Deep Space Network (DSN) has been improved over the years by increasing both the size and number of antennas at each complex to meet spacecraft-support requirements. However, even more aperture was required for the final planetary encounters of the Voyager 2 spacecraft. This need was met by arraying one radio astronomy observatory with the DSN complex in the United States and another with the complex in Australia. Following a review of augmentation for the Uranus encounter, both the preparation at the National Radio Astronomy (NRAO) Very Large Array (VLA) and the Neptune encounter results for the Parkes-Canberra and VLA-Goldstone arrays are presented.

The atmospheric structure and dynamical properties of Neptune derived from ground-based and IUE spectrophotometry

NASA Technical Reports Server (NTRS)

Baines, Kevin H.; Smith, Wm. Hayden

1990-01-01

A wide range of recent full-disk spectral observations is used to constrain the atmospheric structure and dynamical properties of Neptune; analytical determinations are made of the abundances of such spectrally active gas species as the deep-atmosphere CH4 molar fraction and the mean ortho/para hydrogen ratio in the visible atmosphere, as well as stratospheric and tropospheric aerosol properties. Compared to Uranus, the greater abundance and shorter lifetimes of Neptunian particulates in the stratospheric region irradiated by the solar UV flux indicate that such radiation is the darkening agent of stratospheric aerosols on both planets.

Outer-Planet Mission Analysis Using Solar-Electric Ion Propulsion

NASA Technical Reports Server (NTRS)

Woo, Byoungsam; Coverstone, Victoria L.; Hartmann, John W.; Cupples, Michael

2003-01-01

Outer-planet mission analysis was performed using three next generation solar-electric ion thruster models. Optimal trajectories are presented that maximize the delivered mass to the designated outer planet. Trajectories to Saturn and Neptune with a single Venus gravity assist are investigated. For each thruster model, the delivered mass versus flight time curve was generated to obtain thruster model performance. The effects of power to the thrusters and resonance ratio of Venutian orbital periods to spacecraft period were also studied. Multiple locally optimal trajectories to Saturn and Neptune have been discovered in different regions of the parameter search space. The characteristics of each trajectory are noted.

Neptune's Triton: A moon rich in dry ice and carbon

NASA Technical Reports Server (NTRS)

Prentice, A. J. R.

1989-01-01

The encounter of the spacecraft Voyager 2 with Neptune and its large satellite Triton in August 1989 will provide a crucial test of ideas regarding the origin and chemical composition of the outer solar system. In this pre-encounter publication, the possibility is quantified that Titron is a captured moon which, like Pluto and Charon, originally condensed as a major planetesimal within the gas ring that was shed by the contracting protosolar cloud at Neptune's orbit. Ideas of supersonic convective turbulence are used to compute the gas pressure, temperature and rat of catalytic synthesis of CH4, CO2, and C(s) within the protosolar cloud, assuming that all C is initially present as CO. The calculations lead to a unique composition for Triton, Pluto, Charon: each body consists of, by mass, 18 1/2 percent solid CO2 ice, 4 percent graphite, 1/2 percent CH4 ice, 29 percent methanated water ice and 48 percent of anhydrous rock. This mix has a density consistent with that of the Pluto-Charon system and yields a predicted mean density for Triton of 2.20 + or - 0.5 g/cu cm, for satellite radius equal to 1,750 km.

Resolving the inconsistency between the ice giants and cometary D/H ratios

NASA Astrophysics Data System (ADS)

Ali-Dib, M.; Mousis, O.; Petit, J.-M.; Lunine, J. I.

2014-12-01

The properties and chemical compositions of giant planets strongly depend on their formation locations. The formation mechanisms of the ice giants Uranus and Neptune, and their elemental and isotopic compositions, have long been debated. The density of solids in the outer protosolar nebula is too low to explain their formation within a timescale consistent with the presence of the gaseous protoplanetary disk, and spectroscopic observations show that both planets are highly enriched in carbon, very poor in nitrogen, and the ices from which they originally formed might had deuterium-to-hydrogen ratios lower than the predicted cometary value, unexplained properties observed in no other planets. Here we show that all these properties can be explained naturally if Uranus and Neptune both formed at the carbon monoxide iceline location, namely the region where this gas condensates in the protosolar nebula. This outer region of the protosolar nebula intrinsically has enough surface density to form both planets from carbon-rich solids but nitrogen-depleted gas, in abundances consistent with their observed values. Water rich interiors originating mostly from transformed CO ices reconcile the D/H value observed in Uranus and Neptune with the cometary value.

The formation of Uranus and Neptune in the Jupiter-Saturn region of the Solar System.

PubMed

Thommes, E W; Duncan, M J; Levison, H F

1999-12-09

Planets are believed to have formed through the accumulation of a large number of small bodies. In the case of the gas-giant planets Jupiter and Saturn, they accreted a significant amount of gas directly from the protosolar nebula after accumulating solid cores of about 5-15 Earth masses. Such models, however, have been unable to produce the smaller ice giants Uranus and Neptune at their present locations, because in that region of the Solar System the small planetary bodies will have been more widely spaced, and less tightly bound gravitationally to the Sun. When applied to the current Jupiter-Saturn zone, a recent theory predicts that, in addition to the solid cores of Jupiter and Saturn, two or three other solid bodies of comparable mass are likely to have formed. Here we report the results of model calculations that demonstrate that such cores will have been gravitationally scattered outwards as Jupiter, and perhaps Saturn, accreted nebular gas. The orbits of these cores then evolve into orbits that resemble those of Uranus and Neptune, as a result of gravitational interactions with the small bodies in the outer disk of the protosolar nebula.

Thermochemistry and Photochemistry in Thick Atmospheres on Super Earths and Mini Neptunes

NASA Astrophysics Data System (ADS)

Hu, R.; Seager, S.

2013-12-01

Dectection and characterization of low-mass exoplanets is poised to accelerate in the coming decade. Some low-mass exoplanets, namely super Earths and some mini Neptunes, will likely have thick atmospheres that are not H2-dominated. We have developed a photochemistry-thermochemistry model for exploring the compositions of thick atmospheres on super Earths and mini Neptunes, applicable for both H2-dominated atmospheres and non-H2-dominated atmospheres. Using this model, we have simulated the molecular composition of thick atmospheres on warm and hot super Earths/mini Neptunes, and classified thick atmospheres into hydrogen-rich atmospheres, water-rich atmospheres, oxygen-rich atmospheres, and hydrocarbon-rich atmospheres, depending on the hydrogen abundance and the carbon to oxygen abundance ratio. We find that carbon has to be in the form of CO2 rather than CH4 or CO in an H2-depleted water-dominated thick atmosphere, and that the preferred loss of light elements from an oxygen-poor carbon-rich atmosphere leads to formation of unsaturated hydrocarbons. For future observations, we find for GJ 1214b that (1) C2H2 features at 1.0 and 1.5 μm in transmission are diagnostic for hydrocarbon-rich atmospheres; (2) a constraint on the thermal emission at 4.5 μm could differentiate water-rich atmospheres versus hydrocarbon-rich atmospheres; (3) a detection of water-vapor features and a confirmation of nonexistence of methane features would provide sufficient evidence for a water-dominated atmosphere. For a hot super Earth like 55 Cnc e, the diagnostic features of water-rich atmospheres (H2O) and the diagnostic features of hydrocarbon-rich atmospheres (CO and C2H2) are well separated in transmission spectra at 0.6-5 μm, which would enable straightforward characterization. In general, our simulations show that chemical stability has to be taken into account when interpreting the spectrum of a super Earth/mini Neptune. Theoretical transmission spectra and thermal emission spectra of non-H2-dominated atmospheres on GJ 1214b based on photochemistry-thermochemistry simulations in comparison with current observations. The simulated spectra are for an hydrogen abundance of 0.5 and a variety of carbon to oxygen ratios ranging from oxygen rich to carbon rich. The atmospheric scenarios with different carbon to oxygen ratios can be constrained via the spectral features of their hallmark molecules.

Ongoing Dynamics and Evolution of Neptune's Ring-Moon System

NASA Astrophysics Data System (ADS)

Showalter, Mark R.; de Pater, Imke; Lissauer, Jack J.; French, Robert S.

2017-06-01

We report results derived from observations of the Neptune system using the Hubble Space Telescope (HST) during August 2016. These observations entail repeated, extremely long exposures through the broadest available filter on the WFC3/UVIS instrument to reveal details of Neptune's faint rings and small, inner moons. The work complements similar observations performed by HST in 2004-2005 and 2009. A principal goal was the recovery of the small moon S/2004 N 1 (henceforth N14), which was first reported in 2009. New images show the moon clearly and make it possible to obtain accurate orbital elements for the first time. A complete analysis of all data 2004-2016 reveals that the mean motion n = 378.90616 +/- 0.00003 degrees per day, corresponding to a semimajor axis a = 105,283 km. Eccentricity and inclination are quite small, with e < 0.001 and i < 0.1 degrees. (This result accounts for the local Laplace Plane tilt of ~ 0.4 degrees). N14 has a physical radius R = 13-15 km, assuming its albedo is 0.09 +/- 0.01, which is the range of Neptune's other inner moons. It orbits interior to the much larger moon Proteus (a = 117,647 km; R = 210 km). Tides are believed to have caused Proteus to spiral outward significantly since its origin, and we find that N14 orbits within the radial zone likely crossed by Proteus. We suggest that N14 may have originated as debris ejected from an impact into Proteus; Proteus subsequently continued to evolve outward but the debris accreted into N14 and remains at its original point of origin. Naiad, the innermost of Neptune's moons, is now orbiting ~ 120 degrees ahead of its published orbital elements. This represents only a 1-sigma correction from its mean motion as derived from Voyager data, but it indicates that later, purported detections of Naiad with the Keck telescope were almost certainly misidentifications. The arcs in the Adams ring show that trends reported previously have continued: the two leading arcs are no longer visible, but the trailing two persist and have been relatively stable. Their mean motion is 820.1119 +/- 0.0003 degrees/day. This value has sufficient precision to rule out any of the previously proposed resonant confinement mechanisms.

Leveraging the power of a planet population: Mass-radius relation, host star multiplicity, and composition distribution of Kepler's sub-Neptunes

NASA Astrophysics Data System (ADS)

Wolfgang, Angie K.

With the advent of large, dedicated planet hunting surveys, the search for extrasolar planets has evolved into an effort to understand the properties and formation of a planet population whose characteristics continue to surprise the provincial perspective we've derived from our own Solar System. The Kepler Mission in particular has enabled a large number of these studies, as it was designed to stare simultaneously at thousands of stars for several years and its automated transit search pipeline enables fairly uniform detection criteria and characterizable completeness and false positive rates. With the detection of nearly 5000 planet candidates, 80% of which are smaller than 4 REarth, Kepler has especially illuminated the unexpectedly vast sub-Neptune population. Such a rich dataset provides an unprecedented opportunity for rigorous statistical study of the physics of these planets that have no analogs in our Solar System. Contributing to this endeavor, I present the statistical characterization of several aspects of this population, including the comparison between Kepler's planet candidates and low-mass occurrence rates inferred from radial velocity detections, the relationship between a sub-Neptune's mass and its radius, the frequency of Kepler planet candidate host stars which have nearby visual companions as revealed by follow-up high resolution imaging, and the distribution of gaseous mass fractions that these sub-Neptunes could possess given a rock-plus-hydrogen composition. To do so, I have used sophisticated statistical analyses such as Monte Carlo simulations and hierarchical Bayesian modeling to tie theory more closely to observations and have acquired near infrared laser guide star adaptive optics imaging of 196 Kepler Objects of Interest. I find that even within this sub-Neptune population these planets are very diverse in nature: there is intrinsic scatter in masses at a given radius, the planet host stars have visual companions at a wide range of separations, and the composition distribution spans two orders of magnitude, with a peak at 1% hydrogen and helium by mass. There is much work to be done to explain this diversity quantitatively, and especially to tie these results to various planet formation scenarios; I have no doubt that many more surprises await us.

Bright features in Neptune on 2013-2015 from ground-based observations with small (40 cm) and large telescopes (10 m)

NASA Astrophysics Data System (ADS)

Hueso, Ricardo; Delcroix, Marc; Baranec, Christoph; Sánchez-Lavega, Agustín; María Gómez-Forrellad, Josep; Félix Rojas, Jose; Luszcz-Cook, Statia; de Pater, Imke; de Kleer, Katherine; Colas, François; Guarro, Joan; Goczynski, Peter; Jones, Paul; Kivits, Willem; Maxson, Paul; Phillips, Michael; Sussenbach, John; Wesley, Anthony; Hammel, Heidi B.; Pérez-Hoyos, Santiago; Mendikoa, Iñigo; Riddle, Reed; Law, Nicholas M.; Sayanagi, Kunio

2015-11-01

Observations of Neptune over the last few years obtained with small telescopes (30-50 cm) have resulted in several detections of bright features on the planet. In 2013, 2014 and 2015, different observers have repeatedly observed features of high contrast at Neptune’s mid-latitudes using long-pass red filters. This success at observing Neptune clouds with such small telescopes is due to the presence of strong methane absorption bands in Neptune’s spectra at red and near infrared wavelengths; these bands provide good contrast for elevated cloud structures. In each case, the atmospheric features identified in the images survived at least a few weeks, but were essentially much more variable and apparently shorter-lived, than the large convective system recently reported on Uranus [de Pater et al. 2015]. The latest and brightest spot on Neptune was first detected on July 13th 2015 with the 2.2m telescope at Calar Alto observatory with the PlanetCam UPV/EHU instrument. The range of wavelengths covered by PlanetCam (from 350 nm to the H band including narrow-band and wide-band filters in and out of methane bands) allows the study of the vertical cloud structure of this bright spot. In particular, the spot is particularly well contrasted at the H band where it accounted to a 40% of the total planet brightness. Observations obtained with small telescopes a few days later provide a good comparison that can be used to scale similar structures in 2013 and 2014 that were observed with 30-50 cm telescopes and the Robo-AO instrument at Palomar observatory. Further high-resolution observations of the 2015 event were obtained in July 25th with the NIRC2 camera in the Keck 2 10-m telescope. These images show the bright spot as a compact bright feature in H band with a longitudinal size of 8,300 km and a latitudinal extension of 5,300 km, well separated from a nearby bright band. The ensemble of observations locate the structure at -41º latitude drifting at about +24.27º/day or -92.3 m/s consistently with the zonal winds. This work demonstrates excellent opportunities for pro-am collaboration in the study of Neptune and the value of nearly continuous monitoring of the planet by a broad network of amateur collaborators.

Progress on the NEPTUNE Canada Seismograph Network

NASA Astrophysics Data System (ADS)

Rogers, G. C.; Meldrum, R. D.; Heesemann, M.; Mulder, T. L.; Brillon, C. D.; Cassidy, J. F.

2012-12-01

NEPTUNE Canada is the world's first deep-sea regional multi-disciplinary scientific cabled ocean observatory. In the fall of 2007 an 800 kilometer ring of powered fiber optic cable was laid on the seafloor over the northern part of the Juan de Fuca plate and connected to a shore facility near Port Alberni on Vancouver Island. In September 2009, three broadband OBS packages were deployed in the form of a large triangle with apexes at mid plate near ODP 1027 (water depth of 2654m) and two sites on the continental slope, near ODP 889 (1256m) and Barkley Canyon (396m). The broadband systems comprise a broadband seismometer and strong motion accelerometer in a spherical titanium case surficially buried in a caisson backfilled with glass beads. Noise levels observed are as expected with the spectra being similar to, or quieter than, coastal seismograph stations in approximately the 10 to 20 second period range. The OBS's have higher noise levels at longer periods where ocean swells and the resultant infragravity waves dominate the noise spectra, and in the 1-10 Hz bandwidth typically used for locating local earthquakes. The shallowest site at Barkley Canyon has the highest noise levels. A small array, about 6 km in maximum dimension, is under construction on the Endeavour segment of the Juan de Fuca Ridge to record earthquake activity in the vicinity of the many NEPTUNE Canada multi-disciplinary ridge experiments. Two short period instruments were installed there in 2010. A broadband instrument and two additional short period instruments are planned to complete the initial ridge array. Even though the NEPTUNE Canada seismograph network is not yet complete, measured by the use of its data, it is a success already. The data are routinely used along with data from land seismographs of the Canadian National Seismograph Network for locating earthquakes in the region. However, the smallest seismic arrivals picked on the land stations cannot be routinely picked on the OBS instruments due to the higher noise levels. Real-time data are also ingested by NOAA tsunami warning centers and researchers have accessed archived data to do such diverse things as track baleen whales, carry out receiver function analyses, and study microseismic noise. NEPTUNE Canada seismic data is freely available from IRIS.

Serum creatinine detection by a conducting-polymer-based electrochemical sensor to identify allograft dysfunction.

PubMed

Wei, Fang; Cheng, Scott; Korin, Yael; Reed, Elaine F; Gjertson, David; Ho, Chih-ming; Gritsch, H Albin; Veale, Jeffrey

2012-09-18

Kidney transplant recipients who have abnormally high creatinine levels in their blood often have allograft dysfunction secondary to rejection. Creatinine has become the preferred marker for renal dysfunction and is readily available in hospital clinical settings. We developed a rapid and accurate polymer-based electrochemical point-of-care (POC) assay for creatinine detection from whole blood to identify allograft dysfunction. The creatinine concentrations of 19 blood samples from transplant recipients were measured directly from clinical serum samples by the conducting polymer-based electrochemical (EC) sensor arrays. These measurements were compared to the traditional clinical laboratory assay. The time required for detection was <5 min from sample loading. Sensitivity of the detection was found to be 0.46 mg/dL of creatinine with only 40 μL sample in the creatinine concentration range of 0 mg/dL to 11.33 mg/dL. Signal levels that were detected electrochemically correlated closely with the creatinine blood concentration detected by the UCLA Ronald Reagan Medical Center traditional clinical laboratory assay (correlation coefficient = 0.94). This work is encouraging for the development of a rapid and accurate POC device for measuring creatinine levels in whole blood.

Electrostatic solitary waves generated by beam injection in LAPD

NASA Astrophysics Data System (ADS)

Chen, L.; Gekelman, W. N.; Lefebvre, B.; Kintner, P. M.; Pickett, J. S.; Pribyl, P.; Vincena, S. T.

2011-12-01

Spacecraft data have revealed that electrostatic solitary waves are ubiquitous in non-equilibrium collisionless space plasmas. These solitary waves are often the main constituents of the observed electrostatic turbulence. The ubiquitous presence of these solitary waves in space motivated laboratory studies on their generation and evolution in the Large Plasma Device (LAPD) at UCLA. In order to observe these structures, microprobes with scale sizes of order of the Debye length (30 microns) had to be built using Mems technology. A suprathermal electron beam was injected into the afterglow plasma, and solitary waves as well as nonlinear wave packets were measured. The solitary waves are interpreted as BGK electron holes based on their width, amplitude, and velocity characteristics. The ensuing turbulence, including the solitary waves and wave packets, exhibits a band dispersion relation with its central line consistent with the electrostatic whistler mode. One surprise brought by the laboratory experiments is that the electron holes were not generated through resonant two-stream instabilities, but likely through an instability due to parallel currents. The characteristics of the LAPD electron holes and those observed in space will be compared to motivate further theoretical, simulation, and experimental work.

Carbon in the outer solar system

NASA Technical Reports Server (NTRS)

Simonelli, D. P.; Pollack, J. B.; Mckay, C. P.

1990-01-01

The satellites of Uranus, with densities between 1.3 and 1.7 g cm(-3) (from Voyager 2 observations) and the Pluto-Charon system, with a mean density of just above 1.8 g cm(-3) (from terrestrial observations of mutual eclipse events), are too dense to have a significant amount of methane ice in their interiors. However, the observed densities do not preclude contributions from such organic materials as the acid-insoluble residue in carbonaceous chondrites and laboratory-produced tholins, which have densities on the order of approximately 1.5 g cm(-3). These and other considerations have led researchers to investigate the carbon mass budget in the outer solar system, with an emphasis on understanding the contribution of organic materials. Modeling of the interiors of Pluto and Charon (being carried out by R. Reynolds and A. Summers of NASA/Ames), assuming rock and water ice as the only constituents, suggests a silicate mass fraction for this system on the order of 0.65 to 0.70. The present work includes the most recent estimates of the C/H enhancements and high z/low z ratios of the giant planets (Pollack and Bodenheimer, 1987), and involves a more careful estimation of the high z/low z mass ratio expected from solar abundances than was used in Pollack et al. (1986), including the influence of the fraction of C in CO on the amount of condensed water ice. These calculations indicate that for a particular fraction of C in CO and a given fraction of C-bearing planetesimals that dissolve in the envelope (most likely in the range 0.50 to 0.75), (1) Jupiter and Saturn require a larger fraction of C in condensed materials than Uranus and Neptune, but (2) the Jupiter and Saturn results are much less strongly constrained by the error bars on the observed C/H enhancements and high z/low z ratios than is the case for Uranus and Neptune. The clearest result is that in the region of the solar nebula near Uranus and Neptune, the minority of carbon that is not in gaseous CO (1) must include a nonzero amount of condensed material, but (2) is most likely not condensed material alone, i.e., there must be a third carbon-bearing component besides condensed material and gaseous CO. Given the implied dearth of methane ice, the condensed carbon is likely dominated by organic material, and the third component present in addition to CO and organics is assumed to be CH4 gas.

Final Technical Report for DOE Award SC0006616

DOE Office of Scientific and Technical Information (OSTI.GOV)

Robertson, Andrew

2015-08-01

This report summarizes research carried out by the project "Collaborative Research, Type 1: Decadal Prediction and Stochastic Simulation of Hydroclimate Over Monsoonal Asia. This collaborative project brought together climate dynamicists (UCLA, IRI), dendroclimatologists (LDEO Tree Ring Laboratory), computer scientists (UCI), and hydrologists (Columbia Water Center, CWC), together with applied scientists in climate risk management (IRI) to create new scientific approaches to quantify and exploit the role of climate variability and change in the growing water crisis across southern and eastern Asia. This project developed new tree-ring based streamflow reconstructions for rivers in monsoonal Asia; improved understanding of hydrologic spatio-temporal modesmore » of variability over monsoonal Asia on interannual-to-centennial time scales; assessed decadal predictability of hydrologic spatio-temporal modes; developed stochastic simulation tools for creating downscaled future climate scenarios based on historical/proxy data and GCM climate change; and developed stochastic reservoir simulation and optimization for scheduling hydropower, irrigation and navigation releases.« less

Towards Development of Robotic Aid for Rehabilitation of Locomotion-Impaired Subjects

NASA Technical Reports Server (NTRS)

Bejczy, Antal K.

2000-01-01

Manual assistance of therapists to help movement of legs of spinal cord injured (SCI) subjects during stepping on a treadmill for locomotion rehabilitation has severe economic and technical limitations. Scientists at the Department of Physiological Science at the University of California Los Angeles (UCLA) and roboticists at the Jet Propulsion Laboratory (JPL) initiated a joint effort to develop a robotic mechanism capable of performing controlled motions equivalent to the arm and hand motions of therapists assisting the stepping of locomotion impaired subjects on a treadmill, while the subjects' body weight is partially supported by an overhead harness. A first necessary technical step towards this development is to measure and understand the kinematics and dynamics of the therapists' arm and hand motions as they are reflected on the subjects' leg movement. This paper describes an initial measurement system developed for this purpose together with the related measurement results, and outlines the planned future technical work.

Strategy for exploration of the outer planets: 1986-1996

NASA Technical Reports Server (NTRS)

1986-01-01

Over the past decade COMPLEX has published three strategy reports which, taken together, encompass the entire planetary system and recommend a coherent program of planetary exploration. The highest priority for outer planet exploration during the next decade is intensive study of Saturn (the planet, satellites, rings, and magnetosphere) as a system. The Committee additionally recommends that NASA engage in the following supporting activities: increased support of laboratory and theoretical studies; pursuit of earth-based and earth-orbital observations; commitment to continued operation of productive spacecraft; implementation of the instrument development plan as appropriate for the outer solar system; studies of deep atmospheric probes; development of penetrators or other hard landers; development of radiation-hardened spacecraft; and development of low-thrust propulsion systems. Longer-term objectives include exploration and intensive study of: the Uranus and Neptune systems; planetology of the Galilean satellites and Titan; and the inner Jovian system.

Organic Matter in the Outer Solar System

NASA Technical Reports Server (NTRS)

Cruiskshank, Dale P.; DeVincenzi, Donald L. (Technical Monitor)

2000-01-01

Many solid bodies in the outer Solar System are covered with ices of various compositions, including water, carbon dioxide, methane, nitrogen, and other molecules that are solid at the low temperatures that prevail there. These ices have all been detected by remote sensing observations made with telescopes on Earth, or more recently, spacecraft in orbit (notably Galileo at Jupiter). The data also reveal other solid materials that could be minerals or complex carbon-bearing organic molecules. A study in progress using large ground-based telescopes to acquire infrared spectroscopic data, and laboratory results on the optical properties of complex organic matter, seeks to identify the non-icy materials on several satellites of Saturn, Uranus, and Neptune. The work on the satellites of Saturn is in part preparatory to the Cassini spacecraft investigation of the Saturn system, which will begin in 2004 and extend for four years.

Precise CCD positions of Triton in 2014-2016 from the Gaia DR1

NASA Astrophysics Data System (ADS)

Wang, N.; Peng, Q. Y.; Peng, H. W.; Zhang, Q. F.

2018-04-01

755 CCD observations during the years 2014-2016 have been reduced to derive the precise positions of Triton, the first satellite of Neptune. The observations were made by the 1 m telescope at Yunnan Observatory over 15 nights during the years 2014-2016. The theoretical position of Triton was retrieved from the Jet Propulsion Laboratory Horizons system. Our results show that when the newest Gaia catalogue (Gaia DR1) is referred to the mean O-Cs (observed minus computed) residuals are about 0.042 and -0.006 arcsec, the dispersions are 0.012 and 0.012 arcsec in right ascension and declination, respectively. The dispersions are improved very significantly when the Gaia DR1 is referred to. However, the agreement in right ascension is not so good as that in declination, the reason might come from the uncertainty of planet ephemeris. More observations are needed to confirm this.

Low-Temperature Hydrocarbon Photochemistry: CH3 + CH3 Recombination in Giant Planet Atmospheres

NASA Technical Reports Server (NTRS)

Smith, Gregory P.; Huestis, David L.

2002-01-01

Planetary emissions of the methyl radical CH3 were observed for the first time in 1998 on Saturn and Neptune by the ISO (Infrared Space Observatory) mission satellite. CH3 is produced by VUV photolysis of CH4 and is the key photochemical intermediate leading complex organic molecules on the giant planets and moons. The CH3 emissions from Saturn were unexpectedly weak. A suggested remedy is to increase the rate of the recombination reaction CH3 + CH3 + H2 --> C2H6 + H2 at 140 K to a value at least 10 times that measured at room temperature in rare gases, but within the range of disagreeing theoretical expressions at low temperature. We are performing laboratory experiments at low temperature and very low pressure. The experiments are supported by RRKM theoretical modeling that is calibrated using the extensive combustion literature.

DSN 70-meter antenna X-band gain, phase, and pointing performance, with particular application for Voyager 2 Neptune encounter

NASA Technical Reports Server (NTRS)

Slobin, S. D.; Bathker, D. A.

1988-01-01

The gain, phase, and pointing performance of the Deep Space Network (DSN) 70 m antennas are investigated using theoretical antenna analysis computer programs that consider the gravity induced deformation of the antenna surface and quadripod structure. The microwave effects are calculated for normal subreflector focusing motion and for special fixed-subreflector conditions that may be used during the Voyager 2 Neptune encounter. The frequency stability effects of stepwise lateral and axial subreflector motions are also described. Comparisons with recently measured antenna efficiency and subreflector motion tests are presented. A modification to the existing 70 m antenna pointing squint correction constant is proposed.

Quasar Host Galaxies/Neptune Rotation/Galaxy Building Blocks/Hubble Deep Field/Saturn Storm

NASA Technical Reports Server (NTRS)

2001-01-01

Computerized animations simulate a quasar erupting in the core of a normal spiral galaxy, the collision of two interacting galaxies, and the evolution of the universe. Hubble Space Telescope (HST) images show six quasars' host galaxies (including spirals, ellipticals, and colliding galaxies) and six clumps of galaxies approximately 11 billion light years away. A false color time lapse movie of Neptune displays the planet's 16-hour rotation, and the evolution of a storm on Saturn is seen though a video of the planet's rotation. A zoom sequence starts with a ground-based image of the constellation Ursa major and ends with the Hubble Deep Field through progressively narrower and deeper views.

Model of the vertical structure of the optical parameters of the Neptune atmosphere.

NASA Astrophysics Data System (ADS)

Morozhenko, A. V.

Analyzes the wavelength dependence of the geometric albedo of Neptune's disk and estimates some parameters of the planet's atmosphere by the method based on the determination of deviations of the vertical structure of the cloud layer from the homogeneity condition. The ratio between the methane and gas scale heights is found to be about 0.4. For the upper atmosphere, components of methane, aerosol, the mean geometric radius of particles, the turbulent mixing coefficient are determined. Two solutions were found for deeper atmospheric layers. The first one suggests a rather dense cloud; in the second solution the lower cloud layer is an extension of the upper aerosol layer.

Initial source and site characterization studies for the U.C. Santa Barbara campus

DOE Office of Scientific and Technical Information (OSTI.GOV)

Archuleta, R.; Nicholson, C.; Steidl, J.

1997-12-01

The University of California Campus-Laboratory Collaboration (CLC) project is an integrated 3 year effort involving Lawrence Livermore National Laboratory (LLNL) and four UC campuses - Los Angeles (UCLA), Riverside (UCR), Santa Barbara (UCSB), and San Diego (UCSD) - plus additional collaborators at San Diego State University (SDSU), at Los Alamos National Laboratory and in industry. The primary purpose of the project is to estimate potential ground motions from large earthquakes and to predict site-specific ground motions for one critical structure on each campus. This project thus combines the disciplines of geology, seismology, geodesy, soil dynamics, and earthquake engineering into amore » fully integrated approach. Once completed, the CLC project will provide a template to evaluate other buildings at each of the four UC campuses, as well as provide a methodology for evaluating seismic hazards at other critical sites in California, including other UC locations at risk from large earthquakes. Another important objective of the CLC project is the education of students and other professional in the application of this integrated, multidisciplinary, state-of-the-art approach to the assessment of earthquake hazard. For each campus targeted by the CLC project, the seismic hazard study will consist of four phases: Phase I - Initial source and site characterization, Phase II - Drilling, logging, seismic monitoring, and laboratory dynamic soil testing, Phase III - Modeling of predicted site-specific earthquake ground motions, and Phase IV - Calculations of 3D building response. This report cover Phase I for the UCSB campus and incudes results up through March 1997.« less

Law of Large Numbers: the Theory, Applications and Technology-based Education

PubMed Central

Dinov, Ivo D.; Christou, Nicolas; Gould, Robert

2011-01-01

Modern approaches for technology-based blended education utilize a variety of recently developed novel pedagogical, computational and network resources. Such attempts employ technology to deliver integrated, dynamically-linked, interactive-content and heterogeneous learning environments, which may improve student comprehension and information retention. In this paper, we describe one such innovative effort of using technological tools to expose students in probability and statistics courses to the theory, practice and usability of the Law of Large Numbers (LLN). We base our approach on integrating pedagogical instruments with the computational libraries developed by the Statistics Online Computational Resource (www.SOCR.ucla.edu). To achieve this merger we designed a new interactive Java applet and a corresponding demonstration activity that illustrate the concept and the applications of the LLN. The LLN applet and activity have common goals – to provide graphical representation of the LLN principle, build lasting student intuition and present the common misconceptions about the law of large numbers. Both the SOCR LLN applet and activity are freely available online to the community to test, validate and extend (Applet: http://socr.ucla.edu/htmls/exp/Coin_Toss_LLN_Experiment.html, and Activity: http://wiki.stat.ucla.edu/socr/index.php/SOCR_EduMaterials_Activities_LLN). PMID:21603584

Hospitals prepare plans, drill staff to ensure that potential Ebola patients are identified, isolated, and managed safely.

PubMed

2014-12-01

Hospitals around the country have stepped up their efforts to train staff and implement procedures to ensure the safe identification and management of any patients with signs of Ebola virus disease (EVD). Ronald Reagan UCLA Medical Center in Los Angeles, CA, held an "Ebola preparedness exercise" to give staff an opportunity to walk through the hospital's protocol for handling a simulated patient with EVD. The University of Alabama at Birmingham (UAB) Medical Center has held similar exercises, and is now holding twice-weekly meetings of its leadership team to make sure that all new developments in the Ebola outbreak are communicated. UCLA Medical Center has prepared PPE kits based on the practices developed at Emory University Hospital, which has thus far had the most experience in this country in caring for patients with EVD. The UCLA Health System has adjusted its medical record system so that a red flag is placed on the electronic medical record [EMR] of any patient who has recently traveled to a high-risk area. UAB Medical Center has incorporated what had been a paper-and-pencil screening tool for EVD into its electronic medical record. Training on PPE as well as EVD screening is being provided to first-responders and 911 call center dispatchers in the UAB system.

An intensive primary-literature-based teaching program directly benefits undergraduate science majors and facilitates their transition to doctoral programs.

PubMed

Kozeracki, Carol A; Carey, Michael F; Colicelli, John; Levis-Fitzgerald, Marc; Grossel, Martha

2006-01-01

UCLA's Howard Hughes Undergraduate Research Program (HHURP), a collaboration between the College of Letters and Science and the School of Medicine, trains a group of highly motivated undergraduates through mentored research enhanced by a rigorous seminar course. The course is centered on the presentation and critical analysis of scientific journal articles as well as the students' own research. This article describes the components and objectives of the HHURP and discusses the results of three program assessments: annual student evaluations, interviews with UCLA professors who served as research advisors for HHURP scholars, and a survey of program alumni. Students indicate that the program increased their ability to read and present primary scientific research and to present their own research and enhanced their research experience at UCLA. After graduating, they find their involvement in the HHURP helped them in securing admission to the graduate program of their choice and provided them with an advantage over their peers in the interactive seminars that are the foundation of graduate education. On the basis of the assessment of the program from 1998-1999 to 2004-2005, we conclude that an intensive literature-based training program increases student confidence and scientific literacy during their undergraduate years and facilitates their transition to postgraduate study.

Mode conversion and heating in a UCLA-high schools collaborative experiment

NASA Astrophysics Data System (ADS)

Smith, Miana; Buckley-Bonnano, Samuel; Pribyl, Patrick; Gekelman, Walter; Wise, Joe; Baker, Bob; Marmie, Ken

2016-10-01

A small plasma device is in operation for use by undergraduates and high school students at UCLA. Magnetic field up to 100 G, with density 108 <=ne <=1011cm-3 and temperature Te < 3eV are available in a 50 cm diameter plasma 2 meters long. The plasma is generated by an ICP source at one end operating at about 500 kHz. For this experiment, a small plate located near the edge of the plasma column is used as an electrostatic launcher. High frequency waves ωce < ω < 3ωce are launched radially from the plate in the low-density region, with electric field perpendicular to B and to the density gradient. A Langmuir probe located some distance away axially measures plasma heating along a field line that passes several cm in front of the launcher, localized in radius with δr 1cm Absorption and strong electron heating are observed at the plasma resonant layer. We explore the ``double resonance condition at which ωpe = 2ωce . Here strong interaction with electron Bernstein waves is expected. The Bernstein waves are also launched at low power and their dispersion relation verified. Work done at the BaPSF at UCLA which is supported by the DOE/NSF.

Neptune Blue-green Atmosphere

NASA Image and Video Library

2000-02-16

Neptune's blue-green atmosphere is shown in greater detail than ever before by the Voyager 2 spacecraft as it rapidly approaches its encounter with the giant planet. This color image, produced from a distance of about 16 million kilometers, shows several complex and puzzling atmospheric features. The Great Dark Spot (GDS) seen at the center is about 13,000 km by 6,600 km in size -- as large along its longer dimension as the Earth. The bright, wispy "cirrus-type" clouds seen hovering in the vicinity of the GDS are higher in altitude than the dark material of unknown origin which defines its boundaries. A thin veil often fills part of the GDS interior, as seen on the image. The bright cloud at the southern (lower) edge of the GDS measures about 1,000 km in its north-south extent. The small, bright cloud below the GDS, dubbed the "scooter," rotates faster than the GDS, gaining about 30 degrees eastward (toward the right) in longitude every rotation. Bright streaks of cloud at the latitude of the GDS, the small clouds overlying it, and a dimly visible dark protrusion at its western end are examples of dynamic weather patterns on Neptune, which can change significantly on time scales of one rotation (about 18 hours). https://photojournal.jpl.nasa.gov/catalog/PIA02245

Whistlers in Neptune's magnetosphere: Evidence of atmospheric lightning

NASA Technical Reports Server (NTRS)

Gurnett, D. A.; Kurth, W. S.; Cairns, I. H.; Granroth, L. J.

1990-01-01

During the Voyager 2 flyby of Neptune, a series of 16 whistler-like events were detected by the plasma wave instrument near closest approach. These events were observed at radial distances from 1.30 to 1.99 R sub N and magnetic latitudes from -7 to 33 deg. The frequencies ranged from 6.1 to 12.0 kHz, and the dispersions fit the Eckersley law for lightning-generated whistlers. Lightning in the atmosphere of Neptune is the only known source of such signals. The frequency range of the whistlers (up to 12 kHz) indicates that the local electron densities are substantially higher (N sub e greater than 30 t0 100 per cu cm) than indicated by the in situ plasma measurements. The dispersion of the whistlers is very large, typically 26,000 sec Hz(exp 0.5). Based on existing plasma density models and measurements, the dispersions are too large to be accounted for by a single direct path from the lightning source to the spacecraft. Therefore, multiple bounces from one hemisphere to the other are required. The most likely propagation path probably involves a lightning source on the dayside of the planet, with repeated bounces through the dense dayside ionosphere at low L-values.

Helium-Shrouded Planets Artist Concept

NASA Image and Video Library

2015-06-11

Planets having atmospheres rich in helium may be common in our galaxy, according to a new theory based on data from NASA's Spitzer Space Telescope. These planets would be around the mass of Neptune, or lighter, and would orbit close to their stars, basking in their searing heat. According to the new theory, radiation from the stars would boil off hydrogen in the planets' atmospheres. Both hydrogen and helium are common ingredients of gas planets like these. Hydrogen is lighter than helium and thus more likely to escape. After billions of years of losing hydrogen, the planet's atmosphere would become enriched with helium. Scientists predict the planets would appear covered in white or gray clouds. This is in contrast to our own Neptune, which is blue due to the presence of methane. Methane absorbs the color red, leaving blue. Neptune is far from our sun and hasn't lost its hydrogen. The hydrogen bonds with carbon to form methane. This artist's concept depicts a proposed helium-atmosphere planet called GJ 436b, which was found by Spitzer to lack in methane -- a first clue about its lack of hydrogen. The planet orbits every 2.6 days around its star, which is cooler than our sun and thus appears more yellow-orange in color. http://photojournal.jpl.nasa.gov/catalog/PIA19344

Neptune's blue-green atmosphere

NASA Technical Reports Server (NTRS)

1989-01-01

Neptune's blue-green atmosphere is shown in greater detail than ever before by the Voyager 2 spacecraft as it rapidly approaches its encounter with the giant planet. This color image, produced from a distance of about 16 million kilometers, shows several complex and puzzling atmospheric features. The Great Dark Spot (GDS) seen at the center is about 13,000 km by 6,600 km in size -- as large along its longer dimension as the Earth. The bright, wispy 'cirrus-type' clouds seen hovering in the vicinity of the GDS are higher in altitude than the dark material of unknown origin which defines its boundaries. A thin veil often fills part of the GDS interior, as seen on the image. The bright cloud at the southern (lower) edge of the GDS measures about 1,000 km in its north-south extent. The small, bright cloud below the GDS, dubbed the 'scooter,' rotates faster than the GDS, gaining about 30 degrees eastward (toward the right) in longitude every rotation. Bright streaks of cloud at the latitude of the GDS, the small clouds overlying it, and a dimly visible dark protrusion at its western end are examples of dynamic weather patterns on Neptune, which can change significantly on time scales of one rotation (about 18 hours).

Lifting Transit Signals from the Kepler Noise Floor. I. Discovery of a Warm Neptune

NASA Astrophysics Data System (ADS)

Kunimoto, Michelle; Matthews, Jaymie M.; Rowe, Jason F.; Hoffman, Kelsey

2018-01-01

Light curves from the 4-year Kepler exoplanet hunting mission have been searched for transits by NASA’s Kepler team and others, but there are still important discoveries to be made. We have searched the light curves of 400 Kepler Objects of Interest (KOIs) to find transit signals down to signal-to-noise ratio (S/N) ∼ 6, which is under the limit of S/N ∼ 7.1 that has been commonly adopted as a strict threshold to distinguish between a transit candidate and false alarm. We detect four new and convincing planet candidates ranging in radius from near-Mercury-size to slightly larger than Neptune. We highlight the discovery of KOI-408.05 (period = 637 days; radius = 4.9 R ⊕ incident flux = 0.6 S ⊕), a planet candidate within its host star’s Habitable Zone. We dub this planet a “warm Neptune,” a likely volatile-rich world that deserves closer inspection. KOI-408.05 joins 21 other confirmed and candidate planets in the current Kepler sample with semimajor axes a > 1.4 au. These discoveries are significant as a demonstration that the S/N threshold for detection used by the Kepler project is open to debate.

Dynamo Scaling Laws for Uranus and Neptune: The Role of Convective Shell Thickness on Dipolarity

NASA Astrophysics Data System (ADS)

Stanley, Sabine; Yunsheng Tian, Bob

2017-10-01

Previous dynamo scaling law studies (Christensen and Aubert, 2006) have demonstrated that the morphology of a planet’s magnetic field is determined by the local Rossby number (Ro_l): a non-dimensional diagnostic variable that quantifies the ratio of inertial forces to Coriolis forces on the average length scale of the flow. Dynamos with Ro_l <~ 0.1 produce dipolar dominated magnetic fields whereas dynamos with Ro_l >~ 0.1 produce multipolar magnetic fields. Scaling studies have also determined the dependence of the local Rossby number on non-dimensional parameters governing the system - specifically the Ekman, Prandtl, magnetic Prandtl and flux-based Rayleigh numbers (Olson and Christensen, 2006). When these scaling laws are applied to the planets, it appears that Uranus and Neptune should have dipole-dominated fields, contrary to observations. However, those scaling laws were derived using the specific convective shell thickness of the Earth’s core. Here we investigate the role of convective shell thickness on dynamo scaling laws. We find that the local Rossby number depends exponentially on the convective shell thickness. Including this new dependence on convective shell thickness, we find that the dynamo scaling laws now predict that Uranus and Neptune reside deeply in the multipolar regime, thereby resolving the previous contradiction with observations.

ARC-1989-A89-7042

NASA Image and Video Library

1989-08-11

P-34578 BW One of two new ring arcs, or partial rings, discovered by Voyager 2, is faintly visible just outside the orbit of the Neptunian moon 1989N4.The 155-second exposure taken by the spacecraft's narrow-angle camera shows the glare of an overexposed Neptune to the right of the moon and ring arc. The two bright streaks below the moon and ring arc are stars. The ring arc is approximately 50,000 kilometers (30,000 miles) long. The second ring arc, not apparent here, is about 10,000 kilometers (6,000 miles) long and is assoiciated with moon 1989N3. The ring arc, along with 1989N4, orbits about 62,000 kilometers (38,000 miles) from the planet's cloud tops. Astronomers long suspected the existence of such an irregular ring system around Neptune. Data from repeated ground-based observations hinted at the existence of irregular strands of partial rings orbiting Neptune. Voyager's photographs of the ring arcs are the first photographic evidence that such a ring system exists. Voyager scientists said the ring arcs may be comprised of debris associated with the nearby moons, or may be the remnants of moons that have been torn apart or ground down through collisions. Close-up studies of the ring arcs by Voyager 2 will help determine their composition.

Using the Neptune project to benefit Australian aquatic animal health research.

PubMed

McNamara, M; Ernst, I; Adlard, R D

2015-06-29

Diseases of aquatic animals have had, and continue to have, a significant impact on aquatic animal health. In Australia, where fisheries and aquaculture are important industries, aquatic species have been subject to serious disease outbreaks, including pilchard herpesvirus, the cause of one of the largest wild fish kills ever recorded. At the same time, there is a consensus that Australia's parasite fauna are largely unknown, and that aquatic animal health information is difficult to access. Managing aquatic animal diseases is challenging because they may be entirely new, their hosts may be new to aquaculture, and specialist expertise and basic diagnostic tools may be lacking or absent. The Neptune project was created in response to these challenges, and it aims to increase awareness of aquatic animal diseases, improve disease management, and promote communication between aquatic animal health professionals in Australia. The project consists of an online database, a digital microscopy platform containing a whole-slide image library, a community space, and online communications technology. The database contains aquatic animal health information from published papers, government reports, and other sources, while the library contains slides of key diseases both endemic and exotic to Australia. These assets make Neptune a powerful resource for researchers, students, and biosecurity officials.

Des premiers travaux de Le Verrier à la découverte de Neptune

NASA Astrophysics Data System (ADS)

Laskar, Jacques

2017-11-01

Urbain-Jean-Joseph Le Verrier was born in Saint-Lô on March 11, 1811. He entered the "École polytechnique" in 1831, from which he was to emerge eighth of his class two years later. After first devoting himself to chemistry, in 1836 he obtained a position as an astronomy assistant at the "École polytechnique". This choice will decide his future career, which culminates with the discovery of Neptune in 1846. Le Verrier wrote more than 200 contributions to the Comptes rendus de l'Académie des sciences. These contributions are very varied: some original articles, but also reports on publications published elsewhere, sometimes even simple notes of a single page. The whole set gives a very vivid vision of the development of the science of the 19th century. At that time, the Comptes rendus are really a reflection of the debates of the sessions of the Academy. They are published very quickly, and leave a large freedom of speech to the authors. They are therefore a snapshot of the sometimes lively polemics that animated the sessions of the French Academy of Sciences. In this limited essay, we will mainly look at the first years of the career of Le Verrier until the discovery of Neptune.

Outcome of arthroscopic subscapularis tendon repair: Are the results improving with improved techniques and equipment?: A retrospective case series

PubMed Central

Arun, G R; Kumar, Pradeep; Patnaik, Sarthak; Selvaraj, Karthik; Rajan, David; Singh, Anant; Kumaraswamy, Vinay

2016-01-01

Background: Rotator cuff tears are a common cause of shoulder pain and dysfunction. More recently, there has been a renewed interest in understanding the subscapularis tears. There are multiple articles in the literature showing the short term results of isolated subscapularis tendon repair. However, the midterm and long term outcome studies for arthroscopic subscapularis repair are few. This study evaluates the functional outcome after arthroscopic subscapularis repair. Materials and Methods: The records of 35 patients who underwent an arthroscopic subscapularis repair between May 2008 and June 2012 were included in this retrospective study. The records of all patients were reviewed. There were 22 males and 13 female patients with mean age of 58.2 years (range 41-72 years). All patients had a complete history, physical examination, and radiographs of their shoulders. Visual analogue scale (VAS), range of movements, power of cuff muscles, and modified University of California at Los Angeles (UCLA) score were assessed. Results: The mean followup was 2.8 years (range 2-4 year). Functional outcome after arthroscopic subscapularis repair has an excellent outcome as analysed by clinical outcome, VAS score and UCLA score. Results were analyzed and had statistically significant values. The VAS for pain improved significantly (P < 0.001), and the mean modified UCLA score improved significantly (P < 0.001) from 14.24 ± 4.72 preoperatively to 33.15 ± 2.29 at 2 years postoperative. According to the UCLA system, there were 22 excellent, 11 good, and 2 fair results. Around 95% of patients returned to their usual work after surgery. Conclusion: At a median followup of 2 years, 95% of patients had a good to excellent result after an arthroscopic subscapularis tendon repair. We conclude that the midterm results show that arthroscopic subscapularis repair remains a good option for the treatment of patients with subscapularis tendon repair. PMID:27293291

Total ankle arthroplasty versus ankle arthrodesis. Comparison of sports, recreational activities and functional outcome.

PubMed

Schuh, Reinhard; Hofstaetter, Jochen; Krismer, Martin; Bevoni, Roberto; Windhager, Reinhard; Trnka, Hans-Joerg

2012-06-01

Ankle arthrodesis (AAD) and total ankle replacement (TAR) are the major surgical treatment options for severe ankle arthritis. There is an ongoing discussion in the orthopaedic community whether ankle arthrodesis or ankle fusion should be the treatment of choice for end stage osteoarthritis. The purpose of this study was to compare the participation in sports and recreational activities in patients who underwent either AAD or TAR for end-stage osteoarthritis of the ankle. A total of 41 patients (21 ankle arthrodesis /20 TAR) were examined at 34.5 (SD18.0) months after surgery. At follow-up, pre- and postoperative participation in sports and recreational activities has been assessed. Activity levels were determined using the ankle activity score according to Halasi et al. and the University of California at Los Angeles (UCLA) activity scale. Clinical and functional outcome was assessed using the American Orthopaedic Foot and Ankle Society (AOFAS) hindfoot score. The percentage of patients participating in sports and recreational activities, UCLA score and AOFAS score were compared between both treatment groups. In the AAD group 86% were active in sports preoperatively and in the TAR group this number was 76%. Postoperatively in both groups 76% were active in sports (AAD, p = 0.08). The UCLA score was 7.0 (± 1.9) in the AAD group and 6.8 (± 1.8) in the TAR group (p = 0.78). The AOFAS score reached 75.6 (± 14) in the AAD group and 75.6 (± 16) in the TAR group (p = 0.97). The ankle activity score decrease was statistically significant for both groups (p = 0.047). Our study revealed no significant difference between the groups concerning activity levels, participation in sports activities, UCLA and AOFAS score. After AAD the number of patients participating in sports decreased. However, this change was not statistically significant.

[Case-control study on polymer polylactic acid absorbable medical film for preventing acromion adhesion after arthroscopic rotator cuff repair].

PubMed

Lin, Wei; Xu, Huan; Xing, Hai-Lin; Zheng, Rong-Zong; Ying, Jin-He

2018-03-25

To study effect of shoulder joint function after rotator cuff repair of polylactic acid absorbable membrane. From September 2015 to December 2016, 50 patients diagnosed with rotator cuff tear were selected and divided into treatment group and control group. There were 25 patients in control group, including 12 males and 13 females, with an average age of (48.7±3.5) years old, who received simple arthroscopic rotator cuff repair. There were 25 patients in treatment group, including 11 males and 14 females, with an average age of(49.2±4.1) years old, who performed arthroscopic rotator cuff repair with implanting polylactic acid absorbable membraneon shoulder of rotator cuff. Preoperative and postoperative VAS score, ASES score and UCLA score were recorded and compared between two groups. At 6 months after operation, preoperative VAS score in control group was 5.48±1.12, and decreased as 1.28±0.84 after operation; ASES score before operation was 52.24±4.64, and improved to 86.92±3.20 after operation;preoperative UCLA score improved from 14.36±1.89 before operation to 30.72±1.28 after operation. In treatment group, VAS score decreased from 5.36±1.32 before operation to 1.40±0.71 after operation;preoperative ASES score was 51.04±4.09, and improved to 88.96±2.79 after operation; UCLA score improved from 15.12±1.81 before operation to 32.12±1.33 after operation. There was no significant difference in VAS score between two groups, and ASES score, UCLA score in treatment group was obviously better than control group. Application of polylactic acid absorbable medical membrane could obviously improve shoulder function, and effectively prevent acromion adhesion after arthroscopic rotator cuff repair. Copyright© 2018 by the China Journal of Orthopaedics and Traumatology Press.

Use of plate fixation without coracoclavicular ligament augmentation for unstable distal clavicle fractures.

PubMed

Shin, Sang-Jin; Ko, Young-Won; Lee, Juyeob; Park, Min-Gyue

2016-06-01

The purpose of this study was to evaluate the clinical and radiologic outcomes of unstable distal clavicle fractures treated with anatomic plate fixation without coracoclavicular ligament augmentation and to compare the outcome of Neer type IIA with that of type IIB. Twenty-five patients with unstable distal clavicle fractures who underwent anatomic plate fixation without coracoclavicular ligament augmentation were enrolled prospectively, including 9 patients of Neer type IIA and 16 patients of Neer type IIB. Clinical outcomes were evaluated using Constant and University of California-Los Angeles (UCLA) scores. Coracoclavicular distance was measured on plain radiographs. Bone union was achieved in all patients. Satisfactory clinical and radiologic outcomes were obtained regardless of fracture type. After operation, the mean coracoclavicular distance on the injured side was increased by 10% compared with the uninjured side. However, between the patients who showed an increased coracoclavicular distance >10% (Constant score, 89.4 ± 3.7; UCLA score, 32.6 ± 3) and the patients with increased coracoclavicular distance <10% of the uninjured side (Constant score, 88.7 ± 3.6; UCLA score, 31.9 ± 3), there was no statistically significant difference in clinical outcomes of Constant score (P = .934) and UCLA score (P = .598). In unstable distal clavicle fractures, precontoured anatomic plate fixation without coracoclavicular ligament augmentation showed satisfactory clinical outcomes and high union rates even with a small lateral fragment. Patients who had increased coracoclavicular distance also demonstrated satisfactory shoulder functional outcomes regardless of the fracture type. Therefore, anatomic plate fixation without additional coracoclavicular ligament augmentation can be considered one of the treatment options for unstable distal clavicle fracture. Level IV; Case Series; Treatment Study. Copyright © 2016 Journal of Shoulder and Elbow Surgery Board of Trustees. Published by Elsevier Inc. All rights reserved.

OceanGLOBE: an Outdoor Research and Environmental Education Program for K-12 Students

NASA Astrophysics Data System (ADS)

Perry, R. B.; Hamner, W. M.

2006-12-01

OceanGLOBE is an outdoor environmental research and education program for upper elementary, middle and high school students, supplemented by online instructional materials that are available without charge to any educator. OceanGLOBE was piloted in 1995 with support from a National Science Foundation Teacher Enhancement project, "Leadership in Marine Science" (award no.ESI-9454413 to UCLA). Continuing support by a second NSF Teacher Enhancement project (award no. ESI-9819424 to UCLA) and by COSEE-West (NSF awards OCE-215506 to UCLA and OCE-0215497 to USC) has enabled OceanGLOBE to expand to a growing number of schools and to provide an increasingly robust collection of marine science instructional materials on its website, http://www.msc.ucla.edu/oceanglobe/ OceanGLOBE provides a mechanism for students to conduct inquiry-based, hands-on marine science research, providing experiences that anchor the national and state science content standards learned in the classroom. Students regularly collect environmental and biological data from a beach site over an extended period of time. In the classroom they organize, graph and analyze their data, which can lead to a variety of student-created science products. Beach research is supported by instructional marine science materials on the OceanGLOBE website. These online materials also can be used in the classroom independent of the field component. Annotated PowerPoint slide shows explain research protocols and provide marine science content. Field guides and photographs of marine organisms (with emphasis on the Southern California Bight) and a growing collection of classroom investigations (applicable to any ocean location) support the science content presented in the beach research program and slide shows. In summary, OceanGLOBE is a comprehensive learning package grounded in hands-on, outdoor marine science research project in which students are the principal investigators. By doing scientific work repetitively over an extended time period students learn about how science is done as much as they learn science content.

Photochemistry in terrestrial exoplanet atmospheres. III. Photochemistry and thermochemistry in thick atmospheres on super Earths and mini Neptunes

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hu, Renyu; Seager, Sara, E-mail: hury@caltech.edu

Some super Earths and mini Neptunes will likely have thick atmospheres that are not H{sub 2}-dominated. We have developed a photochemistry-thermochemistry kinetic-transport model for exploring the compositions of thick atmospheres on super Earths and mini Neptunes, applicable for both H{sub 2}-dominated atmospheres and non-H{sub 2}-dominated atmospheres. Using this model to study thick atmospheres for wide ranges of temperatures and elemental abundances, we classify them into hydrogen-rich atmospheres, water-rich atmospheres, oxygen-rich atmospheres, and hydrocarbon-rich atmospheres. We find that carbon has to be in the form of CO{sub 2} rather than CH{sub 4} or CO in a H{sub 2}-depleted water-dominated thick atmospheremore » and that the preferred loss of light elements from an oxygen-poor carbon-rich atmosphere leads to the formation of unsaturated hydrocarbons (C{sub 2}H{sub 2} and C{sub 2}H{sub 4}). We apply our self-consistent atmosphere models to compute spectra and diagnostic features for known transiting low-mass exoplanets GJ 1214 b, HD 97658 b, and 55 Cnc e. For GJ 1214 b, we find that (1) C{sub 2}H{sub 2} features at 1.0 and 1.5 μm in transmission and C{sub 2}H{sub 2} and C{sub 2}H{sub 4} features at 9-14 μm in thermal emission are diagnostic for hydrocarbon-rich atmospheres; (2) a detection of water-vapor features and a confirmation of the nonexistence of methane features would provide sufficient evidence for a water-dominated atmosphere. In general, our simulations show that chemical stability has to be taken into account when interpreting the spectrum of a super Earth/mini Neptune. Water-dominated atmospheres only exist for carbon to oxygen ratios much lower than the solar ratio, suggesting that this kind of atmospheres could be rare.« less

Geographic Distribution of N2, CH4, CO2, and H2O Ices on Triton from Near-IR Spectroscopic Monitoring

NASA Astrophysics Data System (ADS)

Grundy, W. M.; Young, L. A.; Young, E. F.; Buie, M. W.; Spencer, J. R.

2004-11-01

We present new 0.8 to 2.4 μ m spectral observations of Neptune's satellite Triton, obtained at IRTF\\slash SpeX between 2001 and 2004 as part of an ongoing search for time-variable phenomena associated with Triton's seasonal volatile transport processes, and also perhaps with reported shorter-term "reddening" events. The ability to detect spectral changes on these time scales depends critically on accurate characterization of any cyclic variations resulting from Triton's 5.877 day rotation period. We will report on our observations of periodic variations of Triton's near-IR absorption bands of N2, CH4, and H2O ices, but not of CO2 ice, in this initial stage of our Triton monitoring program. The observed variations (or lack thereof) give an indication of how these four ice species are distributed in longitude. The most heterogeneously distributed ice is N2, which shows nearly twice as much absorption on Triton's Neptune-facing hemisphere as on the anti-Neptune hemisphere. Comparison with Voyager-era, visual wavelength imaging of Triton's surface suggest that the observed N2 ice is concentrated on low-latitude regions of Triton's polar cap, which are predominantly located on the Neptune-facing hemisphere. Non-volatile H2O ice seems to be slightly concentrated on Triton's leading hemisphere. Despite being highly diluted in N2 ice, the longitudinal distribution of Triton's CH4 ice differs from that of Triton's N2 ice, being slightly concentrated on Triton's trailing hemisphere. Triton's CO2 ice shows the least longitudinal variation, suggesting that it is either very uniformly distributed or that it is confined to high latitudes. This work was supported by NASA's Planetary Astronomy and Planetary Geology &\\ Geophysics programs, and by NSF's Planetary Astronomy program. \\hangindent=0.3truein Grundy, W.M., and L.A. Young (2004) Near infrared spectral monitoring of Triton with IRTF\\slash SpeX I: Establishing a baseline. Icarus (in press).

Neptune's New Dark Vortex: Imaging with HST/WFC3

NASA Astrophysics Data System (ADS)

Wong, M. H.; Tollefson, J.; De Pater, I.; de Kleer, K.; Hammel, H. B.; Luszcz-Cook, S.; Hueso, R.; Sanchez-Lavega, A.; Simon, A. A.; Delcroix, M.; Sromovsky, L. A.; Fry, P. M.; Orton, G. S.; Baranec, C.

2016-12-01

A bright, unusually long-lived outburst of cloud activity on Neptune was observed in 2015 (Hueso et al. 2015, DPS 400.02). This led to speculation about whether the clouds were convective in nature, or bright companions to an unseen dark vortex (similar to the Great Dark Spot studied in detail by Voyager 2: Smith et al. 1989, Science 246, 1422). HST OPAL images at blue wavelengths finally answered this question by discovering a new dark vortex at 45 deg S. We call this feature SDS-2015, for "southern dark spot discovered in 2015" (Wong et al. 2016, CBET 4278). Dark vortices on Neptune are rare; SDS-2015 is only the fifth ever seen. All five were diverse in terms of size and shape, the distribution of bright companion clouds, and horizontal motions (oscillations and drifts). The drift of these vortices is highly sensitive to horizontal and vertical wind shear, making them valuable probes into the structure of Neptune's atmospheric jets. We will present imaging observations of SDS-2015 obtained with the WFC3/UVIS camera on the Hubble Space Telescope, covering the discovery of the vortex in September 2015 and follow-up observations in May 2016. No significant latitudinal drift was seen over this time span. We will compare size estimates, which are complicated by the continual presence of companion clouds, and by the low contrast between the vortex and its surroundings. The 2015 observations included 7 filters spanning 467-845 nm, weighted toward longer wavelengths to study general cloud motions and vertical distributions. The 2016 observations included 7 filters spanning 336-763 nm, weighted toward shorter wavelengths where the dark spot itself can be detected. A companion abstract (Tollefson et al., this meeting) will present results from radiative transfer modeling of the multispectral data. [This conference abstract is based on observations made with the NASA/ESA Hubble Space Telescope, associated with programs GO-13937 ("OPAL") and GO-14492.

The Education and Public Outreach Plan for UCLA's Institute for Planets and Exoplanets (iPLEX)

NASA Astrophysics Data System (ADS)

Glesener, G. B.; Jewitt, D. C.; Curren, I. S.

2012-12-01

Increasing the number and diversity of students pursuing and completing STEM education is a crucial part of UCLA's Institute for Planets and Exoplanets (iPLEX)'s goal of promoting research on planetary systems around the sun and other stars. Cultivating students' interest and success in STEM subject areas from K-12 to the bachelor's degree is an important factor in student retention. As they pursue a bachelor's degree in a STEM major, many become discouraged and decide not to finish with this type of degree; women, underrepresented minorities (URM), and students of low socioeconomic status (SES) have the highest attrition rates (Bayer 2010). Focusing primarily on students at the high school and community college levels, our education and public outreach plan utilizes the multidisciplinary science of astrobiology as a resource for building stronger learning environments in STEM education. By implementing formal education programs that encourage and foster student learning in STEM fields, we intend to (1) increase the efficiency with which students move from high school into STEM-related undergraduate programs, (2) improve the corresponding transfer rate from community colleges to advanced degree programs in STEM at the 4-year university level, and (3) create more opportunities for students to become involved in meaningful research as they progress in their studies. To ensure the success of these programs, we will partner with teachers from local high schools and community colleges, and UCLA's Center X. By being geographically located in Los Angeles County, having one of the highest URM populations in the United States (US Census Bureau, 2007), and partnering with Hampton University (HU) in Virginia, whose student body is 91% African American, we are in a position to make a large impact on diversity. To further ensure the success of our EPO, an independent evaluator will measure and track the following program objectives: increase (1) post-secondary STEM enrollment; (2) community college student transfer rates into four-year universities as STEM majors; (3) science knowledge and effective pedagogical practices for high school and community college teachers; and (4) collaboration between UCLA astrobiology scientists, high school teachers, and community college instructors. Building stronger learning environments for STEM students should result in higher retention rates through the various academic transitions toward the bachelor's, increasing the probability of graduation. Educating the community informally is also important for cultivating students' interest and success in STEM education. In the informal education part of our EPO plan, we will partner with Astronomy Without Borders (AWB) to disseminate planetary and astronomical results to the public, contribute to a series of public astrobiology talks at The Los Angeles County Museum of Natural History, and participate in the Exploring Your Universe / UCLA Science Day event held every year to bring science to the community. Helping young learners achieve success in STEM education through EPO programs that afford meaningful STEM experiences is the ultimate goal of UCLA's iPLEX EPO plan. We hope to make a significant impact on our community and build upon the efforts of our colleagues in STEM education to increase the retention of students pursuing degrees in STEM fields.

The psychometric properties of the Brief Fear of Negative Evaluation Scale.

PubMed

Duke, Danny; Krishnan, Mohan; Faith, Melissa; Storch, Eric A

2006-01-01

This study examined the psychometric properties of the Brief Fear of Negative Evaluation (BFNE) Scale in a nonclinical, nonstudent sample. Participants were administered the BFNE Scale, Beck Depression Inventory (BDI), and the UCLA Loneliness Scale. No differences were found across age, but women scored significantly higher on the BFNE Scale than men. Confirmatory factor analysis supported a two-factor solution corresponding to positive and reverse scored items. Internal consistency was excellent for the positive scored factor (alpha=.94), acceptable for the reverse scored factor (alpha=.73), and good for the full BFNE Scale (alpha=.80). BFNE scores were significantly correlated in the expected directions with the BDI and the UCLA Loneliness Scale. Implications of these findings for clinical practice and future research are discussed.

Evolution of the Uranus-neptune Planetesimal Swarm: Consequences for the Earth

NASA Technical Reports Server (NTRS)

Shoemaker, E. M.; Wolfe, R. F.

1984-01-01

The evolution of planetesimals in the outer Solar System were evaluated, both stellar and planetary encounters. About 20% of the Uranus-Neptune planetesimals (UNP's) enter the comet cloud and are stored primarily in the region inside the observational limits of the Oort cloud. Half of the comets have suruived to the present time; the cloud now has a mass of the order of Jupiter's mass. Most UNP's are ejected from the Solar system, and about half of the planetesimal swarm is passed to the control of Jupiter prior to ejection. Jupiter's perturbations drive a large flux of these planetesimals into Earth-crossing orbits, and it now appears highly probable that UNP's account for most of the heavy bombardment of the Moon and Earth.

Satellite sweeping of electrons at Neptune and Uranus

NASA Technical Reports Server (NTRS)

Cooper, John F.

1990-01-01

Knowledge of satellite sweeping parameters at Neptune and Uranus, and of their functional dependences on particle energy and pitch angle, can be critical in the proper identification of parent absorbers for observed absorption signatures in regions where OTD (offset, tilted dipole) models are valid representations of the measured magnetic fields. In this paper, critical electron energies are calculated for longitudinal drift resonance, snowplow (i.e., strong) absorption, leapfrog, and corkscrew effects, using a reduced version of OTD that neglects nonaxial dipole offsets. Earlier analytic work on sweeping rates is extended to give the radial dependence of these rates within the minimum-L region and to set limits on diffusion of electrons with the simplifying approximation that leapfrog effects are ignored.

PIC simulations of the trapped electron filamentation instability in finite-width electron plasma waves

NASA Astrophysics Data System (ADS)

Winjum, B. J.; Banks, J. W.; Berger, R. L.; Cohen, B. I.; Chapman, T.; Hittinger, J. A. F.; Rozmus, W.; Strozzi, D. J.; Brunner, S.

2012-10-01

We present results on the kinetic filamentation of finite-width nonlinear electron plasma waves (EPW). Using 2D simulations with the PIC code BEPS, we excite a traveling EPW with a Gaussian transverse profile and a wavenumber k0λDe= 1/3. The transverse wavenumber spectrum broadens during transverse EPW localization for small width (but sufficiently large amplitude) waves, while the spectrum narrows to a dominant k as the initial EPW width increases to the plane-wave limit. For large EPW widths, filaments can grow and destroy the wave coherence before transverse localization destroys the wave; the filaments in turn evolve individually as self-focusing EPWs. Additionally, a transverse electric field develops that affects trapped electrons, and a beam-like distribution of untrapped electrons develops between filaments and on the sides of a localizing EPW. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and funded by the Laboratory Research and Development Program at LLNL under project tracking code 12-ERD-061. Supported also under Grants DE-FG52-09NA29552 and NSF-Phy-0904039. Simulations were performed on UCLA's Hoffman2 and NERSC's Hopper.

Quality of life and psychosocial aspects in Greek patients with psoriasis: a cross-sectional study.

PubMed

Kouris, Anargyros; Christodoulou, Christos; Stefanaki, Christina; Livaditis, Miltiadis; Tsatovidou, Revekka; Kouskoukis, Constantinos; Petridis, Athanasios; Kontochristopoulos, George

2015-01-01

Psoriasis is a common, long-term skin disease associated with high levels of psychological distress and a considerable adverse impact on life. The effects of psoriasis, beyond skin affliction, are seldom recognized and often undertreated. The aim of the study is to evaluate the quality of life, anxiety and depression, self-esteem and loneliness in patients with psoriasis. Eighty-four patients with psoriasis were enrolled in the study. The quality of life, depression and anxiety, loneliness and self-esteem of the patient were assessed using the Dermatology Life Quality Index, Hospital Anxiety and Depression Scale, the UCLA loneliness Scale (UCLA-Version 3) and Rosenberg's Self-esteem Scale, respectively. The Dermatology Quality of Life Index score among psoriasis patients was 12.61 ± 4.88. They had statistically significantly higher scores according to the Hospital Anxiety and Depression Scale -anxiety subscale (p=0.032)-compared with healthy volunteers. Moreover, a statistically significant difference was found between the two groups concerning the UCLA-scale (p=0.033) and RSES-scale (p<0.0001). Female patients presented with lower self-esteem than male patients. Psoriasis is a distressing, recurrent disorder that significantly impairs quality of life. Therefore, the recognition and future management of psoriasis may require the involvement of multi-disciplinary teams to manage the physical, psychological and social aspects of the condition, as is the case for systemic, long-term conditions.

A high-density SNP linkage scan with 142 combined subtype ADHD sib pairs identifies linkage regions on chromosomes 9 and 16.

PubMed

Asherson, P; Zhou, K; Anney, R J L; Franke, B; Buitelaar, J; Ebstein, R; Gill, M; Altink, M; Arnold, R; Boer, F; Brookes, K; Buschgens, C; Butler, L; Cambell, D; Chen, W; Christiansen, H; Feldman, L; Fleischman, K; Fliers, E; Howe-Forbes, R; Goldfarb, A; Heise, A; Gabriëls, I; Johansson, L; Lubetzki, I; Marco, R; Medad, S; Minderaa, R; Mulas, F; Müller, U; Mulligan, A; Neale, B; Rijsdijk, F; Rabin, K; Rommelse, N; Sethna, V; Sorohan, J; Uebel, H; Psychogiou, L; Weeks, A; Barrett, R; Xu, X; Banaschewski, T; Sonuga-Barke, E; Eisenberg, J; Manor, I; Miranda, A; Oades, R D; Roeyers, H; Rothenberger, A; Sergeant, J; Steinhausen, H-C; Taylor, E; Thompson, M; Faraone, S V

2008-05-01

As part of the International Multi-centre ADHD Genetics project we completed an affected sibling pair study of 142 narrowly defined Diagnostic and Statistical Manual of Mental Disorders, fourth edition combined type attention deficit hyperactivity disorder (ADHD) proband-sibling pairs. No linkage was observed on the most established ADHD-linked genomic regions of 5p and 17p. We found suggestive linkage signals on chromosomes 9 and 16, respectively, with the highest multipoint nonparametric linkage signal on chromosome 16q23 at 99 cM (log of the odds, LOD=3.1) overlapping data published from the previous UCLA (University of California, Los Angeles) (LOD>1, approximately 95 cM) and Dutch (LOD>1, approximately 100 cM) studies. The second highest peak in this study was on chromosome 9q22 at 90 cM (LOD=2.13); both the previous UCLA and German studies also found some evidence of linkage at almost the same location (UCLA LOD=1.45 at 93 cM; German LOD=0.68 at 100 cM). The overlap of these two main peaks with previous findings suggests that loci linked to ADHD may lie within these regions. Meta-analysis or reanalysis of the raw data of all the available ADHD linkage scan data may help to clarify whether these represent true linked loci.

Changes in lower urinary tract symptoms and quality of life after salvage radiotherapy for biochemical recurrence of prostate cancer.

PubMed

Miyake, Makito; Tanaka, Nobumichi; Asakawa, Isao; Tatsumi, Yoshihiro; Nakai, Yasushi; Anai, Satoshi; Torimoto, Kazumasa; Aoki, Katsuya; Yoneda, Tatsuo; Hasegawa, Masatoshi; Konishi, Noboru; Fujimoto, Kiyohide

2015-06-01

The aim of this study was to evaluate chronologic changes in lower urinary tract symptoms (LUTS), health-related (HR) quality of life (QOL), and disease-specific QOL during the first 12 months after salvage radiotherapy (SRT) for biochemical recurrence of prostate cancer in patients who underwent radical prostatectomy. In 81 patients who received SRT (70 Gy/35fr/7 weeks), International Prostate Symptom Score (IPSS), 36-Item Short Form scores, and UCLA-Prostate Cancer Index (UCLA-PCI) were recorded before, during, and immediately after SRT, and 1-12 months after the completion of SRT. The total IPSS and storage symptom-related sum were significantly increased following initiation of SRT, and returned to the baseline 6 months after SRT. For three of eight domains of HRQOL, and the physical component summary score showed transient deterioration in the period between completion of SRT and 1 month following SRT. The UCLA-PCI for urinary function/bother and bowel function/bother was affected until 1-6 months after SRT. This is the first report to concurrently evaluate detailed chronologic changes in LUTS and QOL in patients who received SRT. Knowledge of changes in LUTS and QOL outcomes associated with SRT may influence treatment recommendations and enable patients to make better-informed decisions. Copyright © 2015 Elsevier Ireland Ltd. All rights reserved.

Atmospheric Mining in the Outer Solar System: Outer Planet In-Space Bases and Moon Bases for Resource Processing

NASA Technical Reports Server (NTRS)

Palaszewski, Bryan

2017-01-01

Atmospheric mining in the outer solar system has been investigated as a means of fuel production for high energy propulsion and power. Fusion fuels such as Helium 3 (3He) and deuterium can be wrested from the atmospheres of Uranus and Neptune and either returned to Earth or used in-situ for energy production. Helium 3 and deuterium were the primary gases of interest with hydrogen being the primary propellant for nuclear thermal solid core and gas core rocket-based atmospheric flight. A series of analyses were undertaken to investigate resource capturing aspects of atmospheric mining in the outer solar system. This included the gas capturing rate, storage options, and different methods of direct use of the captured gases. While capturing 3He, large amounts of hydrogen and 4He are produced. The propulsion and transportation requirements for all of the major moons of Uranus and Neptune are presented. Analyses of orbital transfer vehicles (OTVs), landers, factories, and the issues with in-situ resource utilization (ISRU) low gravity processing factories are included. Preliminary observations are presented on near-optimal selections of moon base orbital locations, OTV power levels, and OTV and lander rendezvous points. Several artificial gravity in-space base designs and orbital sites at Uranus and Neptune and the OTV requirements to support them are also addressed.

A Neptune-sized transiting planet closely orbiting a 5–10-million-year-old star.

PubMed

David, Trevor J; Hillenbrand, Lynne A; Petigura, Erik A; Carpenter, John M; Crossfield, Ian J M; Hinkley, Sasha; Ciardi, David R; Howard, Andrew W; Isaacson, Howard T; Cody, Ann Marie; Schlieder, Joshua E; Beichman, Charles A; Barenfeld, Scott A

2016-06-30

Theories of the formation and early evolution of planetary systems postulate that planets are born in circumstellar disks, and undergo radial migration during and after dissipation of the dust and gas disk from which they formed. The precise ages of meteorites indicate that planetesimals—the building blocks of planets—are produced within the first million years of a star’s life. Fully formed planets are frequently detected on short orbital periods around mature stars. Some theories suggest that the in situ formation of planets close to their host stars is unlikely and that the existence of such planets is therefore evidence of large-scale migration. Other theories posit that planet assembly at small orbital separations may be common. Here we report a newly born, transiting planet orbiting its star with a period of 5.4 days. The planet is 50 per cent larger than Neptune, and its mass is less than 3.6 times that of Jupiter (at 99.7 per cent confidence), with a true mass likely to be similar to that of Neptune. The star is 5–10 million years old and has a tenuous dust disk extending outward from about twice the Earth–Sun separation, in addition to the fully formed planet located at less than one-twentieth of the Earth–Sun separation.

NEPTUNE’S DYNAMIC ATMOSPHERE FROM KEPLER K2 OBSERVATIONS: IMPLICATIONS FOR BROWN DWARF LIGHT CURVE ANALYSES

PubMed Central

Rowe, Jason F.; Gaulme, Patrick; Hammel, Heidi B.; Casewell, Sarah L.; Fortney, Jonathan J.; Gizis, John E.; Lissauer, Jack J.; Morales-Juberias, Raul; Orton, Glenn S.; Wong, Michael H.; Marley, Mark S.

2017-01-01

Observations of Neptune with the Kepler Space Telescope yield a 49 day light curve with 98% coverage at a 1 minute cadence. A significant signature in the light curve comes from discrete cloud features. We compare results extracted from the light curve data with contemporaneous disk-resolved imaging of Neptune from the Keck 10-m telescope at 1.65 microns and Hubble Space Telescope visible imaging acquired nine months later. This direct comparison validates the feature latitudes assigned to the K2 light curve periods based on Neptune’s zonal wind profile, and confirms observed cloud feature variability. Although Neptune’s clouds vary in location and intensity on short and long timescales, a single large discrete storm seen in Keck imaging dominates the K2 and Hubble light curves; smaller or fainter clouds likely contribute to short-term brightness variability. The K2 Neptune light curve, in conjunction with our imaging data, provides context for the interpretation of current and future brown dwarf and extrasolar planet variability measurements. In particular we suggest that the balance between large, relatively stable, atmospheric features and smaller, more transient, clouds controls the character of substellar atmospheric variability. Atmospheres dominated by a few large spots may show inherently greater light curve stability than those which exhibit a greater number of smaller features. PMID:28127087

Transformative ocean science through the VENUS and NEPTUNE Canada ocean observing systems

NASA Astrophysics Data System (ADS)

Martin Taylor, S.

2009-04-01

The health of the world's oceans and their impact on global environmental and climate change make the development of cabled observing systems vital and timely as a data source and archive of unparalleled importance for new discoveries. The VENUS and NEPTUNE Canada observatories are on the forefront of a new generation of ocean science and technology. Funding of over $100M, principally from the Governments of Canada and BC, for these two observatories supports integrated ocean systems science at a regional scale enabled by new developments in powered sub-sea cable technology and in cyber-infrastructure that streams continuous real-time data to Internet-based web platforms. VENUS is a coastal observatory supporting two instrumented arrays in the Saanich Inlet, near Victoria, and in the Strait of Georgia, off Vancouver. NEPTUNE Canada is an 800 km system on the Juan de Fuca Plate off the west coast of British Columbia, which will have five instrumented nodes in operation over the next 18 months. This paper describes the development and management of these two observatories, the principal research themes, and the applications of the research to public policy, economic development, and public education and outreach. Both observatories depend on partnerships with universities, government agencies, private sector companies, and NGOs. International collaboration is central to the development of the research programs, including partnerships with initiatives in the EU, US, Japan, Taiwan and China.

OSSOS. IV. Discovery of a Dwarf Planet Candidate in the 9:2 Resonance with Neptune

NASA Technical Reports Server (NTRS)

Bannister, Michele T.; Alexandersen, Mike; Benecchi, Susan; Chen, Ying-Tung; Delsanti, Audrey; Fraser, Wesley C.; Gladman, Brett; Granvik, Mikael; Grundy, Will M.; Guilbert-Lepoutre, Aurelie;

High Pressure and High Temperature State of Oxygen Enriched Ice

NASA Astrophysics Data System (ADS)

LI, M.; Zhang, S.; Jeanloz, R.; Militzer, B.

2016-12-01

Interior models for Uranus and Neptune include a hydrogen/helium/water outer envelope and a core of rock and metal at the center, with superionic water-rich ice proposed as comprising an intermediate layer. Here we consider an oxygen-enriched ice, such as H2O2 hydrogen peroxide (± water), that could form through chemical reaction between water-rich and underlying rocky (i.e., oxygen-rich) layers. As oxygen and its compounds (e.g., H2O, SiO2) form metallic fluids at pressures above 100-150 GPa, the problem amounts to considering oxygen alloying of semiconducting or metallic water. The density of H2O2 is 1.45 g/cc at ambient pressure and 0° C, increasing to 1.71 g/cc in the solid state at about -20° C. There are no Hugoniot data beyond 30 GPa, so we estimated Hugoniots for H2O2 with different initial densities, using both a mixing model based on Hugoniot data for H2O2 and 1/2 O2 (molar volume summation under pressure) and ab initio calculations for unreacted H2O2. The results agree with each other to pressures of about 200 GPa, and the ab initio calculations show evidence of a superionic state at temperatures as low as 500 K, much lower than for water ice. Hydrogen peroxide is expected to be liquid along planetary isentropes for Uranus and Neptune, suggesting that H2O2 may not be present as a pure compound in these planets. Instead, oxygen-enriched H2O ice may be the relevant form of water and oxygen, and might be produced in the laboratory by way of dynamic compression of H2O2 or laser-heating of statically compressed H2O + O2 and/or H2O2.

Formation of the giant planets

NASA Technical Reports Server (NTRS)

Lissauer, Jack J.

2006-01-01

The observed properties of giant planets, models of their evolution and observations of protoplanetary disks provide constraints on the formation of gas giant planets. The four largest planets in our Solar System contain considerable quantities of hydrogen and helium, which could not have condensed into solid planetesimals within the protoplanetary disk. All three (transiting) extrasolar giant planets with well determined masses and radii also must contain substantial amounts of these light gases. Jupiter and Saturn are mostly hydrogen and helium, but have larger abundances of heavier elements than does the Sun. Neptune and Uranus are primarily composed of heavier elements. HD 149026 b, which is slightly more massive than is Saturn, appears to have comparable quantities of light gases and heavy elements. HD 209458 b and TrES-1 are primarily hydrogen and helium, but may contain supersolar abundances of heavy elements. Spacecraft flybys and observations of satellite orbits provide estimates of the gravitational moments of the giant planets in our Solar System, which in turn provide information on the internal distribution of matter within Jupiter, Saturn, Uranus and Neptune. Atmospheric thermal structure and heat flow measurements constrain the interior temperatures of planets. Internal processes may cause giant planets to become more compositionally differentiated or alternatively more homogeneous; high-pressure laboratory .experiments provide data useful for modeling these processes. The preponderance of evidence supports the core nucleated gas accretion model. According to this model, giant planets begin their growth by the accumulation of small solid bodies, as do terrestrial planets. However, unlike terrestrial planets, the growing giant planet cores become massive enough that they are able to accumulate substantial amounts of gas before the protoplanetary disk dissipates. The primary questions regarding the core nucleated growth model is under what conditions planets with small cores/total heavy element abundances can accrete gaseous envelopes within the lifetimes of gaseous protoplanetary disks.

Mitchell Receives 2013 Ronald Greeley Early Career Award in Planetary Science: Citation

NASA Astrophysics Data System (ADS)

McKinnon, William B.

2014-07-01

The Greeley Early Career Award is named for pioneering planetary scientist Ronald Greeley. Ron was involved in nearly every major planetary mission from the 1970s until his death and was extraordinarily active in service to the planetary science community. Ron's greatest legacies, however, are those he mentored through the decades, and it is young scientists whose work and promise we seek to recognize. This year's Greeley award winner is Jonathan L. Mitchell, an assistant professor at the University of California, Los Angeles (UCLA). Jonathan received his Ph.D. from the University of Chicago, and after a postdoc at the Institute for Advanced Studies in Princeton, he joined the UCLA faculty, where he holds a joint appointment in Earth and space sciences and in atmospheric sciences.

The prevalence of childhood traumatic grief--a comparison of violent/sudden and expected loss.

PubMed

McClatchy, Irene Searles; Vonk, M Elizabeth; Palardy, Gregory

2009-01-01

The purpose of this study was to examine the prevalence of childhood traumatic grief (CTG) and posttraumatic stress disorder (PTSD) symptoms in parentally bereaved children and compare scores between those who had lost a parent to a sudden/violent death and those who had lost a parent to an expected death. A sample of 158 parentally bereaved children ages 7-16 completed the Extended Grief Inventory (EGI); 127 of those also completed the UCLA PTSD Index. A large number of children were experiencing CTG symptoms at moderate and severe levels. There was no significant difference in EGI or UCLA PTSD Index scores between the two types of losses. Findings are discussed in relation to trauma theory, research on parentally bereaved children and implications for practice.

UCLA's Molecular Screening Shared Resource: enhancing small molecule discovery with functional genomics and new technology.

PubMed

Damoiseaux, Robert

2014-05-01

The Molecular Screening Shared Resource (MSSR) offers a comprehensive range of leading-edge high throughput screening (HTS) services including drug discovery, chemical and functional genomics, and novel methods for nano and environmental toxicology. The MSSR is an open access environment with investigators from UCLA as well as from the entire globe. Industrial clients are equally welcome as are non-profit entities. The MSSR is a fee-for-service entity and does not retain intellectual property. In conjunction with the Center for Environmental Implications of Nanotechnology, the MSSR is unique in its dedicated and ongoing efforts towards high throughput toxicity testing of nanomaterials. In addition, the MSSR engages in technology development eliminating bottlenecks from the HTS workflow and enabling novel assays and readouts currently not available.

ARC-1989-AC89-7009

NASA Image and Video Library

1989-08-21

This picture of Neptune was produced from images taken through the ultraviolet, violet and green filters of the Voyager 2 wide-angle camera. This 'false' color image has been made to show clearly details of the cloud structure and to paint clouds located at different altitudes with different colors. Dark, deeplying clouds tend to be masked in the ultraviolet wavelength since overlying air molecules are particularly effective in scattering sunlight there which brightens the sky above them. Such areas appear dark blue in this photo. The Great Dark Spot (GDS) and the high southern latitudes have a deep bluish cast in this image, indication they are regions where visible light (but not ultraviolet light) may penetrate to a deeper layer of dark cloud or haze in Neptune's atmosphere. Conversely, the pinkish clouds may be positioned at high altitudes.

Neptune's Southern Hemisphere

NASA Technical Reports Server (NTRS)

1989-01-01

This photograph of Neptune's southern hemisphere was taken by the narrow-angle camera on NASA's Voyager 2 when the spacecraft was 4.2 million km (2.6 million miles) from the planet. The smallest features that can be seen are 38 km (24 miles) across. The almond-shaped structure at the left is a large cloud system that has been seen for several weeks. Internal details in the feature have become increasingly apparent as Voyager 2 has approached. Systems with similar shapes in Jupiter's atmosphere rotate about their centers, rolling in the local winds that increase toward the south. However, the wispy nature of the white central clouds in this Neptunian feature make confirmation of the system's rotation difficult. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.

A Compact, Multi-view Net Flux Radiometer for Future Uranus and Neptune Probes

NASA Technical Reports Server (NTRS)

Aslam, S.; Amato, M.; Atkinson, D. H.; Hewagama, T.; Jennings, D. E.; Nixon, C. A.; Mousis, O.

2017-01-01

A Net Flux Radiometer (NFR) is presented that can be included in an atmospheric structure instrument suite for future probe missions to the icy giants Uranus and Neptune. The baseline design has two spectral channels i.e., a solar channel (0.4-to-3.5 m) and a thermal channel (4-to-300 m). The NFR is capable of viewing five distinct viewing angles during the descent. Non-imaging Winston cones with band-pass filters are used for each spectral channel and to define a 5 angular acceptance. Uncooled thermopile detectors are used in each spectral channel and are read out using a custom radiation hard application specific integrated circuit (ASIC). The baseline design can easily be changed to increase the number of detector channels from two to seven.

It Takes a Village. Collaborative Outer Planet Missions

NASA Technical Reports Server (NTRS)

Rymer, A. M.; Turtle, E. P.; Hofstadter, M. D.; Simon, A. A.; Hospodarsky, G. B.

2017-01-01

A mission to one or both of our local Ice Giants (Uranus and Neptune) emerged as a high priority in the most recent Planetary Science Decadal Survey and was also specifically mentioned supportively in the Heliophysics Decadal Survey. In 2016, NASA convened a science definition team to study ice giant mission concepts in more detail. Uranus and Neptune represent the last remaining planetary type in our Solar System to have a dedicated orbiting mission. The case for a Uranus mission has been made eloquently in the Decadal Surveys. Here we summarize some of the major drivers that lead to enthusiastic support for an Ice Giant mission in general, and use the example of a Uranus Mission concept to illustrate opportunities such a mission might provide for cross-division collaboration and cost-sharing.

Experimental studies of interactions between Alfv'en waves and striated density depletions in the LAPD

NASA Astrophysics Data System (ADS)

Auerbach, D. W.; Carter, T. A.; Vincena, S.

2008-11-01

Satellite measurements in the earth's magnetosphere have associated Alfv'en frequency fluctuations with density depletions striated along the geomagnetic field. This poster presents laboratory studies in the LADP experiment at UCLA modeling this phenomena. Density depletions are pre-formed in the plasma column by selectively blocking a portion of the drive beam, and Alfv'en waves are driven in the cavity by means of an inserted antenna. Relevant experimental parameters include an ion cyclotron radius around a mm, alfven parallel wavelength several meters, electron inertial length around 6 mm, and electron thermal speeds about a third of the alfv'en speed. We report here on modifications to the wave propagation due to the density depletion. We also report on the details of the interactions between the driven wave and the secondary drift-alfv'en wave instabilities that arise on the density boundary, including wave-wave interactions and possible turbulent broadening effects on the main wave.

Laboratory band strengths of methane and their application to the atmospheres of Jupiter, Saturn, Uranus, Neptune, and Titan. II - The red region 6000-7600 A

NASA Technical Reports Server (NTRS)

Lutz, B. L.; Owen, T.; Cess, R. D.

1982-01-01

Lutz et al. (1976) have reported the first quantitative analyses of the strengths of the blue-green bands of methane which dominate the visible spectra of the outer planets. The present investigation represents an extension of the first study to include a number of bands between 6000 and 7500 A. The objective of this extension is to establish the validity of the scaled numerical curve of growth of the first study further into the saturated region and to test the apparent pressure independence of the high-overtone bands over a large pressure range. In addition, it is desired to provide a set of homogeneously determined band strengths and curves of growth over a large spectral region and over a large range of band strengths. This will make it possible to investigate feasible apparent dependences of planetary methane abundances on wavelength and band strength as a probe of the scattering processes in the planetary atmospheres.

Closure Report for Corrective Action Unit 574: Neptune, Nevada National Security Site, Nevada

DOE Office of Scientific and Technical Information (OSTI.GOV)

NSTec Environmental Restoration

Corrective Action Unit (CAU) 574 is identified in the Federal Facility Agreement and Consent Order (FFACO) as 'Neptune' and consists of the following two Corrective Action Sites (CASs), located in Area 12 of the Nevada National Security Site: (1) CAS 12-23-10, U12c.03 Crater (Neptune); and (2) CAS 12-45-01, U12e.05 Crater (Blanca). This Closure Report presents information supporting closure of CAU 574 according to the FFACO (FFACO, 1996 [as amended March 2010]) and the Streamlined Approach for Environmental Restoration Plan for CAU 574 (U.S. Department of Energy, National Nuclear Security Administration Nevada Site Office [NNSA/NSO], 2011). The following activities were performedmore » to support closure of CAU 574: (1) In situ external dose rate measurements were collected using thermoluminescent dosimeters at CAS 12-45-01, U12e.05 Crater (Blanca). (2) Total effective dose rates were determined at both sites by summing the internal and external dose rate components. (3) A use restriction (UR) was implemented at CAS 12-23-10, U12c.03 Crater (Neptune). Areas that exceed the final action level (FAL) of 25 millirems per year (mrem/yr) based on the Occasional Use Area exposure scenario are within the existing use restricted area for CAU 551. The 25-mrem/yr FAL is not exceeded outside the existing CAU 551 UR for any of the exposure scenarios (Industrial Area, Remote Work Area, and Occasional Use Area). Therefore, the existing UR for CAU 551 is sufficient to bound contamination that exceeds the FAL. (4) An administrative UR was implemented at CAS 12-45-01, U12e.05 Crater (Blanca) as a best management practice (BMP). The 25-mrem/yr FAL was not exceeded for the Remote Work Area or Occasional Use Area exposure scenarios; therefore, a UR is not required. However, because the 25-mrem/yr FAL was exceeded for the Industrial Area exposure scenario, an administrative UR was established as a BMP. UR documentation is included as Appendix B. The UR at CAS 12-23-10, U12c.03 Crater (Neptune), is within the existing UR for CAU 551. Additional postings were not installed, and annual post-closure inspections will be performed in conjunction with the inspections performed for CAU 551. At CAS 12-45-01, U12e.05 Crater (Blanca), the administrative UR does not require postings or inspections. NNSA/NSO requests the following: (1) A Notice of Completion from the Nevada Division of Environmental Protection to NNSA/NSO for closure of CAU 574; and (2) The transfer of CAU 574 from Appendix III to Appendix IV, Closed Corrective Action Units, of the FFACO« less

[Shoulder joint pain of rotator cuff injury treated with electroacupuncture and Mulligan's mobilization: a randomized controlled trial].

PubMed

Wang, Yanwu; Wang, Chongmin; Chen, Huade; Ye, Xinmiao

2018-01-12

To verify the clinical therapeutic effects on shoulder joint pain of rotator cuff injury treated with electroacupuncture (EA) and Mulligan's mobilization. A total of 120 patients of shoulder joint pain of rotator cuff injury were randomized into an EA group, a rehabilitation group and a combined therapy group, 40 cases in each one. In the EA group, EA was applied to Jianzhen (SI 9), Jianliao (TE 14), Jianyu (LI 15), Tianzong (SI 11), Jianqian (extra) and Binao (LI 14) in the affected side. Of these acupoints, Jianliao (TE 14) and Jianyu (LI 15), Jianzhen (SI 9) and Tianzong (SI 11) were stimulated with Han 's electric apparatus. In the rehabilitation group, Mulligan's mobilization was used, including scapular mobilization, static joint mobilization and dynamic joint mobilization. In the combined therapy group, EA was used in combination with Mulligan mobilization. The treatment was given once a day in each group, 5 sessions a week, totally for 6 weeks. The pain intensity of shoulder joint (VAS), the University of California at Los Angeles shoulder rating scale (UCLA) and the range of motion (ROM) of shoulder joint were evaluated before and 6 weeks after treatment separately. The adverse reactions were recorded in each group. VAS scores were all reduced, UCLA scores increased and ROM improved after treatment as compared with those before treatment in the patients of the three groups (all P <0.05). After treatment, VAS score, UCLA score and ROM in the combined therapy group were remarkably improved as compared with those in the EA group and the rehabilitation group (all P <0.05). Regarding the improvements of VAS and UCLA scores, the results in the EA group were better than those in the rehabilitation group (both P <0.05). Regarding ROM improvement, the results in the rehabilitation group were superior to those in the EA group (all P <0.05). There was no adverse reaction in the two groups. The combined therapy of EA and Mulligan's mobilization relieves shoulder joint pain of rotator cuff injury, better than the simple application of either EA or Mulligan's mobilization.

Clouds and hazes in exoplanets and brown dwarfs

NASA Astrophysics Data System (ADS)

Morley, Caroline Victoria

The formation of clouds significantly alters the spectra of cool substellar atmospheres from terrestrial planets to brown dwarfs. In cool planets like Earth and Jupiter, volatile species like water and ammonia condense to form ice clouds. In hot planets and brown dwarfs, iron and silicates instead condense, forming dusty clouds. Irradiated methane-rich planets may have substantial hydrocarbon hazes. During my dissertation, I have studied the impact of clouds and hazes in a variety of substellar objects. First, I present results for cool brown dwarfs including clouds previously neglected in model atmospheres. Model spectra that include sulfide and salt clouds can match the spectra of T dwarf atmospheres; water ice clouds will alter the spectra of the newest and coldest brown dwarfs, the Y dwarfs. These sulfide/salt and ice clouds potentially drive spectroscopic variability in these cool objects, and this variability should be distinguishable from variability caused by hot spots. Next, I present results for small, cool exoplanets between the size of Earth and Neptune. They likely have sulfide and salt clouds and also have photochemical hazes caused by stellar irradiation. Vast resources have been dedicated to characterizing the handful of super Earths and Neptunes accessible to current telescopes, yet of the planets smaller than Neptune studied to date, all have radii in the near-infrared consistent with being constant in wavelength, likely showing that these small planets are consistently enshrouded in thick hazes and clouds. For the super Earth GJ 1214b, very thick, lofted clouds of salts or sulfides in high metallicity (1000x solar) atmospheres create featureless transmission spectra in the near-infrared. Photochemical hazes also create featureless transmission spectra at lower metallicities. For the Neptune-sized GJ 436b, its thermal emission and transmission spectra combine indicate a high metallicity atmosphere, potentially heated by tides and affected by disequilibrium chemistry. I show that despite the challenges, there are promising avenues for understanding small planets: by observing thermal emission and reflected light, we can break the degeneracies and con- strain the atmospheric compositions. These future observations will provide rich diagnostics of molecules and clouds in small planets.

Characterization of the planetary system Kepler-101 with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

NASA Astrophysics Data System (ADS)

Bonomo, A. S.; Sozzetti, A.; Lovis, C.; Malavolta, L.; Rice, K.; Buchhave, L. A.; Sasselov, D.; Cameron, A. C.; Latham, D. W.; Molinari, E.; Pepe, F.; Udry, S.; Affer, L.; Charbonneau, D.; Cosentino, R.; Dressing, C. D.; Dumusque, X.; Figueira, P.; Fiorenzano, A. F. M.; Gettel, S.; Harutyunyan, A.; Haywood, R. D.; Horne, K.; Lopez-Morales, M.; Mayor, M.; Micela, G.; Motalebi, F.; Nascimbeni, V.; Phillips, D. F.; Piotto, G.; Pollacco, D.; Queloz, D.; Ségransan, D.; Szentgyorgyi, A.; Watson, C.

2014-12-01

We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp< 3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 - containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance - is certainly of interest for scenarios of planet formation and evolution. This system does not follow thepreviously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.Table 2 is available in electronic form at http://www.aanda.org

How to distinguish between cloudy mini-Neptunes and water/volatile-dominated super-Earths

DOE Office of Scientific and Technical Information (OSTI.GOV)

Benneke, Björn; Seager, Sara, E-mail: bbenneke@mit.edu

One of the most profound questions about the newly discovered class of low-density super-Earths is whether these exoplanets are predominately H{sub 2}-dominated mini-Neptunes or volatile-rich worlds with gas envelopes dominated by H{sub 2}O, CO{sub 2}, CO, CH{sub 4}, or N{sub 2}. Transit observations of the super-Earth GJ 1214b rule out cloud-free H{sub 2}-dominated scenarios, but are not able to determine whether the lack of deep spectral features is due to high-altitude clouds or the presence of a high mean molecular mass atmosphere. Here, we demonstrate that one can unambiguously distinguish between cloudy mini-Neptunes and volatile-dominated worlds based on wing steepnessmore » and relative depths of absorption features in moderate-resolution near-infrared transmission spectra (R ∼ 100). In a numerical retrieval study, we show for GJ 1214b that an unambiguous distinction between a cloudy H{sub 2}-dominated atmosphere and cloud-free H{sub 2}O atmosphere will be possible if the uncertainties in the spectral transit depth measurements can be reduced by a factor of ∼3 compared to the published Hubble Space Telescope Wide-Field Camera 3 and Very Large Telescope transit observations by Berta et al. and Bean et al. We argue that the required precision for the distinction may be achievable with currently available instrumentation by stacking 10-15 repeated transit observations. We provide a scaling law that scales our quantitative results to other transiting super-Earths and Neptunes such as HD 97658b, 55 Cnc e, GJ 3470b and GJ 436b. The analysis in this work is performed using an improved version of our Bayesian atmospheric retrieval framework. The new framework not only constrains the gas composition and cloud/haze parameters, but also determines our confidence in having detected molecules and cloud/haze species through Bayesian model comparison. Using the Bayesian tool, we demonstrate quantitatively that the subtle transit depth variation in the Berta et al. data is not sufficient to claim the detection of water absorption.« less

Seismology of Giant Planets: General Overview and Results from the Kepler K2 Observations of Neptune

NASA Astrophysics Data System (ADS)

Gaulme, Patrick

2017-10-01

For this invited contribution, I was asked to give an overview about the application of helio and aster-oseismic techniques to study the interior of giant planets, and to specifically present the recent observations of Neptune by Kepler K2. Seismology applied to giant planets could drastically change our understanding of their deep interiors, as it has happened with the Earth, the Sun, and many main-sequence and evolved stars. The study of giant planets' composition is important for understanding both the mechanisms enabling their formation and the origins of planetary systems, in particular our own. Unfortunately, its determination is complicated by the fact that their interior is thought not to be homogeneous, so that spectroscopic determinations of atmospheric abundances are probably not representative of the planet as a whole. Instead, the determination of their composition and structure must rely on indirect measurements and interior models. Giant planets are mostly fluid and convective, which makes their seismology much closer to that of solar-like stars than that of terrestrial planets. Hence, helioseismology techniques naturally transfer to giant planets. In addition, two alternative methods can be used: photometry of the solar light reflected by planetary atmospheres, and ring seismology in the specific case of Saturn. The current decade has been promising thanks to the detection of Jupiter's acoustic oscillations with the ground-based imaging-spectrometer SYMPA and indirect detection of Saturn's f-modes in its rings by the NASA Cassini orbiter. This has motivated new projects of ground-based and space-borne instruments that are under development. The K2 observations represented the first opportunity to search for planetary oscillations with visible photometry. Despite the excellent quality of K2 data, the noise level of the power spectrum of the light curve was not low enough to detect Neptune's oscillations. The main results from the K2 observations are the clear detection of the well-known differential rotation of Neptune, measured for the first time through the rotational modulation of its photometry, and the detection of the Sun's oscillations, for the first time in an indirect way in intensity measurements.

Modeling mid-ocean ridge hydrothermal response to earthquakes, tides, and ocean currents: a case study at the Grotto mound, Endeavour Segment, Juan de Fuca Ridge

NASA Astrophysics Data System (ADS)

Xu, G.; Bemis, K. G.

2014-12-01

Seafloor hydrothermal systems feature intricate interconnections among oceanic, geological, hydrothermal, and biological processes. The advent of the NEPTUNE observatory operated by Ocean Networks Canada at the Endeavour Segment, Juan de Fuca Ridge enables scientists to study these interconnections through multidisciplinary, continuous, real-time observations. The multidisciplinary observatory instruments deployed at the Grotto Mound, a major study site of the NEPTUNE observatory, makes it a perfect place to study the response of a seafloor hydrothermal system to geological and oceanic processes. In this study, we use the multidisciplinary datasets recorded by the NEPTUNE Observatory instruments as observational tools to demonstrate two different aspects of the response of hydrothermal activity at the Grotto Mound to geological and oceanic processes. First, we investigate a recent increase in venting temperature and heat flux at Grotto observed by the Benthic and Resistivity Sensors (BARS) and the Cabled Observatory Vent Imaging Sonar (COVIS) respectively. This event started in Mar 2014 and is still evolving by the time of writing this abstract. An initial interpretation in light of the seismic data recorded by a neighboring ocean bottom seismometer on the NEPTUNE observatory suggests the temperature and heat flux increase is probably triggered by local seismic activities. Comparison of the observations with the results of a 1-D mathematical model simulation of hydrothermal sub-seafloor circulation elucidates the potential mechanisms underlying hydrothermal response to local earthquakes. Second, we observe significant tidal oscillations in the venting temperature time series recorded by BARS and the acoustic imaging of hydrothermal plumes by COVIS, which is evidence for hydrothermal response to ocean tides and currents. We interpret the tidal oscillations of venting temperature as a result of tidal loading on a poroelastic medium. We then invoke poroelastic theories to estimate the crustal permeability, a fundamental property of subsurface hydrothermal circulation, from the phase shift of the tidal oscillations of venting temperature relative to ambient ocean tides. These results together shed light on the influences of seismic and oceanic processes on a seafloor hydrothermal system.

The nature of the giant exomoon candidate Kepler-1625 b-i

NASA Astrophysics Data System (ADS)

Heller, René

2018-02-01

The recent announcement of a Neptune-sized exomoon candidate around the transiting Jupiter-sized object Kepler-1625 b could indicate the presence of a hitherto unknown kind of gas giant moon, if confirmed. Three transits of Kepler-1625 b have been observed, allowing estimates of the radii of both objects. Mass estimates, however, have not been backed up by radial velocity measurements of the host star. Here we investigate possible mass regimes of the transiting system that could produce the observed signatures and study them in the context of moon formation in the solar system, i.e., via impacts, capture, or in-situ accretion. The radius of Kepler-1625 b suggests it could be anything from a gas giant planet somewhat more massive than Saturn (0.4 MJup) to a brown dwarf (BD; up to 75 MJup) or even a very-low-mass star (VLMS; MJup ≈ 0.11 M⊙). The proposed companion would certainly have a planetary mass. Possible extreme scenarios range from a highly inflated Earth-mass gas satellite to an atmosphere-free water-rock companion of about 180 M⊕. Furthermore, the planet-moon dynamics during the transits suggest a total system mass of 17.6-12.6+19.2 MJup. A Neptune-mass exomoon around a giant planet or low-mass BD would not be compatible with the common mass scaling relation of the solar system moons about gas giants. The case of a mini-Neptune around a high-mass BD or a VLMS, however, would be located in a similar region of the satellite-to-host mass ratio diagram as Proxima b, the TRAPPIST-1 system, and LHS 1140 b. The capture of a Neptune-mass object around a 10 MJup planet during a close binary encounter is possible in principle. The ejected object, however, would have had to be a super-Earth object, raising further questions of how such a system could have formed. In summary, this exomoon candidate is barely compatible with established moon formation theories. If it can be validated as orbiting a super-Jovian planet, then it would pose an exquisite riddle for formation theorists to solve.

Still Growing Strong: UCLA Library.

ERIC Educational Resources Information Center

McClung, Patricia

1983-01-01

This description of the development of an academic research library in Los Angeles includes a brief history of the University of California, and discusses university librarians, library buildings, special collections, automation, and cooperative programs. (EJS)

Nancy Haegel | NREL

Science.gov Websites

received the UCLA TRW Excellence in Teaching Award, the Alpha Sigma Nu Teacher of the Year Award at Fairfield University, and the NPS Schieffelin Award for Teaching Excellence. She received the 2004 APS Prize

The parameterization of the planetary boundary layer in the UCLA general circulation model - Formulation and results

NASA Technical Reports Server (NTRS)

Suarez, M. J.; Arakawa, A.; Randall, D. A.

1983-01-01

A planetary boundary layer (PBL) parameterization for general circulation models (GCMs) is presented. It uses a mixed-layer approach in which the PBL is assumed to be capped by discontinuities in the mean vertical profiles. Both clear and cloud-topped boundary layers are parameterized. Particular emphasis is placed on the formulation of the coupling between the PBL and both the free atmosphere and cumulus convection. For this purpose a modified sigma-coordinate is introduced in which the PBL top and the lower boundary are both coordinate surfaces. The use of a bulk PBL formulation with this coordinate is extensively discussed. Results are presented from a July simulation produced by the UCLA GCM. PBL-related variables are shown, to illustrate the various regimes the parameterization is capable of simulating.

Vision screening of abused and neglected children by the UCLA Mobile Eye Clinic.

PubMed

Yoo, R; Logani, S; Mahat, M; Wheeler, N C; Lee, D A

1999-07-01

The purpose of our study was to present descriptive findings of ocular abnormalities in vision screening examinations of abused and neglected children. We compared the prevalence and the nature of eye diseases and refractive error between abused and neglected boys staying at the Hathaway Home, a residential facility for abused children, and boys from neighboring Boys and Girls clubs. The children in the study received vision screening examinations through the UCLA Mobile Eye Clinic following a standard format. Clinical data were analyzed by chi-square test. The children with a history of abuse demonstrated significantly higher prevalence of myopia, astigmatism, and external eye disorders. Our study suggests that children with a history of abuse may be at higher risk for visual impairment. These visual impairments may be the long-term sequelae of child abuse.

UCLA Translational Biomarker Development Program (UTBD)

DOE Office of Scientific and Technical Information (OSTI.GOV)

Czernin, Johannes

2014-09-01

The proposed UTBD program integrates the sciences of diagnostic nuclear medicine and (radio)chemistry with tumor biology and drug development. UTBD aims to translate new PET biomarkers for personalized medicine and to provide examples for the use of PET to determine pharmacokinetic (PK) and pharmacodynamic (PD) drug properties. The program builds on an existing partnership between the Ahmanson Translational Imaging Division (ATID) and the Crump Institute of Molecular Imaging (CIMI), the UCLA Department of Chemistry and the Division of Surgical Oncology. ATID provides the nuclear medicine training program, clinical and preclinical PET/CT scanners, biochemistry and biology labs for probe and drugmore » development, radiochemistry labs, and two cyclotrons. CIMI provides DOE and NIH-funded training programs for radio-synthesis (START) and molecular imaging (SOMI). Other participating entities at UCLA are the Department of Chemistry and Biochemistry and the Division of Surgical Oncology. The first UTBD project focuses on deoxycytidine kinase, a rate-limiting enzyme in nucleotide metabolism, which is expressed in many cancers. Deoxycytidine kinase (dCK) positive tumors can be targeted uniquely by two distinct therapies: 1) nucleoside analog prodrugs such as gemcitabine (GEM) are activated by dCK to cytotoxic antimetabolites; 2) recently developed small molecule dCK inhibitors kill tumor cells by starving them of nucleotides required for DNA replication and repair. Since dCK-specific PET probes are now available, PET imaging of tumor dCK activity could improve the use of two different classes of drugs in a wide variety of cancers.« less

Life satisfaction, loneliness and related factors during female midlife.

PubMed

Fernández-Alonso, Ana M; Trabalón-Pastor, Martina; Vara, Carmen; Chedraui, Peter; Pérez-López, Faustino R

2012-05-01

Studies assessing life satisfaction and feelings of loneliness in mid-aged women are scarce. To assess loneliness, life satisfaction and related factors in mid-aged Spanish women. This was a cross sectional study in which 182 women aged 40 to 65 completed the menopause rating scale (MRS), the University of California at Los Angeles loneliness scale (UCLA-LS), the life satisfaction index A (LSI-A), and a general socio-demographic questionnaire containing personal/partner data. Internal consistency of each tool was also computed. Median [interquartile range] age of the sample was 51 [9.0] years. A 55.5% were postmenopausal, 47.3% had increased body mass index (BMI) values, 57.7% were abdominally obese, 1.6% had hypertension and 86.3% had a stable partner. In addition, 4.9% used hormone therapy and 19.2% psychotropic drugs. Multiple linear regression analysis found that higher UCLA-LS scores (more loneliness) correlated with MRS psychological scores, partner alcohol abuse, living in urban areas, lower LSI-A scores (less life satisfaction) and not having a stable partner. Lower LSI-A scores (worse life satisfaction) correlated with severe female economical problems, BMI values and UCLA-LS and MRS psychological scores. Loneliness and life satisfaction in this mid-aged female sample was influenced by personal and partner issues which seem to play a much more relevant role than biological aspects. More research is warranted in this regard. Copyright © 2012 Elsevier Ireland Ltd. All rights reserved.

Quality of life psychosocial characteristics in Greek patients with leg ulcers: a case control study.

PubMed

Kouris, Anargyros; Armyra, Kalliopi; Christodoulou, Christos; Sgontzou, Themis; Karypidis, Dimitrios; Kontochristopoulos, George; Liordou, Fotini; Zakopoulou, Nikoletta; Zouridaki, Eftychia

2016-10-01

Chronic leg ulcers are a public health problem that can have a significant impact on the patient's physical, socioeconomic and psychological status. The aim of this study is to evaluate the quality of life, anxiety and depression, self-esteem and loneliness in patients suffering from leg ulcers. A total of 102 patients were enrolled in the study. The quality of life, anxiety and depression, self-esteem and loneliness of the patient were assessed using the Dermatology Life Quality Index (DLQI), Hospital Anxiety and Depression Scale (HADS), Rosenberg's Self-esteem Scale (RSES) and the UCLA Loneliness Scale (UCLA-Version 3), respectively. The mean DLQI score was 13·38 ± 2·59, suggesting a serious effect on the quality of life of patients. Those with leg ulcers had statistically significant higher scores according to the HADS-total scale (P = 0·031) and HADS-anxiety subscale (P = 0·015) compared with healthy volunteers. Moreover, a statistically significant difference was found between the two groups concerning the UCLA-scale (P = 0·029). Female patients presented with a higher score of anxiety (P = 0·027) and social isolation (P = 0·048), and worse quality of life (P = 0·018) than male patients. A severe quality of life impairment was documented, reflecting a significant psychosocial impact on patients with leg ulcers. © 2014 The Authors. International Wound Journal © 2014 Medicalhelplines.com Inc and John Wiley & Sons Ltd.

Laboratory for Hydrospheric Processes 1997 Publications

NASA Technical Reports Server (NTRS)

Busalacchi, Antonio J.

1997-01-01

This document is a compilation of publications of the Goddard Space Flight Center Laboratory for Hydrospheric Processes for calendar year 1997. Each two-page entry is a cut-and-pasted extraction from a 1997 published journal article, book chapter, symposium or conference proceedings, or technical memorandum. This provides a quick, inexpensive way to communicate our research. If you wish further information, or a reprint, please contact the author of the article or the publisher. There are two sections, the first consisting of 76 journal articles and book chapters which are arranged according to the science priorities of NASA's Earth Science Enterprise: Land-Cover Change and Global Productivity Seasonal-to-Interannual Climate Prediction Natural Hazards Long-Term Climate Variability Atmospheric Ozone, and an additional category Sensor/Algorithm Development. * Each of these sections is preceded by a foreword. A second section, consisting of 52 other contributions (e.g. conference/symposium proceedings and technical memoranda), provides additional scientific information to the outside community. This document was initiated within the Earth Sciences Directorate at the NASA/Goddard Space Flight Center to provide internal communication. We anticipate it will prove useful to visitors and other people interested in our research. This is our fifth annual document. The Laboratory for Hydrospheric Processes is one of the major elements of the Earth Sciences Directorate at NASA's Goddard Space Flight Center. Scientific investigations within the Division range from theoretical to experimental research dealing with oceanic/physical oceanography, hydrologic, and cryospheric sciences. The Laboratory currently has a staff of 60 civil servants and approximately 138 visiting scientists, postdoctoral fellows, and contractors. At various times throughout the year, the Laboratory hosts additional personnel through NASA and Goddard sponsored enrichment programs for high school, undergraduate and graduate students, and high school and university faculty. For further information see our web site at http://neptune.gsfc.nasa.gov.

Eighteen ninety five and all that

NASA Astrophysics Data System (ADS)

Heilbron, J. L.; Bynum, W. F.

1995-01-01

Anniversarial commemorations this year include the discovery of X-rays, the calculation of the position of the undiscovered planet Neptune, the emergence of syphilis and the mandatory serving of lime juice to British sailors.

Atmospheric Models for Aeroentry and Aeroassist

NASA Technical Reports Server (NTRS)

Justus, C. G.; Duvall, Aleta; Keller, Vernon W.

2005-01-01

Eight destinations in the Solar System have sufficient atmosphere for aeroentry, aeroassist, or aerobraking/aerocapture: Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune, plus Saturn's moon Titan. Engineering-level atmospheric models for Earth, Mars, Titan, and Neptune have been developed for use in NASA's systems analysis studies of aerocapture applications. Development has begun on a similar atmospheric model for Venus. An important capability of these models is simulation of quasi-random perturbations for Monte Carlo analyses in developing guidance, navigation and control algorithms, and for thermal systems design. Characteristics of these atmospheric models are compared, and example applications for aerocapture are presented. Recent Titan atmospheric model updates are discussed, in anticipation of applications for trajectory and atmospheric reconstruct of Huygens Probe entry at Titan. Recent and planned updates to the Mars atmospheric model, in support of future Mars aerocapture systems analysis studies, are also presented.

La planète Vulcain, une perspective américaine, traduction d'un article de William Shehan et Tony Misch

NASA Astrophysics Data System (ADS)

Lequeux, James

2016-10-01

After his discovery of Neptune in 1846, Le Verrier attempted to extend Newton's theory to the innermost planet, Mercury. He found a small unexplained discrepancy in its motion. Applying the same assumption as had succeeded to explain the motion of Uranus with Neptune, he proposed the existence of an intra-Mercurial planet, named Vulcan, which would have perturbed Mercury. This article describes the long searches for Vulcan in America. Vulcan was never found from either side of the Atlantic, as well as a possible ring of debris which could have played the same role. The anomalous precession of the perihelion of Mercury was finally explained by Einstein in1915 in terms of the General Theory of Relativity, and provided one of the first confirmations of the theory's correctness.

Recovering Neptune 170 Years After its Initial Discovery

NASA Astrophysics Data System (ADS)

Myles, Justin

2017-01-01

Recent work by Trujillo and Shephard (2014) and Batygin and Brown (2016) has shown an as-yet unexplained clustering of the periapse vectors of the most distant Kuiper Belt objects. This unusual clustering has motivated the search for an unseen perturbing planet that is responsible for maintaining the alignment. As a proof of concept of a technique for locating unseen solar system planets, we use dynamical N-body integrations to simulate the orbital dynamics of distant Kuiper Belt objects, with the aim of determining the orbital parameters of Neptune (which, for the sake of exercise, we assume is, as-yet, undiscovered). In this poster, we determine the accuracy with which the perturbing planet’s orbital elements and sky location can be determined, and we show how the lessons learned can improve the search strategy for potentially undiscovered trans-Neptunian planets.

Neptune: towards understanding how Adams's upbringing enabled him to predict, then miss the discovery of the century

NASA Astrophysics Data System (ADS)

Sheen, B.

2013-03-01

The story of John Couch Adams the great Cornish astronomer of the nineteenth century is well known and this paper will not revisit old ground. However, many questions remain unanswered and in this paper I propose to indicate some of them as section headings, and seek to address them. In this way Adams's early life is examined, and its effect on his academic life during the time of the Neptune discovery. The row that followed discovery is high-lighted together with the equally contentious issue of the new planet's name. Although it is usually believed that Adams graciously accepted the failure of the Cambridge University Observatory to find his planet, examination of his later work which is often highly critical of French astronomers sheds a different light on that theory.

An explanation for both the large inclination and eccentricity of the dipole-like field of Uranus and Neptune

NASA Technical Reports Server (NTRS)

Akasofu, S.-I.; Lee, L.-H.; Saito, T.

1991-01-01

It is shown that the offset tilted dipole model of Uranus and Neptune, deduced from the spherical harmonic analysis of the Voyager magnetic field observation, can be represented fairly well by the combined field of an axial and an auxiliary dipole; the latter is roughly oriented in the east-west direction and is located near the surface of the core in low latitude. The present dynamo theories of planetary magnetism consider an axial dipolar field as an essential element, since the planetary rotation plays a vital role in the dynamo process. On the other hand, the auxiliary dipoles may be a result of leakage of the toroidal field, like a pair of sunspots on the photosphere, which is also an essential part of the dynamo process.

Development of a Three-Dimensional Spectral Element Model for NWP: Idealized Simulations on the Sphere

NASA Astrophysics Data System (ADS)

Viner, K.; Reinecke, P. A.; Gabersek, S.; Flagg, D. D.; Doyle, J. D.; Martini, M.; Ryglicki, D.; Michalakes, J.; Giraldo, F.

2016-12-01

NEPTUNE: the Navy Environmental Prediction sysTem Using the NUMA*corE, is a 3D spectral element atmospheric model composed of a full suite of physics parameterizations and pre- and post-processing infrastructure with plans for data assimilation and coupling components to a variety of Earth-system models. This talk will focus on the initial struggles and solutions in adapting NUMA for stable and accurate integration on the sphere using both the deep atmosphere equations and a newly developed shallow-atmosphere approximation, as demonstrated through idealized test cases. In addition, details of the physics-dynamics coupling methodology will be discussed. NEPTUNE results for test cases from the 2016 Dynamical Core Model Intercomparison Project (DCMIP-2016) will be shown and discussed. *NUMA: Nonhydrostatic Unified Model of the Atmosphere; Kelly and Giraldo 2012, JCP

Streamlined Approach for Environmental Restoration Plan for Corrective Action Unit 574: Neptune, Nevada National Security Site, Nevada

DOE Office of Scientific and Technical Information (OSTI.GOV)

NSTec Environmental Restoration

2011-08-31

This Streamlined Approach for Environmental Restoration (SAFER) Plan identifies the activities required for closure of Corrective Action Unit (CAU) 574, Neptune. CAU 574 is included in the Federal Facility Agreement and Consent Order (FFACO) (1996 [as amended March 2010]) and consists of the following two Corrective Action Sites (CASs) located in Area 12 of the Nevada National Security Site: (1) CAS 12-23-10, U12c.03 Crater (Neptune); (2) CAS 12-45-01, U12e.05 Crater (Blanca). This plan provides the methodology for the field activities that will be performed to gather the necessary information for closure of the two CASs. There is sufficient information andmore » process knowledge regarding the expected nature and extent of potential contaminants to recommend closure of CAU 574 using the SAFER process. Based on historical documentation, personnel interviews, site process knowledge, site visits, photographs, field screening, analytical results, the results of the data quality objective (DQO) process (Section 3.0), and an evaluation of corrective action alternatives (Appendix B), closure in place with administrative controls is the expected closure strategy for CAU 574. Additional information will be obtained by conducting a field investigation to verify and support the expected closure strategy and provide a defensible recommendation that no further corrective action is necessary. This will be presented in a Closure Report that will be prepared and submitted to the Nevada Division of Environmental Protection (NDEP) for review and approval.« less

Stone Soup Projects: Using real-time resources and creative partnering to meet multiple needs

NASA Astrophysics Data System (ADS)

McLean, S.; Searle, R.; Zala, K.

2010-12-01

Ocean Networks Canada oversees the VENUS and NEPTUNE Canada undersea cabled observatories. Its Centre for Enterprise and Engagement communicates the scientific discoveries and technological innovations happening at the two systems. Not surprisingly, funders in ocean science are interested in seeing evidence of increased recruitment of Highly Qualified Personnel into marine science and industry. This demand creates a series of opportunities for inspiring students, ranging from graduate school down to middle school, to pursue studies in chemistry, biology, physics, geology, engineering, and beyond. As the Engagement section is a small operation, we partner with others to produce educational assets incorporating real-time data from VENUS and NEPTUNE Canada observatories that enable frontline educators to create exciting ocean science experiences for students and the public. In one project, the lab component of an entire undergraduate course lets students conduct their own investigations into marine oxygen levels by using VENUS data. In another, Fine Arts graduate and undergraduate students are using high-tech tools to create a series of webisodes that map the principles of Ocean Literacy onto the science themes of VENUS and NEPTUNE Canada. In a third project, we hosted a website for a collaborative expedition to small coastal towns that focused on the marine science happening in the Salish Sea, British Columbia. Our projects and challenges for engaging students and the public with ocean science using real-time and other data offer strategies for outreach and education sections of similar organizations.

A Search for Transiting Neptune-Mass Extrasolar Planets in High-Precision Photometry of Solar-Type Stars

NASA Technical Reports Server (NTRS)

Henry, Stephen M.; Gillman, Amelie r.; Henry, Gregory W.

2005-01-01

Tennessee State University operates several automatic photometric telescopes (APTs) at Fairborn Observatory in southern Arizona. Four 0.8 m APTs have been dedicated to measuring subtle luminosity variations that accompany magnetic cycles in solar-type stars. Over 1000 program and comparison stars have been observed every clear night in this program for up to 12 years with a precision of approximately 0.0015 mag for a single observation. We have developed a transit-search algorithm, based on fitting a computed transit template for each trial period, and have used it to search our photometric database for transits of unknown companions. Extensive simulations with the APT data have shown that we can reliably recover transits with periods under 10 days as long as the transits have a depth of at least 0.0024 mag, or about 1.6 times the scatter in the photometric observations. Thus, due to our high photometric precision, we are sensitive to transits of possible short-period Neptune-mass planets that likely would have escaped detection by current radial velocity techniques. Our search of the APT data sets for 1087 program and comparison stars revealed no new transiting planets. However, the detection of several unknown grazing eclipsing binaries from among our comparison stars, with eclipse depths of only a few millimags, illustrates the success of our technique. We have used this negative result to place limits on the frequency of Neptune-mass planets in close orbits around solar-type stars in the Sun's vicinity.

A resonant chain of four transiting, sub-Neptune planets.

PubMed

Mills, Sean M; Fabrycky, Daniel C; Migaszewski, Cezary; Ford, Eric B; Petigura, Erik; Isaacson, Howard

2016-05-26

Surveys have revealed many multi-planet systems containing super-Earths and Neptunes in orbits of a few days to a few months. There is debate whether in situ assembly or inward migration is the dominant mechanism of the formation of such planetary systems. Simulations suggest that migration creates tightly packed systems with planets whose orbital periods may be expressed as ratios of small integers (resonances), often in a many-planet series (chain). In the hundreds of multi-planet systems of sub-Neptunes, more planet pairs are observed near resonances than would generally be expected, but no individual system has hitherto been identified that must have been formed by migration. Proximity to resonance enables the detection of planets perturbing each other. Here we report transit timing variations of the four planets in the Kepler-223 system, model these variations as resonant-angle librations, and compute the long-term stability of the resonant chain. The architecture of Kepler-223 is too finely tuned to have been formed by scattering, and our numerical simulations demonstrate that its properties are natural outcomes of the migration hypothesis. Similar systems could be destabilized by any of several mechanisms, contributing to the observed orbital-period distribution, where many planets are not in resonances. Planetesimal interactions in particular are thought to be responsible for establishing the current orbits of the four giant planets in the Solar System by disrupting a theoretical initial resonant chain similar to that observed in Kepler-223.

Gas Planet Orbits

NASA Image and Video Library

2008-08-19

Jupiter, Saturn, Uranus, and Neptune are known as the jovian Jupiter-like planets because they are all gigantic compared with Earth, and they have a gaseous nature. This diagram shows the approximate distance of the jovian planets from the Sun.

Neptune

NASA Image and Video Library

1999-08-08

NASA Voyager 2 obtained these images of satellite 1989N2 and revealed it to be and irregularly shaped, dark object. The satellite appeared to have several craters. The irregular outline suggests that this moon has remained cold and rigid throughout much

The benefit of synthetic versus biological patch augmentation in the repair of posterosuperior massive rotator cuff tears: a 3-year follow-up study.

PubMed

Ciampi, Pietro; Scotti, Celeste; Nonis, Alessandro; Vitali, Matteo; Di Serio, Clelia; Peretti, Giuseppe M; Fraschini, Gianfranco

2014-05-01

Rotator cuff repair typically results in a satisfactory, although variable, clinical outcome. However, anatomic failure of the repaired tendon often occurs. Patch augmentation can improve the results of open rotator cuff repair by supporting the healing process, protecting the suture, and reducing friction in the subacromial space. Cohort study; Level of evidence, 3. A total of 152 patients with a posterosuperior massive rotator cuff tear were treated by open repair only (control group; n = 51; mean age, 67.06 ± 4.42 years), open repair together with collagen patch augmentation (collagen group; n = 49; mean age, 66.53 ± 5.17 years), or open repair together with polypropylene patch augmentation (polypropylene group; n = 52; mean age, 66.17 ± 5.44 years) and were retrospectively studied. Patients were evaluated preoperatively and after 36 months with a visual analog scale (VAS) and the University of California, Los Angeles (UCLA) shoulder rating scale and by measuring elevation of the scapular plane and strength with a dynamometer. The VAS and UCLA scores were also obtained 2 months postoperatively. Tendon integrity was assessed after 1 year by ultrasound. Patients were homogeneous as per the preoperative assessment. After 2 months, results (mean ± standard deviation) for the control, collagen, and polypropylene groups, respectively, were as follows: VAS scores were 6.96 ± 1.11, 6.46 ± 1.02, and 4.92 ± 0.90, while UCLA scores were 11.29 ± 1.46, 11.40 ± 1.51, and 19.15 ± 1.99. After 36 months, the mean scores for the respective groups were 3.66 ± 1.05, 4.06 ± 1.02, and 3.28 ± 1.10 for the VAS and 14.88 ± 1.98, 14.69 ± 1.99, and 24.61 ± 3.22 for the UCLA scale. In addition, after 36 months, elevation on the scapular plane was 140.68° ± 9.84°, 140.61° ± 12.48°, and 174.71° ± 8.18°, and abduction strength was 8.73 ± 0.54 kg, 9.03 ± 0.60 kg, and 13.79 ± 0.64 kg for the control, collagen, and polypropylene groups, respectively. The retear rate after 12 months was 41% (21/51) for the control group, 51% (25/49) for the collagen group, and 17% (9/52) for the polypropylene group. In particular, the reduced 12-month retear rate and the increased UCLA scores, abduction strength, and elevation at 3-year follow-up were statistically significant for patients treated with a polypropylene patch compared with those treated with repair only or with a collagen patch. Polypropylene patch augmentation of rotator cuff repair was demonstrated to significantly improve the 36-month outcome in terms of function, strength, and retear rate.

Probing the vertical cloud structure of Uranus and Neptune with ground-based near-infrared observations at UKIRT, IRTF and Gemini-North

NASA Astrophysics Data System (ADS)

Irwin, Patrick G. J.; Teanby, Nicholas N.; Davis, Gary R.; Orton, Glenn; Fletcher, Leigh; Tice, Dane; Hurley, Jane

2010-05-01

In 2006, 2007 and 2008 observations of the near-infrared spectrum of Uranus were made with the UIST instrument of the UK Infrared Telescope, covering the period of Uranus' Northern Spring Equinox in 2008. A significant change in the visible appearance of Uranus occurred during this time with the southern polar zone at 45°S fading, while a corresponding zone at 45°N began to form. In addition, the visibility of the equatorial zone and darker mid-latitude belts increased. The observed spectra were fitted (Irwin et al., Icarus 203, 287 - 302, 2009), using the NEMESIS optimal estimation retrieval model to determine the variation in the latitudinal and vertical cloud structure during this time. However, since publication, a new set of methane absorption data has become available (Karkoschka and Tomasko, 2009, Icarus, submitted), which appears to be more reliable at the cold temperatures and high pressures of Uranus' deep atmosphere. We have fitted k-coefficients to these new methane absorption data and we find that although the inter-annual changes reported by Irwin et al. (2009) stand, the new k-data place the main cloud deck at lower pressures (2-3 bars) than derived previously in the H-band of ~ 3-4 bars and ~ 6 bars in the J-band. In addition, we find that using the new methane coefficients it is much easier to fit simultaneously the 1.6, 1.3 and 1.1 μm peaks. During the Uranus observations in 2007, corresponding observations were also made of Neptune's near-infrared spectrum, albeit with substantially poorer spatial resolution. The spectra were nevertheless sufficient to retrieve the gross variation in Neptune's latitudinal-vertical cloud structure and, like previous studies, we find the main cloud deck to exist at similar pressure levels to the main Uranus cloud deck, but with considerably thicker overlying stratospheric haze. The retrieved vertical-latitudinal cloud structure on Uranus and Neptune, observed with identical instrument setups, will be presented and discussed. Observations of both Uranus and Neptune were also made in 2009 with the SpeX instrument (0.8 to 2.4 μm) on the NASA Infrared Telescope Facility and also with the NIFS and NIRI instruments on the Gemini North telescope. The IRTF measurements were made with seeing conditions of approximately 0.5 arcsec, while the Gemini observations were made with Adaptive Optics and thus have considerably better spatial resolution. We intend to use the NIFS observations to study the limb-darkening curves from 1.45 to 1.75 μm, which should provide better constraints in the vertical cloud structure and we intend to use the IRTF measurements to extend our analysis to shorter wavelengths and also provide better radiometric calibration between the different reflectance peaks. These new observations will be presented and compared with the previous UKIRT observations.

Dynamical Evolution of Planetesimals in the Outer Solar System. II. The Saturn/Uranus and Uranus/Neptune Zones

NASA Astrophysics Data System (ADS)

Grazier, Kevin R.; Newman, William I.; Varadi, Ferenc; Kaula, William M.; Hyman, James M.

1999-08-01

We report on numerical simulations exploring the dynamical stability of planetesimals in the gaps between the outer Solar System planets. We search for stable niches in the Saturn/Uranus and Uranus/Neptune zones by employing 10,000 massless particles-many more than previous studies in these two zones-using high-order optimized multistep integration schemes coupled with roundoff error minimizing methods. An additional feature of this study, differing from its predecessors, is the fact that our initial distributions contain particles on orbits which are both inclined and noncircular. These initial distributions were also Gaussian distributed such that the Gaussian peaks were at the midpoint between the neighboring perturbers. The simulations showed an initial transient phase where the bulk of the primordial planetesimal swarm was removed from the Solar System within 105 years. This is about 10 times longer than we observed in our previous Jupiter/Saturn studies. Next, there was a gravitational relaxation phase where the particles underwent a random walk in momentum space and were exponentially eliminated by random encounters with the planets. Unlike our previous Jupiter/Saturn simulation, the particles did not fully relax into a third Lagrangian niche phase where long-lived particles are at Lagrange points or stable niches. This is either because the Lagrangian niche phase never occurs or because these simulations did not have enough particles for this third phase to manifest. In these simulations, there was a general trend for the particles to migrate outward and eventually to be cleared out by the outermost planet in the zone. We confirmed that particles with higher eccentricities had shorter lifetimes and that the resonances between the jovian planets "pumped up" the eccentricities of the planetesimals with low-inclination orbits more than those with higher inclinations. We estimated the expected lifetime of particles using kinetic theory and even though the time scale of the Uranus/Neptune simulation was 380 times longer than our previous Jupiter/Saturn simulation, the planetesimals in the Uranus/Neptune zone were cleared out more quickly than those in the Saturn/Uranus zone because of the positions of resonances with the jovian planets. These resonances had an even greater effect than random gravitational stirring in the winnowing process and confirm that all the jovian planets are necessary in long simulations. Even though we observed several long-lived zones near 12.5, 14.4, 16, 24.5, and 26 AU, only two particles remained at the end of the 109-year integration: one near the 2 : 3 Saturn resonance, and the other near the Neptune 1 : 1 resonance. This suggests that niches for planetesimal material in the jovian planets are rare and may exist either only in extremely narrow bands or in the neighborhoods of the triangular Lagrange points of the outer planets.

Relationship among self-esteem, psychological reactance, and other personality variables.

PubMed

Joubert, C E

1990-06-01

69 women and 42 men responded to the Coopersmith Self-esteem Inventory, the Revised UCLA Loneliness Scale, the Hong Psychological Reactance Scale, and the Famous Sayings test. Also, subjects rated their happiness using a Likert scale. Men scored significantly higher than did women on the UCLA Loneliness, Hostility, and Psychological Reactance measures, and lower on the Conventional Mores and Social Acquiescence measures. Loneliness scores positively correlated with Psychological Reactance scores and negatively with Self-esteem and Conventional Mores scores and with happiness self-ratings for both sexes. Men who scored higher on Psychological Reactance tended to score lower on Conventional Mores. Happiness ratings correlated negatively with Psychological Reactance for all subjects and positively with Conventional Mores for men subjects only. Women's self-esteem scores correlated positively with self-ratings of happiness and negatively with Psychological Reactance, Hostility, and Fear of Failure. Finally, women's Psychological Reactance scores correlated positively with those on Bass's Fear of Failure scale.

Experimental And Theoretical High Energy Physics Research At UCLA

DOE Office of Scientific and Technical Information (OSTI.GOV)

Cousins, Robert D.

2013-07-22

This is the final report of the UCLA High Energy Physics DOE Grant No. DE-FG02- 91ER40662. This report covers the last grant project period, namely the three years beginning January 15, 2010, plus extensions through April 30, 2013. The report describes the broad range of our experimental research spanning direct dark matter detection searches using both liquid xenon (XENON) and liquid argon (DARKSIDE); present (ICARUS) and R&D for future (LBNE) neutrino physics; ultra-high-energy neutrino and cosmic ray detection (ANITA); and the highest-energy accelerator-based physics with the CMS experiment and CERN’s Large Hadron Collider. For our theory group, the report describesmore » frontier activities including particle astrophysics and cosmology; neutrino physics; LHC interaction cross section calculations now feasible due to breakthroughs in theoretical techniques; and advances in the formal theory of supergravity.« less

[Cost-effectiveness of local steroid combined with therapeutic exercise in subacromial impingement syndrome].

PubMed

Ramírez-Ortiz, Julio; Mendoza-Eufracio, José Dolores; García-Viveros, María Ricarda; Márquez-Celedonio, Félix Guillermo

2017-01-01

The most common cause of injury is shoulder impingement syndrome. Management includes physical therapy, analgesics, steroids and surgery. The aim of the study was to determine the cost-effectiveness of using steroids combined with therapeutic exercise at home in the chronic impingement syndrome. Clinical trial randomized in 30 people with subacromial impingement syndrome underwent two treatments: steroid and at home rehabilitation booklet evaluated at the first and fourth week through UCLA Shoulder rating scale. We studied 17 men (56.7 %) and 13 women (43.3 %), mean age was 42.87 years. Group 2 earned greater improvement in UCLA Shoulder rating scale 18.87 at baseline and 27.60 at the end. With 30.27 accumulated disability days for group 1, and 14.80 for group 2. The combination of local steroids with therapeutic exercise is more effective clinically and declining disability compared to conventional physical therapy.

UCLA IGPP Space Plasma Simulation Group

NASA Technical Reports Server (NTRS)

1998-01-01

During the past 10 years the UCLA IGPP Space Plasma Simulation Group has pursued its theoretical effort to develop a Mission Oriented Theory (MOT) for the International Solar Terrestrial Physics (ISTP) program. This effort has been based on a combination of approaches: analytical theory, large scale kinetic (LSK) calculations, global magnetohydrodynamic (MHD) simulations and self-consistent plasma kinetic (SCK) simulations. These models have been used to formulate a global interpretation of local measurements made by the ISTP spacecraft. The regions of applications of the MOT cover most of the magnetosphere: the solar wind, the low- and high-latitude magnetospheric boundary, the near-Earth and distant magnetotail, and the auroral region. Most recent investigations include: plasma processes in the electron foreshock, response of the magnetospheric cusp, particle entry in the magnetosphere, sources of observed distribution functions in the magnetotail, transport of oxygen ions, self-consistent evolution of the magnetotail, substorm studies, effects of explosive reconnection, and auroral acceleration simulations.