Solar Dynamics Observatory Artist Concept

NASA Image and Video Library

2010-02-11

The Solar Dynamics Observatory SDO spacecraft, shown above the Earth as it faces toward the Sun. SDO is designed to study the influence of the Sun on the Earth and the inner solar system by studying the solar atmosphere. http://photojournal.jpl.nasa.gov/catalog/PIA18169

Communicating Solar Astronomy to the public

NASA Astrophysics Data System (ADS)

Yaji, Kentaro; Solar Observatory NAOJ, The

2015-08-01

The Sun is the nearest star to us, so that the public is greatly interested in the Sun itself and in solar activity. The Solar Observatory, National Astronomical Observatory of Japan is one of the solar research divisions. Various data of the Sun obtained with our instruments, systematically accumulated more than one hundred years since 1910s, are open to not only researchers but also the public as online database. So, we have many chances that the public request solar images for the education and the media. In addition, we release daily solar observation informations on the web and with social media and guide visitors to our observation facilities. It is reviewed about the public relations and outreach activities of the Solar Observatory, including recent solar observation topics.

OSO-7 Orbiting Solar Observatory program

NASA Technical Reports Server (NTRS)

1972-01-01

The seventh Orbiting Solar Observatory (OSO-7) in the continuing series designed to gather solar and celestial data that cannot be obtained from the earth's surface is described. OSO-7 was launched September 29, 1971. It has been highly successful in returning scientific data giving new and important information about solar flare development, coronal temperature variations, streamer dynamics of plasma flow, and solar nuclear processes. OSO-7 is expected to have sufficient lifetime to permit data comparisons with the Skylab A mission during 1973. The OSO-7 is a second generation observatory. It is about twice as large and heavy as its predecessors, giving it considerably greater capability for scientific measurements. This report reviews mission objectives, flight history, and scientific experiments; describes the observatory; briefly compares OSO-7 with the first six OSO's; and summarizes the performance of OSO-7.

The Carl Sagan solar and stellar observatories as remote observatories

NASA Astrophysics Data System (ADS)

Saucedo-Morales, J.; Loera-Gonzalez, P.

In this work we summarize recent efforts made by the University of Sonora, with the goal of expanding the capability for remote operation of the Carl Sagan Solar and Stellar Observatories, as well as the first steps that have been taken in order to achieve autonomous robotic operation in the near future. The solar observatory was established in 2007 on the university campus by our late colleague A. Sánchez-Ibarra. It consists of four solar telescopes mounted on a single equatorial mount. On the other hand, the stellar observatory, which saw the first light on 16 February 2010, is located 21 km away from Hermosillo, Sonora at the site of the School of Agriculture of the University of Sonora. Both observatories can now be remotely controlled, and to some extent are able to operate autonomously. In this paper we discuss how this has been accomplished in terms of the use of software as well as the instruments under control. We also briefly discuss the main scientific and educational objectives, the future plans to improve the control software and to construct an autonomous observatory on a mountain site, as well as the opportunities for collaborations.

Lockheed Solar Observatory and the Discovery of Moreton-Ramsey Waves

NASA Astrophysics Data System (ADS)

Tarbell, Theodore D.

2014-06-01

Moreton Waves are high-speed disturbances seen traveling away from large solar flares in H-alpha movies of the solar chromosphere. They were discovered by the observer Harry Ramsey in the late 1950s, and then published and publicized by the director Gail Moreton, both of the Lockheed Solar Observatory in the Hollywood Hills of Southern California. These efforts established the scientific reputation and secured continuing funding of the observatory, whose present-day successor is the Lockheed Martin Solar and Astrophysics Lab in Palo Alto. Moreton waves are rare, and there was limited interest in them until the EIT instrument on SOHO began seeing large numbers of similar waves in the corona in the late 1990s. The exact relation between the two observations is still a research topic today. This talk will describe some of the history of the observatory and the discovery and early interpretation of the waves.

The Coronal Solar Magnetism Observatory

NASA Astrophysics Data System (ADS)

Tomczyk, S.; Landi, E.; Zhang, J.; Lin, H.; DeLuca, E. E.

2015-12-01

Measurements of coronal and chromospheric magnetic fields are arguably the most important observables required for advances in our understanding of the processes responsible for coronal heating, coronal dynamics and the generation of space weather that affects communications, GPS systems, space flight, and power transmission. The Coronal Solar Magnetism Observatory (COSMO) is a proposed ground-based suite of instruments designed for routine study of coronal and chromospheric magnetic fields and their environment, and to understand the formation of coronal mass ejections (CME) and their relation to other forms of solar activity. This new facility will be operated by the High Altitude Observatory of the National Center for Atmospheric Research (HAO/NCAR) with partners at the University of Michigan, the University of Hawaii and George Mason University in support of the solar and heliospheric community. It will replace the current NCAR Mauna Loa Solar Observatory (http://mlso.hao.ucar.edu). COSMO will enhance the value of existing and new observatories on the ground and in space by providing unique and crucial observations of the global coronal and chromospheric magnetic field and its evolution. The design and current status of the COSMO will be reviewed.

Center for Adaptive Optics | Links

Science.gov Websites

extraterrestrische Physik, Infrared/Submillimeter Astronomy MMT Adaptive Optics Mount Wilson Observatory National Astronomical Observatory of Japan National Solar Observatory National Optical Astronomy Observatories, AO Astronomy Observatoire de Paris Osservatorio Astrofisico di Arcetri Padua Observatory Palomar Observatory

Installation package for Hyde Memorial Observatory, Lincoln, Nebraska

NASA Technical Reports Server (NTRS)

1978-01-01

Installation information for a solar heating system installed in Hyde Memorial Observatory at Lincoln, Nebraska is presented. This package included a system operation and maintenance manual, hardware brochures, schematics, system operating modes, and drawings. This prototype solar heating system consisted of the following subsystems: solar collector, control, and storage.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2017-12-08

Scientists presented the first images from NASA's Solar Dynamics Observatory [SDO] during a special "first light" press conference, Wednesday, April 21 2010, at held at the Newseum in Washington DC. Credit: NASA/GSFC

NASA Provides Coast-to-Coast Coverage of Aug. 21 Solar Eclipse (Solar Dynamics Observatory)

NASA Image and Video Library

2017-08-21

On Monday, Aug. 21, NASA provided coast-to-coast coverage of the solar eclipse across America – featuring views of the phenomenon from unique vantage points, including from the ground, from aircraft, and from spacecraft including the ISS, during a live broadcast seen on NASA Television and the agency’s website. This is footage from NASA’s Solar Dynamics Observatory.

A solar observing station for education and research in Peru

NASA Astrophysics Data System (ADS)

Kaname, José Iba, Ishitsuka; Ishitsuka, Mutsumi; Trigoso Avilés, Hugo; Takashi, Sakurai; Yohei, Nishino; Miyazaki, Hideaki; Shibata, Kazunari; Ueno, Satoru; Yumoto, Kiyohumi; Maeda, George

2007-12-01

Since 1937 Carnegie Institution of Washington made observations of active regions of the Sun with a Hale type spectro-helioscope in Huancayo observatory of the Instituto Geofísico del Perú (IGP). IGP has contributed significantly to geophysical and solar sciences in the last 69 years. Now IGP and the Faculty of Sciences of the Universidad Nacional San Luis Gonzaga de Ica (UNICA) are planning to refurbish the coelostat at the observatory with the support of National Astronomical Observatory of Japan. It is also planned to install a solar Flare Monitor Telescope (FMT) at UNICA, from Hida observatory of Kyoto University. Along with the coelostat, the FMT will be useful to improve scientific research and education.

Multiple-etalon systems for the Advanced Technology Solar Telescope

NASA Technical Reports Server (NTRS)

Gary, G. Allen; Balasubramaniam, K. S.; Sigwarth, Michael

2003-01-01

Multiple etalon systems are discussed that meet the science requirements for a narrow-passband imaging system for the 4-meter National Solar Observatory (NSO)/Advance Technology Solar Telescope (ATST). A multiple etalon system can provide an imaging interferometer that works in four distinct modes: as a spectro-polarimeter, a filter-vector magnetograph, an intermediate-band imager, and broadband high-resolution imager. Specific dual and triple etalon configurations are described that provide a spectrographic passband of 2.0-3.5 micron and reduce parasitic light levels to 10(exp -4) as required for precise polarization measurement, e.g., Zeeman measurements of magnetic sensitive lines. A TESOS-like (Telecentric Etalon SOlar Spectrometer) triple etalon system provides a spectral purity of 10(exp -5). The triple designs have the advantage of reducing the finesse requirement on each etalon; allow the use of more stable blocking filters, and have very high spectral purity. A dual-etalon double-pass (Cavallini-like) system can provide a competing configuration. Such a dual-etalon design can provide high contrast. The selection of the final focal plane instrument will depend on a trade-off between an ideal instrument and practical reality. The trade study will include the number of etalons, their aperture sizes, complexities of the optical train, number of blocking filters, configuration of the electronic control system, computer interfaces, temperature controllers, etalon controllers, and their associated feedback electronics. The heritage of single and multiple etalon systems comes from their use in several observatories, including the Marshall Space Flight Center (MSFC) Solar Observatory, Sacramento Peak Observatory (NSO), and Kiepenheuer-Institut fur Sonnenphysik (KIS, Germany), Mees Solar Observatory (University of Hawaii), and Arcetri Astrophysical Observatory (Italy). The design of the ATST multiple etalon system will benefit from the experience gained at these observatories.

Overview of Space Station attached payloads in the areas of solar physics, solar terrestrial physics, and plasma processes

NASA Technical Reports Server (NTRS)

Roberts, W. T.; Kropp, J.; Taylor, W. W. L.

1986-01-01

This paper outlines the currently planned utilization of the Space Station to perform investigations in solar physics, solar terrestrial physics, and plasma physics. The investigations and instrumentation planned for the Solar Terrestrial Observatory (STO) and its associated Space Station accommodation requirements are discussed as well as the planned placement of the STO instruments and typical operational scenarios. In the area of plasma physics, some preliminary plans for scientific investigations and for the accommodation of a plasma physics facility attached to the Space Station are outlined. These preliminary experiment concepts use the space environment around the Space Station as an unconfined plasma laboratory. In solar physics, the initial instrument complement and associated accommodation requirements of the Advanced Solar Observatory are described. The planned evolutionary development of this observatory is outlined, making use of the Space Station capabilities for servicing and instrument reconfiguration.

Solar Polarimetry: Proceedings of the National Solar Observatory/ Sacramento Peak Summer Workshop 11th Held in Sunspot, New Mexico on 27-31 August 1990

DTIC Science & Technology

1991-01-01

test at Arosa A,,t rphys- ical Observatory of the ETH Zdrich. Two beam splitters are positioned behind the mcdulat(r parkac’e if three CCD array sensors...data obtained with the Horizontal Telescope of the Arosa Astrophysical Observatory (HAT). The latter consist of simultaneous recordings of the Stokes

Current Status of Carl Sagan Observatory in Mexico

NASA Astrophysics Data System (ADS)

Sanchez-Ibarra, A.

The current status of Observatory "Carl Sagan" (OCS) of University of Sonora is presented. This project was born in 1996 focused to build a small solar-stellar observatory completely operated by remote control. The observatory will be at "Cerro Azul", a 2480 m peak in one of the best regions in the world for astronomical observation, at the Sonora-Arizona desert. The OCS, with three 16 cm solar telescopes and a 55 cm stellar telescope is one of the cheapest observatories, valuated in US200,000 Added to its scientific goals to study solar coronal holes and Supernovae Type 1A, the OCS has a strong educative and cultural program in Astronomy to all levels. At the end of 2001, we started the Program "Constelacion", to build small planetariums through all the countries with a cost of only US80,000. Also, the webcast system for transmission of the solar observations from the prototype OCS at the campus, was expanded to webcast educational programs in Astronomy since July of this year, including courses and diplomats for Latin American people. All of these advances are exposed here.

The Space-Age Legacy of Telescope Designer George A. Carroll

NASA Astrophysics Data System (ADS)

Briggs, John W.

2013-01-01

Remembered particularly as a founding member of Stony Ridge Observatory near Mount Wilson, George A. Carroll (1902-1987) was legendary in the Southern California telescope making community. In Texas at the age of sixteen, Carroll built and flew his own aircraft, becoming one of the youngest aviators in the country. He eventually became an employee of Lockheed's "Skunk Works" in Burbank. His earliest known commercial telescopes were high-end amateur instruments built by R. R. Cook. As described in a brochure describing his later telescope work, he had "experience in so many branches of technology that it is unbelievable." By the time Carroll's designs were built by Thomas Tool & Die in Sun Valley, his telescopes were well known in the solar community and in use at National Solar Observatory, Caltech, and at many other domestic and international research institutions. Among the most remarkable were large solar spars for Lockheed Solar Observatory in California and Ottawa River Solar Observatory in Canada. His instrumentation also equipped educational facilities including observatories at UCLA, Westmont College, Pasadena City College, Bevard Community College, and many others. A Carroll telescope boasting a particularly distinguished educational history was a small astrograph built in 1953 for Professor George Moyen of Hollywood and subsequently used for the long-running Summer Science Program in Ojai, California. Later solar instruments built by Carson Instruments were closely derivative of Carroll designs.

The National Solar Observatory Digital Library - a resource for space weather studies

NASA Astrophysics Data System (ADS)

Hill, F.; Erdwurm, W.; Branston, D.; McGraw, R.

2000-09-01

We describe the National Solar Observatory Digital Library (NSODL), consisting of 200GB of on-line archived solar data, a RDBMS search engine, and an Internet HTML-form user interface. The NSODL is open to all users and provides simple access to solar physics data of basic importance for space weather research and forecasting, heliospheric research, and education. The NSODL can be accessed at the URL www.nso.noao.edu/diglib.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Dean Pesnell, SDO project scientist, Goddard Space Flight Center in Greenbelt, Md. speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, Wednesday, April 21, 2010, at the Newseum in Washington. Photo Credit: (NASA/Carla Cioffi)

ON THE VARIATION OF SOLAR RADIUS IN ROTATION CYCLES

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

Qu, Z. N.; Kong, D. F.; Xiang, N. B.

2015-01-10

The Date Compensated Discrete Fourier Transform and CLEANest algorithm are used to study the temporal variations of the solar radius observed at Rio de Janeiro Observatory from 1998 March 2 to 2009 November 6. The CLEANest spectra show several significant periodicities around 400, 312, 93.5, 86.2, 79.4, 70.9, 53.2, and 26.3 days. Then, combining the data on the daily solar radius measured at Calern Observatory and Rio de Janeiro Observatory and the corresponding daily sunspot areas, we study the short-term periodicity of the solar radius and the role of magnetic field in the variation of the solar radius. The rotation periodmore » of the daily solar radius is determined to be statistically significant. Moreover, its temporal evolution is anti-phase with that of sunspot activity, and it is found anti-phase with solar activity. Generally, the stronger solar activity is, the more obvious is the anti-phase relation of radius with solar activity. This indicates that strong magnetic fields have a greater inhibitive effect than weak magnetic fields on the variation of the radius.« less

Graphics interfaces and numerical simulations: Mexican Virtual Solar Observatory

NASA Astrophysics Data System (ADS)

Hernández, L.; González, A.; Salas, G.; Santillán, A.

2007-08-01

Preliminary results associated to the computational development and creation of the Mexican Virtual Solar Observatory (MVSO) are presented. Basically, the MVSO prototype consists of two parts: the first, related to observations that have been made during the past ten years at the Solar Observation Station (EOS) and at the Carl Sagan Observatory (OCS) of the Universidad de Sonora in Mexico. The second part is associated to the creation and manipulation of a database produced by numerical simulations related to solar phenomena, we are using the MHD ZEUS-3D code. The development of this prototype was made using mysql, apache, java and VSO 1.2. based GNU and `open source philosophy'. A graphic user interface (GUI) was created in order to make web-based, remote numerical simulations. For this purpose, Mono was used, because it is provides the necessary software to develop and run .NET client and server applications on Linux. Although this project is still under development, we hope to have access, by means of this portal, to other virtual solar observatories and to be able to count on a database created through numerical simulations or, given the case, perform simulations associated to solar phenomena.

Assessment of Knowledge, Attitude, Behaviour and Interpersonal Factors Related to the Use of Tobacco among Youth of Udaipur City, Rajasthan, India: A Cross-Sectional Study

PubMed Central

Multani, Suraj; Reddy, Jaddu Jyothirmai; Bhat, Nagesh; Sharma, Ashish

2012-01-01

Background Tobacco is the most important preventable cause of disease burden and death all over the world. Apart from being the single most important determinant of cancer and cardiovascular diseases, smoking is also a threat to oral health. The Global Youth Tobacco Survey (GYTS) as a part of Global Tobacco Surveillance System (GTSS) was developed to monitor tobacco use, elicit attitudes about tobacco, and obtain information on exposure to tobacco smoke among youth. This study aimed to assess the prevalence, knowledge, attitude, behaviour and interpersonal factors related to the use of tobacco among youth of Udaipur city, Rajasthan, India. Methods This study was conducted among 1031, 15 to 25 year old youths studying in the different colleges of Udaipur city, Rajasthan, India. The Global Youth Tobacco Survey (GYTS) core questionnaire was used. Simple descriptive statistics were used for the data. Findings Out of the total 1031 participants (mean age: 19.55 ± 1.35), 632 (61.2%) were men (mean age: 19.66 ± 1.36) and 399 (38.7%) were women (mean age: 19.35 ± 1.35). 493 (47.8%) were current tobacco users, the majority of which were men 411 (39.8%). 122 (11.8%) had a previous history of tobacco use, while 416 (40.3%) reported that they had never used tobacco in any form. The majority of the men, 305 (29.5%), were consuming tobacco daily. Majority of current, 152 (30.8%), and ever tobacco users, 122 (41.8%), smoke and chew gutkha at places of entertainment followed by smoking or chewing at school/college premises. The majority of them bought gutkha themselves, 292 (47.4%). Moreover, the majority of current tobacco users, 298 (72.5%) men and 82 (100%) women, wanted to stop smoking /gutkha chewing. Conclusion The present study indicates that there is a high prevalence of use of tobacco among youth of Udaipur city, Rajasthan, India. PMID:24494149

First solar radio spectrometer deployed in Scotland, UK

NASA Astrophysics Data System (ADS)

Monstein, Christian

2012-10-01

A new Callisto solar radio spectrometer system has recently been installed and set into operation at Acre Road Observatory, a facility of University of Glasgow, Scotland UK. There has been an Observatory associated with Glasgow University since 1757, and they presently occupy two different sites. The main observatory ('Acre Road') is close to the Garscube Estate on the outskirts of the city of Glasgow. The outstation ('Cochno', housing the big 20 inch Grubb Parsons telescope) is located farther out at a darker site in the Kilpatrick Hills. The Acre Road Observatory comprises teaching and research labs, a workshop, the main dome housing the 16 inch Meade, the solar dome, presently housing the 12 inch Meade, a transit house containing the transit telescope, a 3m HI radio telescope and a 408 MHz pulsar telescope. They also have 10 and 8 inch Meade telescopes and several 5 inch Celestron instruments. There is a small planetarium beneath the solar dome. The new Callisto instrument is mainly foreseen for scientific solar burst observations as well as for student projects and for 'bad-weather' outreach activities.

Education and public outreach at the Carl Sagan Solar Observatory of the University of Sonora

NASA Astrophysics Data System (ADS)

Saucedo-Morales Julio; Loera-González, Pablo

2013-05-01

We discuss the importance of small solar observatories for EPO (Education and Public Outreach), mentioning why they are relevant and what kind of equipment and software require. We stress the fact that technological advances have made them affordable and that they should be widely available. This work is a result of our experience with one: The Carl Sagan Solar Observatory (CSSO). We briefly describe its status and the solar data obtained daily with students participation. We present examples of the data obtained in the visible, Ca II and two in Hα. Data which is widely used for education. Finally we talk about the capability for remote operation as an open invitation for collaboration in educational and scientific projects.

Education and public outreach at the Carl Sagan Solar Observatory of the University of Sonora.

PubMed

Saucedo-Morales, Julio; Loera-González, Pablo

2013-05-01

We discuss the importance of small solar observatories for EPO (Education and Public Outreach), mentioning why they are relevant and what kind of equipment and software require. We stress the fact that technological advances have made them affordable and that they should be widely available. This work is a result of our experience with one: The Carl Sagan Solar Observatory (CSSO). We briefly describe its status and the solar data obtained daily with students participation. We present examples of the data obtained in the visible, Ca II and two in Hα. Data which is widely used for education. Finally we talk about the capability for remote operation as an open invitation for collaboration in educational and scientific projects.

Education and public outreach at the Carl Sagan Solar Observatory of the University of Sonora

PubMed Central

Saucedo-Morales, Julio; Loera-González, Pablo

2013-01-01

We discuss the importance of small solar observatories for EPO (Education and Public Outreach), mentioning why they are relevant and what kind of equipment and software require. We stress the fact that technological advances have made them affordable and that they should be widely available. This work is a result of our experience with one: The Carl Sagan Solar Observatory (CSSO). We briefly describe its status and the solar data obtained daily with students participation. We present examples of the data obtained in the visible, Ca II and two in Hα. Data which is widely used for education. Finally we talk about the capability for remote operation as an open invitation for collaboration in educational and scientific projects. PMID:25685436

Solar Dynamics Observatory Briefing

NASA Image and Video Library

2010-01-21

Madhulika Guhathakurta, SDO Program Scientist, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

The Helioseismic and Magnetic Imager (HMI) Investigation for the Solar Dynamics Observatory (SDO)

NASA Technical Reports Server (NTRS)

Scherrer, Philip Hanby; Schou, Jesper; Bush, R. I.; Kosovichev, A. G.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.; Duvall, T. L., Jr.; Zhao, J.; Title, A. M.;

Multiple Etalon Systems for the Advanced Technology Solar Telescope

NASA Technical Reports Server (NTRS)

Gary, G. Allen; Balasubramaniam, K. S.; Sigwarth, Michael; Six, N. Frank (Technical Monitor)

2002-01-01

Multiple etalons systems are discussed that meet the 4-meter NSO/Advance Technology Solar Telescope (http://www.nso.edu/ATST/index.html) instrument and science requirements for a narrow bandpass imaging system. A multiple etalon system can provide an imaging interferometer working in four distinct modes: as a spectro-polarimeter, a filter-vector magnetograph, and a wide-band and broad-band high-resolution imager. Specific dual and triple etalon configurations will be described that provides spectrographic passband of 2.0-3.5nm and reduces parasitic light levels to 1/10000 as required by precise polarization measurement, e.g., Zeeman measurements of magnetic sensitive lines. A TESOS-like triple etalon system provides for spectral purity of 100 thousandths. The triple designs have the advantage of reducing the finesse requirement on each etalon, allowing much more stable blocking filters, and can have very high spectral purity. A dual-etalon double-pass Cavallini-like configuration can provide a competing configuration. This design can provide high contrast with only a double etalon. The selection of the final focal plan instrument will depend on a trade-off of the ideal instrument versus reality, the number of etalons, the aperture of etalons, the number of blocking filters the electronic control system and computer interfaces, the temperature control and controllers for the etalons and the electronics. The use of existing experience should provide significant cost savings. The heritage of use of etalons and multiple etalon systems in solar physics come from a number of observatories, which includes MSFC Solar Observatory (NASA), Sac Peak Observatory (NSO), and Kiepenheuer Institute for Solar Physics (Germany), Mees Solar Observatory (University of Hawaii), and Arcetri Astrophysical Observatory (Italy). The design of the ATST multiple etalon system will reply on the existing experience from these observatories.

International ultraviolet explorer solar array power degradation

NASA Technical Reports Server (NTRS)

Day, J. H., Jr.

1983-01-01

The characteristic electrical performance of each International Ultraviolet Explorer (IUE) solar array panel is evaluated as a function of several prevailing variables (namely, solar illumination, array temperature and solar cell radiation damage). Based on degradation in the current-voltage characteristics of the array due to solar cell damage accumulated over time by space charged particle radiations, the available IUE solar array power is determined for life goals up to 10 years. Best and worst case calculations are normalized to actual IUE flight data (available solar array power versus observatory position) to accurately predict the future IUE solar array output. It is shown that the IUE solar array can continue to produce more power than is required at most observatory positions for at least 5 more years.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2017-12-08

Scientists presented the first images from NASA's Solar Dynamics Observatory [SDO] during a special "first light" press conference, Wednesday, April 21 2010, at held at the Newseum in Washington DC. Here, scientists are showing an animation from Walt Feimer, lead animator for the Heliophysics team. Credit: NASA/GSFC

Solar Dynamics Observatory Briefing

NASA Image and Video Library

2010-01-21

Richard Fisher, Heliophysics Division Director at NASA Headquarters, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

Solar observations carried out at the INAF - Catania Astrophysical Observatory

NASA Astrophysics Data System (ADS)

Zuccarello, F.; Contarino, L.; Romano, P.

2011-10-01

Solar observations at the INAF - Catania Astrophysical Observatory are carried out by means of an equatorial spar, which includes: a Cook refractor, used to make daily drawings of sunspot groups from visual observations; a 150-mm refractor with an Hα Lyot filter for chromospheric observations; a 150-mm refractor feeding an Hα Halle filter for limb observations of the chromosphere. The photospheric and chromospheric data are daily distributed to several international Solar Data Centers. Recently, a program of Flare Warning has been implemented, with the aim of determining the probability that an active region yields a flare on the basis of its characteristics deduced from optical observations. Some science results obtained by means of solar data acquired at the INAF - Catania Astrophysical Observatory, as well as by space-instruments data, are briefly described.

NASA Marshall Space Flight Center solar observatory report, January - June 1991

NASA Technical Reports Server (NTRS)

Smith, James E.

1991-01-01

Given here is a summary of the solar vector magnetic field, H-alpha, and white-light observations made at the NASA/Marshall Space Flight Center (MSFC) Solar Observatory during its daily periods of operation. The MSFC Solar Observatory facilities consist of the Solar Magnetograph, an f/13, 30-cm Cassegrain system with a 3.5-cm image of the Sun, housed on top of a 12.8-meter tower; a 12.5-cm Razdow H-alpha telescope housed at the base of the tower; an 18-cm Questar telescope with a full aperture white-light filter mounted at the base of the tower; a 30-cm Cassegrain telescope located in a second metal dome; and a 16.5-cm H-alpha telescope mounted on side of the Solar Vector Magnetograph. A concrete block building provides office space, a darkroom for developing film and performing optical testing, a workshop, video displays, and a computer facility for data reduction.

NASA Marshall Space Flight Center Solar Observatory report, July - December 1991

NASA Technical Reports Server (NTRS)

Smith, James E.

1992-01-01

A summary is given of the solar vector magnetic field, H-alpha, and white light observations made at the NASA/Marshall Space Flight Center (MSFC) Solar Observatory during its daily periods of observation. The MSFC Solar Observatory facilities consist of the Solar Magnetograph, an f-13, 30 cm Cassegrain system with a 3.5 cm image of the Sun housed on top of a 12.8 meter tower, a 12.5 cm Razdow H-alpha telescope housed at the base of the tower, an 18 cm Questar telescope with a full aperture white-light filter mounted at the base of the tower, a 30 cm Cassegrain telescope located in a second metal dome, and a 16.5 cm H-alpha telescope mounted on the side of the Solar Vector Magnetograph. A concrete block building provides office space, a darkroom for developing film and performing optical testing, a workshop, video displays, and a computer facility for data reduction.

Analysis of Supergranule Sizes and Velocities Using Solar Dynamics Observatory (SDO)/Helioseismic Magnetic Imager (HMI) and Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI) Dopplergrams

NASA Technical Reports Server (NTRS)

Williams, Peter E.; Pesnell, W. Dean; Beck, John G.; Lee, Shannon

2013-01-01

Co-temporal Doppler images from Solar and Heliospheric Observatory (SOHO)/ Michelson Doppler Imager (MDI) and Solar Dynamics Observatory (SDO)/Helioseismic Magnetic Imager (HMI) have been analyzed to extract quantitative information about global properties of the spatial and temporal characteristics of solar supergranulation. Preliminary comparisons show that supergranules appear to be smaller and have stronger horizontal velocity flows within HMI data than was measured with MDI. There appears to be no difference in their evolutionary timescales. Supergranule sizes and velocities were analyzed over a ten-day time period at a 15-minute cadence. While the averages of the time-series retain the aforementioned differences, fluctuations of these parameters first observed in MDI data were seen in both MDI and HMI time-series, exhibiting a strong cross-correlation. This verifies that these fluctuations are not instrumental, but are solar in origin. The observed discrepancies between the averaged values from the two sets of data are a consequence of instrument resolution. The lower spatial resolution of MDI results in larger observed structures with lower velocities than is seen in HMI. While these results offer a further constraint on the physical nature of supergranules, they also provide a level of calibration between the two instruments.

On the Origin of the Solar Moreton Wave of 2006 December 6

DTIC Science & Technology

2010-11-01

Flight Center. Huntsville. AL 35812. USA 9 National Solar Observatory. Tucson, AZ 85719, USA 10 Faculty of Geodesy, University of Zagreb , Hvar...Observatory, HR 10000 Zagreb , Croatia 1’ Space Vehicles Directorate, Air Force Research Laboratory, Kirtland AFB, NM 87117, US A Received 2010 April 7

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Tom Woods, (second from right), principal investigator, Extreme Ultraviolet Variability Experiment instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, Wednesday, April 21, 2010, at the Newseum in Washington. Photo Credit: (NASA/Carla Cioffi)

A continued program of planetary study at the University of Texas McDonald Observatory

NASA Technical Reports Server (NTRS)

Trafton, L.

1991-01-01

The program conducts solar system research in support of NASA missions and of general astronomical interest. Investigations of composition, physical characteristics and changes in solar system bodies are conducted primarily using the facilities of McDonald Observatory. Progress, accomplishments, and projected accomplishments are discussed.

Factors influencing caries status and treatment needs among pregnant women attending a maternity hospital in Udaipur city, India.

PubMed

Kumar, Santhosh; Tadakamadla, Jyothi; Tibdewal, Harish; Duraiswamy, Prabu; Kulkarni, Suhas

2013-04-01

To estimate the prevalence and severity of dental caries along with the treatment needs; to determine the factors that influence dental caries status among pregnant women attending a district maternity hospital in Udaipur, India. Study sample comprised of 206 pregnant women attending a district maternity hospital in Udaipur, India. Clinical data were collected on dental caries by DMFT and treatment needs as described in World Health Organization Dentition status and Treatment needs. The overall caries prevalence was 87%. Mean caries experience differed significantly among women in various trimesters, it was found to be 3.59 and 3.00 in 1st and 2nd trimester subjects respectively while it was greatest (4.13) among those in 3rd trimester. One surface filling was the most predominant treatment need. Age and occupation of husband explained a variance of 6.8% and 4.2% for decayed and filled components respectively while the only predictor for missing teeth and DMFT that explained a variance of 9.6% and 5.7% respectively was trimester of pregnancy. Dental caries experience and the need for one surface restoration increased with age. Trimester of pregnancy was a significant predictor for missing teeth and DMFT, while decayed teeth and filled teeth were influenced by age and socio-economic level respectively. Key words:Dental caries, treatment needs, pregnant, age, trimester.

Factors influencing caries status and treatment needs among pregnant women attending a maternity hospital in Udaipur city, India

PubMed Central

Tadakamadla, Jyothi; Tibdewal, Harish; Duraiswamy, Prabu; Kulkarni, Suhas

2013-01-01

Objectives: To estimate the prevalence and severity of dental caries along with the treatment needs; to determine the factors that influence dental caries status among pregnant women attending a district maternity hospital in Udaipur, India. Study design: Study sample comprised of 206 pregnant women attending a district maternity hospital in Udaipur, India. Clinical data were collected on dental caries by DMFT and treatment needs as described in World Health Organization Dentition status and Treatment needs. Results: The overall caries prevalence was 87%. Mean caries experience differed significantly among women in various trimesters, it was found to be 3.59 and 3.00 in 1st and 2nd trimester subjects respectively while it was greatest (4.13) among those in 3rd trimester. One surface filling was the most predominant treatment need. Age and occupation of husband explained a variance of 6.8% and 4.2% for decayed and filled components respectively while the only predictor for missing teeth and DMFT that explained a variance of 9.6% and 5.7% respectively was trimester of pregnancy. Conclusions: Dental caries experience and the need for one surface restoration increased with age. Trimester of pregnancy was a significant predictor for missing teeth and DMFT, while decayed teeth and filled teeth were influenced by age and socio-economic level respectively. Key words:Dental caries, treatment needs, pregnant, age, trimester. PMID:24455060

Atmospheric Extinction Coefficients in the Ic Band for Several Major International Observatories: Results from the BiSON Telescopes, 1984-2016

NASA Astrophysics Data System (ADS)

Hale, S. J.; Chaplin, W. J.; Davies, G. R.; Elsworth, Y. P.; Howe, R.; Lund, M. N.; Moxon, E. Z.; Thomas, A.; Pallé, P. L.; Rhodes, E. J., Jr.

2017-09-01

Over 30 years of solar data have been acquired by the Birmingham Solar Oscillations Network (BiSON), an international network of telescopes used to study oscillations of the Sun. Five of the six BiSON telescopes are located at major observatories. The observational sites are, in order of increasing longitude: Mount Wilson (Hale) Observatory (MWO), California, USA; Las Campanas Observatory, Chile; Observatorio del Teide, Izaña, Tenerife, Canary Islands; the South African Astronomical Observatory, Sutherland, South Africa; Carnarvon, Western Australia; and the Paul Wild Observatory, Narrabri, New South Wales, Australia. The BiSON data may be used to measure atmospheric extinction coefficients in the {{{I}}}{{c}} band (approximately 700-900 nm), and presented here are the derived atmospheric extinction coefficients from each site over the years 1984-2016.

Close Binary Star Speckle Interferometry on the McMath-Pierce 0.8-Meter Solar Telescope

NASA Astrophysics Data System (ADS)

Wiley, Edward; Harshaw, Richard; Jones, Gregory; Branston, Detrick; Boyce, Patrick; Rowe, David; Ridgely, John; Estrada, Reed; Genet, Russell

2015-09-01

Observations were made in April 2014 to assess the utility of the 0.8-meter solar telescope at the McMath-Pierce Solar Observatory at Kitt Peak National Observatory for performing speckle interferometry observations of close binary stars. Several configurations using science cameras, acquisition cameras, eyepieces, and flip mirrors were evaluated. Speckle images were obtained and recommendations for further improvement of the acquisition system are presented.

Toward a Virtual Solar Observatory: Starting Before the Petabytes Fall

NASA Technical Reports Server (NTRS)

Gurman, J. B.; Fisher, Richard R. (Technical Monitor)

2002-01-01

NASA is currently engaged in the study phase of a modest effort to establish a Virtual Solar Observatory (VSO). The VSO would serve ground- and space-based solar physics data sets from a distributed network of archives through a small number of interfaces to the scientific community. The basis of this approach, as of all planned virtual observatories, is the translation of metadata from the various sources via source-specific dictionaries so the user will not have to distinguish among keyword usages. A single Web interface should give access to all the distributed data. We present the current status of the VSO, its initial scope, and its relation to the European EGSO effort.

Results of Spectral Corona Observations in Solar Activity Cycles 17-24

NASA Astrophysics Data System (ADS)

Aliev, A. Kh.; Guseva, S. A.; Tlatov, A. G.

2017-12-01

The results of the work of the global observation network are considered, and a comparative analysis of the data of various coronal observatories is performed. The coronal activity index has been reconstructed for the period 1939-2016 based on the data of various observatories in Kislovodsk system. For this purpose, the corona daily intensity maps from the Sacramento Peak and Lomnický Štít observatories according to the Solar-Geophysical Data journal have been digitized; they supplement the data of other observatories. The homogeneity and continuity of the corona observations at the Kislovodsk station, including activity cycle 24, is confirmed. Unfortunately, the only observatory at present that continues observation of the spectral corona in Fe XIV 5303 Å and Fe XIV 6374 Å lines is the Kislovodsk astronomical station Mountain Astronomical Station (MAS) of the Central Astronomical Observatory, Russian Academy of Sciences (Pulkovo). The data on the combined corona in 5303 Å line are analyzed. It is shown that there is a high correlation of the intensity index of green corona with solar radiation measurements in the vacuum UV region. Data on the beginning of the new 25th activity cycle in the corona at high latitudes are presented.

Astrophysics from the moon; Proceedings of the Workshop, Annapolis, MD, Feb. 5-7, 1990

NASA Technical Reports Server (NTRS)

Mumma, Michael J. (Editor); Smith, Harlan J. (Editor)

1990-01-01

The present conference on astrophysics from the moon encompasses the study of the Galaxy, external planetary systems, solar physics, stars and stellar evolution, the frontiers of Galactic, extragalactic, and cosmological astronomy, an introduction to lunar-based astronomy, concepts for lunar observatories including high-energy observatories, solar observatories, and observatories for particle astrophysics and gravitational studies. Specific issues addressed include the dynamics of Jovian atmospheres, planetary magnetospheres, flare physics, exobiology and SETI from the lunar farside, and the study of interactive stars, star formation, H II regions in absorption at low frequencies, and normal galaxies. Also addressed are the potential lunar investigation of quasars, the formation epoch, and the large-scale structure of the universe, and observational issues related to X-ray large arrays, optical interferometers, VLF radio astronomy, a UV-solar reflecting coronagraph, and a heavy-nucleus detector.

Solar Dynamics Observatory Briefing

NASA Image and Video Library

2010-01-21

Richard Fisher, Heliophysics Division Director at NASA Headquarters, left, speaks during a briefing to discuss the upcoming launch of NASA's Solar Dynamic Observatory, or SDO, Thursday, Jan. 21, 2010, as Madhulika Guhathakurta, SDO Program Scientist looks on at NASA Headquarters in Washington. The mission is to study the Sun and its dynamic behavior. Photo Credit: (NASA/Paul E. Alers)

ATM photoheliograph. [at a solar observatory

NASA Technical Reports Server (NTRS)

Prout, R. A.

1975-01-01

The design and fabrication are presented of a 65 cm photoheliograph functional verification unit (FVU) installed in a major solar observatory. The telescope is used in a daily program of solar observation while serving as a test bed for the development of instrumentation to be included in early space shuttle launched solar telescopes. The 65 cm FVU was designed to be mechanically compatible with the ATM spar/canister and would be adaptable to a second ATM flight utilizing the existing spar/canister configuration. An image motion compensation breadboard and a space-hardened, remotely tuned H alpha filter, as well as solar telescopes of different optical configurations or increased aperture are discussed.

The Observatory as Laboratory: Spectral Analysis at Mount Wilson Observatory

NASA Astrophysics Data System (ADS)

Brashear, Ronald

2018-01-01

This paper will discuss the seminal changes in astronomical research practices made at the Mount Wilson Observatory in the early twentieth century by George Ellery Hale and his staff. Hale’s desire to set the agenda for solar and stellar astronomical research is often described in terms of his new telescopes, primarily the solar tower observatories and the 60- and 100-inch telescopes on Mount Wilson. This paper will focus more on the ancillary but no less critical parts of Hale’s research mission: the establishment of associated “physical” laboratories as part of the observatory complex where observational spectral data could be quickly compared with spectra obtained using specialized laboratory equipment. Hale built a spectroscopic laboratory on the mountain and a more elaborate physical laboratory in Pasadena and staffed it with highly trained physicists, not classically trained astronomers. The success of Hale’s vision for an astronomical observatory quickly made the Carnegie Institution’s Mount Wilson Observatory one of the most important astrophysical research centers in the world.

Lockyer, Joseph Norman (1836-1920)

NASA Astrophysics Data System (ADS)

Murdin, P.

2000-11-01

Civil servant, professor at the Solar Physics Observatory, Kensington (later moved to Cambridge), born in Rugby, Warwickshire, England. Attracted to astronomy by an observation of the annular solar eclipse of 1858, erected an observatory at his home in Hampstead, observed Mars. Lockyer showed spectroscopically that phenomena seen during a total eclipse (such as the prominences) could be seen in d...

The IRIS network site at the Wilcox Solar Observatory

NASA Technical Reports Server (NTRS)

Hoeksema, J. T.; Scherrer, P. H.

1991-01-01

The site for the International Research on the Interior of the Sun (IRIS) instrument housed at the Wilcox Solar Observatory at Stanford University (near San Francisco, USA) is described together with the instrument operation procedure. The IRIS instrument, which measures global oscillations of the sun, operates continuously every clear day since it was installed in August 1987.

Still Virtual After All These Years: Recent Developments in the Virtual Solar Observatory

NASA Astrophysics Data System (ADS)

Gurman, J. B.; Bogart, R. S.; Davey, A. R.; Hill, F.; Martens, P. C.; Zarro, D. M.; Team, T. v.

2008-05-01

While continuing to add access to data from new missions, including Hinode and STEREO, the Virtual Solar Observatory is also being enhanced as a research tool by the addition of new features such as the unified representation of catalogs and event lists (to allow joined searches in two or more catalogs) and workable representation and manipulation of large numbers of search results (as are expected from the Solar Dynamics Observatory database). Working with our RHESSI colleagues, we have also been able to improve the performance of IDL-callable vso_search and vso_get functions, to the point that use of those routines is a practical alternative to reproducing large subsets of mission data on one's own LAN.

Still Virtual After All These Years: Recent Developments in the Virtual Solar Observatory

NASA Technical Reports Server (NTRS)

Gurman, Joseph B.; Bogart; Davey; Hill; Masters; Zarro

2008-01-01

While continuing to add access to data from new missions, including Hinode and STEREO, the Virtual Solar Observatory is also being enhanced as a research tool by the addition of new features such as the unified representation of catalogs and event lists (to allow joined searches in two or more catalogs) and workable representation and manipulation of large numbers of search results (as are expected from the Solar Dynamics Observatory database). Working with our RHESSI colleagues, we have also been able to improve the performance of IDL-callable vso_search and vso_get functions, to the point that use of those routines is a practical alternative to reproducing large subsets of mission data on one's own LAN.

Keele Observatory

NASA Astrophysics Data System (ADS)

Theodorus van Loon, Jacco; Albinson, James; Bagnall, Alan; Bryant, Lian; Caisley, Dave; Doody, Stephen; Johnson, Ian; Klimczak, Paul; Maddison, Ron; Robinson, StJohn; Stretch, Matthew; Webb, John

2015-08-01

Keele Observatory was founded by Dr. Ron Maddison in 1962, on the hill-top campus of Keele University in central England, hosting the 1876 Grubb 31cm refractor from Oxford Observatory. It since acquired a 61cm research reflector, a 15cm Halpha solar telescope and a range of other telescopes. Run by a group of volunteering engineers and students under directorship of a Keele astrophysicist, it is used for public outreach as well as research. About 4,000 people visit the observatory every year, including a large number of children. We present the facility, its history - including involvement in the 1919 Eddington solar eclipse expedition which proved Albert Einstein's theory of general relativity - and its ambitions to erect a radio telescope on its site.

KSC-06pd1229

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., technicians prepare to deploy the solar panel on the STEREO observatory "A." STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

KSC-06pd1233

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., the deployed solar panel on the STEREO observatory "A" undergoes testing. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

KSC-06pd1232

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., engineers perform testing on the solar panel on the STEREO observatory "A." STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

KSC-06pd1231

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., the deployed solar panel on the STEREO observatory "A" undergoes testing. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

The Virtual Solar-Terrestrial Observatory; access to and use of diverse solar and solar- terrestrial data.

NASA Astrophysics Data System (ADS)

Fox, P.; McGuinness, D.; Cinquini, L.; West, P.; Garcia, J.; Zednik, S.; Benedict, J.

2008-05-01

This presentation will demonstrate how users and other data providers can utilize the Virtual Solar-Terrestrial Observatory (VSTO) to find, access and use diverse data holdings from the disciplines of solar, solar-terrestrial and space physics. VSTO provides a web portal, web services and a native applications programming interface for various levels of users. Since these access methods are based on semantic web technologies and refer to the VSTO ontology, users also have the option of taking advantage of value added services when accessing and using the data. We present example of both conventional use of VSTO as well as the advanced semantics use. Finally, we present our future directions for VSTO and semantic data frameworks in general.

The Virtual Solar-Terrestrial Observatory; access to and use of diverse solar and solar-terrestrial data

NASA Astrophysics Data System (ADS)

Fox, P.

2007-05-01

This presentation will demonstrate how users and other data providers can utilize the Virtual Solar-Terrestrial Observatory (VSTO) to find, access and use diverse data holdings from the disciplines of solar, solar-terrestrial and space physics. VSTO provides a web portal, web services and a native applications programming interface for various levels of users. Since these access methods are based on semantic web technologies and refer to the VSTO ontology, users also have the option of taking advantage of value added services when accessing and using the data. We present example of both conventional use of VSTO as well as the advanced semantics use. Finally, we present our future directions for VSTO and semantic data frameworks in general.

Statistical analysis of geomagnetic field variations during solar eclipses

NASA Astrophysics Data System (ADS)

Kim, Jung-Hee; Chang, Heon-Young

2018-04-01

We investigate the geomagnetic field variations recorded by INTERMAGNET geomagnetic observatories, which are observed while the Moon's umbra or penumbra passed over them during a solar eclipse event. Though it is generally considered that the geomagnetic field can be modulated during solar eclipses, the effect of the solar eclipse on the observed geomagnetic field has proved subtle to be detected. Instead of exploring the geomagnetic field as a case study, we analyze 207 geomagnetic manifestations acquired by 100 geomagnetic observatories during 39 solar eclipses occurring from 1991 to 2016. As a result of examining a pattern of the geomagnetic field variation on average, we confirm that the effect can be seen over an interval of 180 min centered at the time of maximum eclipse on a site of a geomagnetic observatory. That is, demonstrate an increase in the Y component of the geomagnetic field and decreases in the X component and the total strength of the geomagnetic field. We also find that the effect can be overwhelmed, depending more sensitively on the level of daily geomagnetic events than on the level of solar activity and/or the phase of solar cycle. We have demonstrated it by dividing the whole data set into subsets based on parameters of the geomagnetic field, solar activity, and solar eclipses. It is suggested, therefore, that an evidence of the solar eclipse effect can be revealed even at the solar maximum, as long as the day of the solar eclipse is magnetically quiet.

The Solar Dynamics Observatory, Studying the Sun and Its Influence on Other Bodies in the Solar System

NASA Technical Reports Server (NTRS)

Chamberlin, P. C.

2011-01-01

The solar photon output, which was once thought to be constant, varies over all time scales from seconds during solar flares to years due to the solar cycle. These solar variations cause significant deviations in the Earth and space environments on similar time scales, such as affecting the atmospheric densities and composition of particular atoms, molecules, and ions in the atmospheres of the Earth and other planets. Presented and discussed will be examples of unprecedented observations from NASA's new solar observatory, the Solar Dynamics Observatory (SDO). Using three specialized instruments, SDO measures the origins of solar activity from inside the Sun, though its atmosphere, then accurately measuring the Sun's radiative output in X-ray and EUV wavelengths (0.1-121 nm). Along with the visually appealing observations will be discussions of what these measurements can tell us about how the plasma motions in all layers of the Sun modifies and strengthens the weak solar dipole magnetic field to drive large energy releases in solar eruptions. Also presented will be examples of how the release of the Sun's energy, in the form of photons and high energy particles, physically influence other bodies in the solar system such as Earth, Mars, and the Moon, and how these changes drive changes in the technology that we are becoming dependent upon. The presentation will continuously emphasize how SDO, the first satellite in NASA's Living with a Star program, improving our understanding of the variable Sun and its Heliospheric influence.

The diverse utility of ground-based magnetometer data

NASA Astrophysics Data System (ADS)

Love, J. J.

2012-12-01

The global network of magnetic observatories represents a unique collective asset for the scientific community. Since observatory data record a wide range of physical phenomena, they are also used for a wide range of applications. Historically, magnetic observatories were first established in the 19th century to support global magnetic-field mapping projects, and this application continues to be important today. But since the dawn of the space age and the International Geophysical Year, observatory data have become important for research analysis of the ionosphere, the magnetosphere, and, indirectly, the heliosphere. Over the past couple of solar cycles, magnetic observatories have also played an important role in real-time operational monitoring of the changing conditions of space weather and assessment of ground-level geomagnetic hazards. This diversification and expansion of the observatory-data user community has brought demands for data that meet new and more stringent standards. In cooperation with the many institutes that support magnetic observatories, INTERMAGNET has been helping to coordinate and facilitate observatory modernization and improved operation. In this presentation, we give an overview of the diversity of signals recorded in observatory data, including secular, quiet, storm-time, and solar-cycle variations. We discuss future opportunities, especially for global integration and data sharing.

NASA's SDO Sees a Solar Flare and a Lunar Transit

NASA Image and Video Library

2017-12-08

A solar flare erupts on Jan. 30, 2014, as seen by the bright flash on the left side of the sun, captured here by NASA's Solar Dynamics Observatory. In the lower right corner the moon can be seen, having just passed between the observatory and the sun. --- The sun emitted a mid-level solar flare, peaking at 11:11 a.m. EST on Jan. 30, 2014. Images of the flare were captured by NASA's Solar Dynamics Observatory, or SDO, shortly after the observatory witnessed a lunar transit. The black disk of the moon can be seen in the lower right of the images. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however -- when intense enough -- they can disturb the atmosphere in the layer where GPS and communications signals travel. To see how this event may impact Earth, please visit NOAA's Space Weather Prediction Center at spaceweather.gov, the U.S. government's official source for space weather forecasts, alerts, watches and warnings. This flare is classified as an M6.6 class flare. Updates will be provided as needed. Credit: NASA/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

VICE PRESIDENT PENCE VIEWS SOLAR ECLIPSE WITH STUDENTS AT U.S. NAVAL OBSERVATORY

NASA Image and Video Library

2017-08-21

On Monday, Aug. 21, Vice President Mike Pence welcomed students from a Washington area school to the U.S. Naval Observatory, to view the 2017 solar eclipse and learn about heliophysics – the study of our sun. The event was also attended by former NASA astronaut Pam Melroy, NASA scientist Brad Bailey, and education specialist Evelina Felicite-Maurice.

Advanced Solar Observatory (ASO) accommodations requirements study

NASA Technical Reports Server (NTRS)

1989-01-01

Results of an accommodations analysis for the Advanced Solar Observatory on Space Station Freedom are reported. Concepts for the High Resolution Telescope Cluster, Pinhole/Occulter Facility, and High Energy Cluster were developed which can be accommodated on Space Station Freedom. It is shown that workable accommodations concepts are possible. Areas of emphasis for the next stage of engineering development are identified.

The Virtual Solar Observatory: What Are We Up To Now?

NASA Technical Reports Server (NTRS)

Gurman, J. B.; Hill, F.; Suarez-Sola, F.; Bogart, R.; Amezcua, A.; Martens, P.; Hourcle, J.; Hughitt, K.; Davey, A.

2012-01-01

In the nearly ten years of a functional Virtual Solar Observatory (VSO), http://virtualsolar.org/ we have made it possible to query and access sixty-seven distinct solar data products and several event lists from nine spacecraft and fifteen observatories or observing networks. We have used existing VSO technology, and developed new software, for a distributed network of sites caching and serving SDO HMI and/ or AlA data. We have also developed an application programming interface (API) that has enabled VSO search and data access capabilities in IDL, Python, and Java. We also have quite a bit of work yet to do, including completion of the implementation of access to SDO EVE data, and access to some nineteen other data sets from space- and ground-based observatories. In addition, we have been developing a new graphic user interface that will enable the saving of user interface and search preferences. We solicit advice from the community input prioritizing our task list, and adding to it

KSC-06pd1538

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - In the hazardous processing facility at Astrotech Space Operations in Titusville, Fla., technicians check Observatory A before lifting onto a scale for weight measurements. The observatory is one of two in the STEREO spacecraft and later will be fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/Jack Pfaller

KSC-06pd1798

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers guide one of the STEREO observatories as it is lowered toward the other observatory. They will be mated for launch. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

KSC-06pd1793

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers prepare one of the STEREO observatories that will be lifted and moved. It will be mated to the other observatory, in the background, for launch. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

KSC-06pd1796

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., one of the STEREO observatories is lifted and moved toward the other observatory, in the background. They will be mated for launch. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

KSC-06pd1797

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers guide one of the STEREO observatories as it is lowered toward the other observatory. They will be mated for launch. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

KSC-06pd1795

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., one of the STEREO observatories is lifted and moved toward the other observatory, in the background. They will be mated for launch. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

A National Solar Digital Observatory

NASA Astrophysics Data System (ADS)

Hill, F.

2000-05-01

The continuing development of the Internet as a research tool, combined with an improving funding climate, has sparked new interest in the development of Internet-linked astronomical data bases and analysis tools. Here I outline a concept for a National Solar Digital Observatory (NSDO), a set of data archives and analysis tools distributed in physical location at sites which already host such systems. A central web site would be implemented from which a user could search all of the component archives, select and download data, and perform analyses. Example components include NSO's Digital Library containing its synoptic and GONG data, and the forthcoming SOLIS archive. Several other archives, in various stages of development, also exist. Potential analysis tools include content-based searches, visualized programming tools, and graphics routines. The existence of an NSDO would greatly facilitate solar physics research, as a user would no longer need to have detailed knowledge of all solar archive sites. It would also improve public outreach efforts. The National Solar Observatory is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation.

Selection of astrophysical/astronomical/solar sites at the Argentina East Andes range taking into account atmospheric components

NASA Astrophysics Data System (ADS)

Piacentini, R. D.; García, B.; Micheletti, M. I.; Salum, G.; Freire, M.; Maya, J.; Mancilla, A.; Crinó, E.; Mandat, D.; Pech, M.; Bulik, T.

2016-06-01

In the present work we analyze sites in the Argentinian high Andes mountains as possible places for astrophysical/astronomical/solar observatories. They are located at: San Antonio de los Cobres (SAC) and El Leoncito/CASLEO region: sites 1 and 2. We consider the following atmospheric components that affect, in different and specific wavelength ranges, the detection of photons of astronomical/astrophysical/solar origin: ozone, microscopic particles, precipitable water and clouds. We also determined the atmospheric radiative transmittance in a day near the summer solstice at noon, in order to confirm the clearness of the sky in the proposed sites at SAC and El Leoncito. Consequently, all the collected and analyzed data in the present work, indicate that the proposed sites are very promising to host astrophysical/astronomical/solar observatories. Some atmospheric components, like aerosols, play a significant role in the attenuation of light (Cherencov and/or fluorescence) detected in cosmic rays (particles or gamma photons) astrophysical observatories, while others, like ozone have to be considered in astronomical/solar light detection.

``Route of astronomical observatories'' project: Classical observatories from the Renaissance to the rise of astrophysics

NASA Astrophysics Data System (ADS)

Wolfschmidt, Gudrun

2016-10-01

Observatories offer a good possibility for serial transnational applications. For example one can choose groups like baroque or neoclassical observatories, solar physics observatories or a group of observatories equipped with the same kind of instruments or made by famous firms. I will discuss what has been achieved and show examples, like the route of astronomical observatories, the transition from classical astronomy to modern astrophysics. I will also discuss why the implementation of the World Heritage & Astronomy initiative is difficult and why there are problems to nominate observatories for election in the national tentative lists.

KSC-06pd1228

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., technicians remove the protective cover on the solar panel on the STEREO observatory "A" before deployment and testing. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

Laboratory study supporting the interpretation of Solar Dynamics Observatory data

DOE PAGES

Trabert, E.; Beiersdorfer, P.

2015-01-29

High-resolution extreme ultraviolet spectra of ions in an electron beam ion trap are investigated as a laboratory complement of the moderate-resolution observation bands of the AIA experiment on board the Solar Dynamics Observatory (SDO) spacecraft. Here, the latter observations depend on dominant iron lines of various charge states which in combination yield temperature information on the solar plasma. Our measurements suggest additions to the spectral models that are used in the SDO data interpretation. In the process, we also note a fair number of inconsistencies among the wavelength reference data bases.

The Virtual Solar Observatory: Progress and Diversions

NASA Astrophysics Data System (ADS)

Gurman, Joseph B.; Bogart, R. S.; Amezcua, A.; Hill, Frank; Oien, Niles; Davey, Alisdair R.; Hourcle, Joseph; Mansky, E.; Spencer, Jennifer L.

2017-08-01

The Virtual Solar Observatory (VSO) is a known and useful method for identifying and accessing solar physics data online. We review current "behind the scenes" work on the VSO, including the addition of new data providers and the return of access to data sets to which service was temporarily interrupted. We also report on the effect on software development efforts when government IT “security” initiatives impinge on finite resoruces. As always, we invite SPD members to identify data sets, services, and interfaces they would like to see implemented in the VSO.

KSC-06pd1230

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., the solar panel on the STEREO observatory "A" has been deployed for testing. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

Coordination of Advanced Solar Observatory (ASO) Science Working Group (SWG) for the study of instrument accommodation and operational requirements on space station

NASA Technical Reports Server (NTRS)

Wu, S. T.

1989-01-01

The objectives are to coordinate the activities of the Science Working Group (SWG) of the Advanced Solar Observatory (ASO) for the study of instruments accommodation and operation requirements on board space station. In order to facilitate the progress of the objective, two conferences were organized, together with two small group discussions.

The Sudbury Neutrino Observatory

DOE PAGES

Bellerive, Alain; Klein, J. R.; McDonald, A. B.; ...

2016-04-27

This review paper provides a summary of the published results of the Sudbury Neutrino Observatory (SNO) experiment that was carried out by an international scientific collaboration with data collected during the period from 1999 to 2006. By using heavy water as a detection medium, the SNO experiment demonstrated clearly that solar electron neutrinos from 8B decay in the solar core change into other active neutrino flavors in transit to Earth. The reaction on deuterium that has equal sensitivity to all active neutrino flavors also provides a very accurate measure of the initial solar flux for comparison with solar models. Thismore » review summarizes the results from three phases of solar neutrino detection as well as other physics results obtained from analyses of the SNO data.« less

Development of ultrastable filters and lasers for solar seismology

NASA Technical Reports Server (NTRS)

Rust, D. M.; Kunski, R.; Cohn, R. F.

1986-01-01

The Stable Solar Analyzer is a recently developed instrument for the measurement of solar magnetic fields and surface velocities that is being employed at the U.S. National Solar Observatory to study the subsurface convection cells of the sun and the structure of surface and subsurface magnetic fields. The Analyzer is expected to ultimately be flown aboard such spacecraft as the ESA/NASA Solar and Heliospheric Observatory. This instrument is based on a crystalline lithium niobate Fabry-Perot filter that is used in conjunction with a stabilized laser that furnishes an absolute wavelength reference; this laser Fabry-Perot combination has achieved wavelength stabilities of the order of 2 parts in 10 to the 10th, over a six-hour interval.

Understanding the Physical Nature of Coronal "EIT Waves"

NASA Astrophysics Data System (ADS)

Long, D. M.; Bloomfield, D. S.; Chen, P.-F.; Downs, C.; Gallagher, P. T.; Kwon, R.-Y.; Vanninathan, K.; Veronig, A.; Vourlidas, A.; Vrsnak, B.; Warmuth, A.; Zic, T.

2016-10-01

For almost 20 years the physical nature of globally-propagating waves in the solar corona (commonly called "EIT waves") has been controversial and subject to debate. Additional theories have been proposed throughout the years to explain observations that did not fit with the originally proposed fast-mode wave interpretation. However, the incompatibility of observations made using the Extreme-ultraviolet Imaging Telescope (EIT) on the Solar and Heliospheric Observatory with the fast-mode wave interpretation have been challenged by differing viewpoints from the Solar Terrestrial Relations Observatory spacecraft and higher spatial/temporal resolution data from the Solar Dynamics Observatory. In this paper, we reexamine the theories proposed to explain "EIT waves" to identify measurable properties and behaviours that can be compared to current and future observations. Most of us conclude that "EIT waves" are best described as fast-mode large-amplitude waves/shocks, which are initially driven by the impulsive expansion of an erupting coronal mass ejection in the low corona.

Understanding the Physical Nature of Coronal "EIT Waves".

PubMed

Long, D M; Bloomfield, D S; Chen, P F; Downs, C; Gallagher, P T; Kwon, R-Y; Vanninathan, K; Veronig, A M; Vourlidas, A; Vršnak, B; Warmuth, A; Žic, T

2017-01-01

For almost 20 years the physical nature of globally propagating waves in the solar corona (commonly called "EIT waves") has been controversial and subject to debate. Additional theories have been proposed over the years to explain observations that did not agree with the originally proposed fast-mode wave interpretation. However, the incompatibility of observations made using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory with the fast-mode wave interpretation was challenged by differing viewpoints from the twin Solar Terrestrial Relations Observatory spacecraft and data with higher spatial and temporal resolution from the Solar Dynamics Observatory . In this article, we reexamine the theories proposed to explain EIT waves to identify measurable properties and behaviours that can be compared to current and future observations. Most of us conclude that the so-called EIT waves are best described as fast-mode large-amplitude waves or shocks that are initially driven by the impulsive expansion of an erupting coronal mass ejection in the low corona.

Analysis of Geomagnetic Field Variations during Total Solar Eclipses Using INTERMAGNET Data

NASA Astrophysics Data System (ADS)

KIM, J. H.; Chang, H. Y.

2017-12-01

We investigate variations of the geomagnetic field observed by INTERMAGNET geomagnetic observatories over which the totality path passed during a solar eclipse. We compare results acquired by 6 geomagnetic observatories during the 4 total solar eclipses (11 August 1999, 1 August 2008, 11 July 2010, and 20 March 2015) in terms of geomagnetic and solar ecliptic parameters. These total solar eclipses are the only total solar eclipse during which the umbra of the moon swept an INTERMAGNET geomagnetic observatory and simultaneously variations of the geomagnetic field are recorded. We have confirmed previous studies that increase BY and decreases of BX, BZ and F are conspicuous. Interestingly, we have noted that variations of geomagnetic field components observed during the total solar eclipse at Isla de Pascua Mataveri (Easter Island) in Chile (IPM) in the southern hemisphere show distinct decrease of BY and increases of BX and BZ on the contrary. We have found, however, that variations of BX, BY, BZ and F observed at Hornsund in Norway (HRN) seem to be dominated by other geomagnetic occurrence. In addition, we have attempted to obtain any signatures of influence on the temporal behavior of the variation in the geomagnetic field signal during the solar eclipse by employing the wavelet analysis technique. Finally, we conclude by pointing out that despite apparent success a more sophisticate and reliable algorithm is required before implementing to make quantitative comparisons.

STRUCTURE AND DYNAMICS OF THE 2012 NOVEMBER 13/14 ECLIPSE WHITE-LIGHT CORONA

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

Pasachoff, J. M.; Rušin, V.; Saniga, M.

2015-02-20

Continuing our series of observations of coronal motion and dynamics over the solar-activity cycle, we observed from sites in Queensland, Australia, during the 2012 November 13 (UT)/14 (local time) total solar eclipse. The corona took the low-ellipticity shape typical of solar maximum (flattening index ε = 0.01), a change from the composite coronal images we observed and analyzed in this journal and elsewhere for the 2006 and 2008-2010 eclipses. After crossing the northeast Australian coast, the path of totality was over the ocean, so further totality was seen only by shipborne observers. Our results include velocities of a coronal massmore » ejection (CME; during the 36 minutes of passage from the Queensland coast to a ship north of New Zealand, we measured 413 km s{sup –1}) and we analyze its dynamics. We discuss the shapes and positions of several types of coronal features seen on our higher-resolution composite Queensland coronal images, including many helmet streamers, very faint bright and dark loops at the bases of helmet streamers, voids, and radially oriented thin streamers. We compare our eclipse observations with models of the magnetic field, confirming the validity of the predictions, and relate the eclipse phenomenology seen with the near-simultaneous images from NASA's Solar Dynamics Observatory (SDO/AIA), NASA's Extreme Ultraviolet Imager on Solar Terrestrial Relations Observatory, ESA/Royal Observatory of Belgium's Sun Watcher with Active Pixels and Image Processing (SWAP) on PROBA2, and Naval Research Laboratory's Large Angle and Spectrometric Coronagraph Experiment on ESA's Solar and Heliospheric Observatory. For example, the southeastern CME is related to the solar flare whose origin we trace with a SWAP series of images.« less

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

Like almost all solar observatories, NASA's IRIS can provide images of different layers of the sun's atmosphere, which together create a whole picture of what's happening. This image shows light at a wavelength of 1400 Angstrom, which highlights material some 650 miles above the sun's surface. The vertical line in the middle shows the slit for IRIS's spectrograph, which can separate light into its many wavelengths to provide even more information about the temperature and velocity of material during a flare. Credit: NASA/IRIS/Goddard Space Flight Center -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

INTERMAGNET and magnetic observatories

USGS Publications Warehouse

Love, Jeffrey J.; Chulliat, Arnaud

2012-01-01

A magnetic observatory is a specially designed ground-based facility that supports time-series measurement of the Earth’s magnetic field. Observatory data record a superposition of time-dependent signals related to a fantastic diversity of physical processes in the Earth’s core, mantle, lithosphere, ocean, ionosphere, magnetosphere, and, even, the Sun and solar wind.

Limb shape observations at the Pic du Midi Observatory. Determination of the solar gravitational moments

NASA Astrophysics Data System (ADS)

Rozelot, J. P.; Lefebvre, S.

The accurate shape of the Sun has been actively debated since 1974. So far, balloon and satellite experiments achieved the required sensibility to measure the expected small asphericities of the solar limb shape. However, exceptional good meteorological conditions encountered during several missions at the Pic du Midi Observatory have permitted to measure the coefficients shape of the solar limb on the two first Legendre polynomials expansion. In theory, this photospheric outer shape is sensitive to the interior rate, and asphericities can be explained both in terms of gravitational moments and thermal wind. We present observations made at the Pic du Midi Observatory and we compare results with these obtained by SDS (Sofia et al., 1994, 1996) and SOHO/MDI (Kuhn, 1999). The accepted and dedicated PICARD space mission on this subject is briefly presented.

Terminator 2020: Get Ready for the "Event" of The Next Decade

NASA Astrophysics Data System (ADS)

McIntosh, S. W.; Leamon, R. J.; Fan, Y.; Rempel, M.; Dikpati, M.

2017-12-01

The abrupt end of solar activity cycles 22 and 23 at the Sun's equator are observed with instruments from the Solar and Heliospheric Observatory (SOHO), Solar Terrestrial Relations Observatory (STEREO), and Solar Dynamics Observatory (SDO). These events are remarkable in that they rapidly trigger the onset of magnetic activity belonging to the next solar cycle at mid-latitudes. The triggered onset of new cycle flux emergence leads to blossoming of the new cycle shortly thereafter. Using small-scale tracers of magnetic solar activity we examine the timing of the cycle ``termination points'' in relation to the excitation of new activity and find that the time taken for the solar plasma to communicate this transition is less than one solar rotation, and possibly as little as a eight days. This very short transition time implies that the mean magnetic field present in the Sun's convection zone is approximately 80 kG. This value may be considerably larger than conventional explorations estimate and therefore, have a significant dynamical impact on the physical appearance of solar activity, and considerably impacting our ability to perform first-principles numerical simulations of the same. Should solar cycle 24 [and 25] continue in their progression we anticipate that a termination event of this type should occur in the 2020 timeframe. PSP will have a front row seat to observe this systemic flip in solar magnetism and the induced changes in our star's radiative and partiuculate output. Such observations may prove to be critical in assessing the Sun's ability to force short term evolution in the Earth's atmosphere.

A solar station in Ica - Mutsumi Ishitsuka: a research center to improve education at the university and schools

NASA Astrophysics Data System (ADS)

Terrazas-Ramos, Raúl

2012-07-01

The San Luis Gonzaga National University of Ica has built a solar station, in collaboration with the Geophysical Institute of Peru, the National Astronomical Observatory of Japan and the Hida Observatory. The Solar Station has the following equipment: a digital Spectrograph Solar Refractor Telescope Takahashi 15 cm aperture, 60 cm reflector telescope aperture, a magnetometer-MAGDAS/CPNM and a Burst Monitor Telescope Solar-FMT (Project CHAIN). These teams support the development of astronomical science and Ica in Peru, likewise contributing to science worldwide. The development of basic science will be guaranteed when university students, professors and researchers work together. The Solar Station will be useful for studying the different levels of university education and also for the general public. The Solar Station will be a good way to spread science in the region through public disclosure.

Low-frequency Radio Observatory on the Lunar Surface (LROLS)

NASA Astrophysics Data System (ADS)

MacDowall, Robert; Network for Exploration and Space Science (NESS)

2018-06-01

A radio observatory on the lunar surface will provide the capability to image solar radio bursts and other sources. Radio burst imaging will improve understanding of radio burst mechanisms, particle acceleration, and space weather. Low-frequency observations (less than ~20 MHz) must be made from space, because lower frequencies are blocked by Earth’s ionosphere. Solar radio observations do not mandate an observatory on the farside of the Moon, although such a location would permit study of less intense solar bursts because the Moon occults the terrestrial radio frequency interference. The components of the lunar radio observatory array are: the antenna system consisting of 10 – 100 antennas distributed over a square kilometer or more; the system to transfer the radio signals from the antennas to the central processing unit; electronics to digitize the signals and possibly to calculate correlations; storage for the data until it is down-linked to Earth. Such transmission requires amplification and a high-gain antenna system or possibly laser comm. For observatories on the lunar farside a satellite or other intermediate transfer system is required to direct the signal to Earth. On the ground, the aperture synthesis analysis is completed to display the radio image as a function of time. Other requirements for lunar surface systems include the power supply, utilizing solar arrays with batteries to maintain the system at adequate thermal levels during the lunar night. An alternative would be a radioisotope thermoelectric generator requiring less mass. The individual antennas might be designed with their own solar arrays and electronics to transmit data to the central processing unit, but surviving lunar night would be a challenge. Harnesses for power and data transfer from the central processing unit to the antennas are an alternative, but a harness-based system complicates deployment. The concept of placing the antennas and harnesses on rolls of polyimide and rolling them out may be a solution for solar radio observations, but it probably does not provide a sufficiently-uniform beam for other science targets.

A large-scale solar dynamics observatory image dataset for computer vision applications.

PubMed

Kucuk, Ahmet; Banda, Juan M; Angryk, Rafal A

2017-01-01

The National Aeronautics Space Agency (NASA) Solar Dynamics Observatory (SDO) mission has given us unprecedented insight into the Sun's activity. By capturing approximately 70,000 images a day, this mission has created one of the richest and biggest repositories of solar image data available to mankind. With such massive amounts of information, researchers have been able to produce great advances in detecting solar events. In this resource, we compile SDO solar data into a single repository in order to provide the computer vision community with a standardized and curated large-scale dataset of several hundred thousand solar events found on high resolution solar images. This publicly available resource, along with the generation source code, will accelerate computer vision research on NASA's solar image data by reducing the amount of time spent performing data acquisition and curation from the multiple sources we have compiled. By improving the quality of the data with thorough curation, we anticipate a wider adoption and interest from the computer vision to the solar physics community.

Solar heating for an observatory--Lincoln, Nebraska

NASA Technical Reports Server (NTRS)

1981-01-01

Report describes solar-energy system for 50 seat observatory that provides 60 percent of space heating needs. System includes 9 flat-plate collectors, rock storage bin, blowers, controls, ducting, and auxiliary natural-gas furnace; it has five operation modes. Net energy savings were 11.31 million Btu for 12 months, or equivalent of 1.9 barrels of oil. Report appendixes list performance factor definitions, performance equations, and average area weather conditions.

The McDonnell Douglas geophysical observatory program progress report 13 Conjugate point riometer program

NASA Technical Reports Server (NTRS)

Baker, M. B.

1975-01-01

This report, the thirteenth and final progress report on the McDonnell Douglas Geophysical Observatory Program, discusses history of the program from 1962 through 1973, and results of the research carried out in 1974. Topic areas covered include: Station operation; Ionospheric work; Solar studies, Magnetospheric studies; Satellite measurements; International participation; and, 1974 research on solar activity, ATS-6 studies, magnetospheric physics, and station operation.

KSC-06pd1235

NASA Image and Video Library

2006-06-26

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., the Solar Electron and Proton Telescope (SEPT) is seen on the STEREO observatory "B." SEPT is part of the Solar Energetic Particles Package of four telescopes, all part of the In situ Measurements of Particles & CME Transients (IMPACT) instrument suite. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than July 30. Photo credit: NASA/George Shelton

Skylab

NASA Image and Video Library

1970-01-01

This is a photograph of a technician checking on a solar array wing for the Orbital Workshop as it is deployed. A solar array, consisting of two wings covered on one side with solar cells, was mounted outside the workshop to generate electrical power to augment the power generated by another solar array mounted on the solar observatory.

The Virtual Solar Observatory: Still a Small Box

NASA Technical Reports Server (NTRS)

Gurman, J. B.; Bogart, R. S.; Davey, A. R.; Dimitoglou, G.; Hill, F.; Hourcle, J. A.; Martens, P. C.; Surez-Sola, I.; Tian, K. Q.; Wampler, S.

2005-01-01

Two and a half years after a design study began, and a year and a half after development commenced, version 1.0 of the Virtual Solar Observatory (VSO) was released at the 2004 Fall AGU meeting. Although internal elements of the VSO have changed, the basic design has remained the same, reflecting the team's belief in the importance of a simple, robust mechanism for registering data provider holdings, initiating queries at the appropriate provider sites, aggregating the responses, allowing the user to iterate before making a final selection, and enabling the delivery of data directly from the providers. In order to make the VSO transparent, lightweight, and portable, the developers employed XML for the registry, SOAP for communication between a VSO instance and data services, and HTML for the graphic user interface (GUI's). We discuss the internal data model, the API, and user responses to various trial GUI's as typical design issues for any virtual observatory. We also discuss the role of the "small box" of data search, identification, and delivery services provided by the VSO in the larger, Sun-Solar System Connection virtual observatory (VxO) scheme.

KSC-06pd1868

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla., on Aug. 11. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1867

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla., on Aug. 11. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1535

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - In the hazardous processing facility at Astrotech Space Operations in Titusville, Fla., technicians remove the protective cover from the top of Observatory A, one of two STEREO spacecraft. The observatory will be lifted onto a scale for weight measurements and later will be fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/Jack Pfaller

KSC-06pd1864

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla., on Aug. 11. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1534

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - In the hazardous processing facility at Astrotech Space Operations in Titusville, Fla., technicians begin removing the protective cover from Observatory A of the STEREO spacecraft. The observatory will be lifted onto a scale for weight measurements and later will be fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/Jack Pfaller

KSC-06pd1862

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1533

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - In the hazardous processing facility at Astrotech Space Operations in Titusville, Fla., technicians begin removing the protective cover from Observatory A of the STEREO spacecraft. The observatory will be lifted onto a scale for weight measurements and later will be fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/Jack Pfaller

KSC-06pd1860

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1863

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1540

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., technicians perform black-light inspection and cleaning of Observatory B, part of the STEREO spacecraft. The observatory will later be wrapped for transfer to the hazardous processing facility where it will be weighed and fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/George Shelton

KSC-06pd1866

NASA Image and Video Library

2006-08-11

KENNEDY SPACE CENTER, FLA. - The STEREO observatories are the focus of attention at a media viewing held at Astrotech Space Operations in Titusville, Fla., on Aug. 11. The two observatories were mated for launch but will separate into different orbits for their mission. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

George Ellery Hale's Early Solar Research at Chicago, Kenwood, Harvard, and Yerkes Observatories, 1882-1904

NASA Astrophysics Data System (ADS)

Osterbrock, D. E.

1999-05-01

Growing up in Chicago, George Ellery Hale, later the prime spirit in founding the AAS, was a precocious boy scientist. He was deeply interested in spectroscopy and astrophysics from an early age. His wealthy parents encouraged Hale's aspirations with magazines, books, and instruments, and he acquired his first telescope when he was 14. He knew as mentors classical astronomers S. W. Burnham and George W. Hough, but he preferred astrophysics and designed his own Kenwood Physical Obseervatory around a grating in a Rowland circle mounting, fed by a heliostat, both built for him by instrument-maker John A. Brashear. For his undergraduate thesis at MIT, Hale invented and (at Harvard College Observatory) demonstrated the spectroheliograph. With it, and a high-quality 12-in refractor at his later Kenwood Astrophysical Observatory (at the same site, the Hale family home, 4 miles from the present Hilton Hotel where the SPD, HAD and AAS are meeting) Hale did excellent solar research, especially on promineneces, flocculi, and the near-ultraviolet spectrum of the chromosphere. As a teen-ager and a young adult Hale traveled widely, and met several important piuoneer solar physicists, including Charles A. Young, Jules Janssen, Samuel P. Langley, and Henry Rowland. Hale designed Yerkes Observatory for solar and stellar research, and headed the solar work himself. One of his aims always was to compare other stars with the sun. Hale's telescopes, instruments, methods, and resulting papers will be described and illustrated by numerous slides.

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Building a Virtual Solar Observatory: I Look Around and There's a Petabyte Following Me

NASA Technical Reports Server (NTRS)

Gurman, J. B.; Bogart, R.; Hill. F.; Martens, P.; Oergerle, William (Technical Monitor)

2002-01-01

The 2001 July NASA Senior Review of Sun-Earth Connections missions and data centers directed the Solar Data Analysis Center (SDAC) to proceed in studying and implementing a Virtual Solar Observatory (VSO) to ease the identification of and access to distributed archives of solar data. Any such design (cf. the National Virtual Observatory and NASA's Planetary Data System) consists of three elements: the distributed archives, a "broker" facility that translates metadata from all partner archives into a single standard for searches, and a user interface to allow searching, browsing, and download of data. Three groups are now engaged in a six-month study that will produce a candidate design and implementation roadmap for the VSO. We hope to proceed with the construction of a prototype VSO in US fiscal year 2003, with fuller deployment dependent on community reaction to and use of the capability. We therefore invite as broad as possible public comment and involvement, and invite interested parties to a "birds of a feather" session at this meeting. VSO is partnered with the European Grid of Solar Observations (EGSO), and if successful, we hope to be able to offer the VSO as the basis for the solar component of a Living With a Star data system.

Observatories and Telescopes of Modern Times

NASA Astrophysics Data System (ADS)

Leverington, David

2016-11-01

Preface; Part I. Optical Observatories: 1. Palomar Mountain Observatory; 2. The United States Optical Observatory; 3. From the Next Generation Telescope to Gemini and SOAR; 4. Competing primary mirror designs; 5. Active optics, adaptive optics and other technical innovations; 6. European Northern Observatory and Calar Alto; 7. European Southern Observatory; 8. Mauna Kea Observatory; 9. Australian optical observatories; 10. Mount Hopkins' Whipple Observatory and the MMT; 11. Apache Point Observatory; 12. Carnegie Southern Observatory (Las Campanas); 13. Mount Graham International Optical Observatory; 14. Modern optical interferometers; 15. Solar observatories; Part II. Radio Observatories: 16. Australian radio observatories; 17. Cambridge Mullard Radio Observatory; 18. Jodrell Bank; 19. Early radio observatories away from the Australian-British axis; 20. The American National Radio Astronomy Observatory; 21. Owens Valley and Mauna Kea; 22. Further North and Central American observatories; 23. Further European and Asian radio observatories; 24. ALMA and the South Pole; Name index; Optical observatory and telescope index; Radio observatory and telescope index; General index.

JHelioviewer. Time-dependent 3D visualisation of solar and heliospheric data

NASA Astrophysics Data System (ADS)

Müller, D.; Nicula, B.; Felix, S.; Verstringe, F.; Bourgoignie, B.; Csillaghy, A.; Berghmans, D.; Jiggens, P.; García-Ortiz, J. P.; Ireland, J.; Zahniy, S.; Fleck, B.

2017-09-01

Context. Solar observatories are providing the world-wide community with a wealth of data, covering wide time ranges (e.g. Solar and Heliospheric Observatory, SOHO), multiple viewpoints (Solar TErrestrial RElations Observatory, STEREO), and returning large amounts of data (Solar Dynamics Observatory, SDO). In particular, the large volume of SDO data presents challenges; the data are available only from a few repositories, and full-disk, full-cadence data for reasonable durations of scientific interest are difficult to download, due to their size and the download rates available to most users. From a scientist's perspective this poses three problems: accessing, browsing, and finding interesting data as efficiently as possible. Aims: To address these challenges, we have developed JHelioviewer, a visualisation tool for solar data based on the JPEG 2000 compression standard and part of the open source ESA/NASA Helioviewer Project. Since the first release of JHelioviewer in 2009, the scientific functionality of the software has been extended significantly, and the objective of this paper is to highlight these improvements. Methods: The JPEG 2000 standard offers useful new features that facilitate the dissemination and analysis of high-resolution image data and offers a solution to the challenge of efficiently browsing petabyte-scale image archives. The JHelioviewer software is open source, platform independent, and extendable via a plug-in architecture. Results: With JHelioviewer, users can visualise the Sun for any time period between September 1991 and today; they can perform basic image processing in real time, track features on the Sun, and interactively overlay magnetic field extrapolations. The software integrates solar event data and a timeline display. Once an interesting event has been identified, science quality data can be accessed for in-depth analysis. As a first step towards supporting science planning of the upcoming Solar Orbiter mission, JHelioviewer offers a virtual camera model that enables users to set the vantage point to the location of a spacecraft or celestial body at any given time.

The Virtual Solar Observatory and the Heliophysics Meta-Virtual Observatory

NASA Astrophysics Data System (ADS)

Gurman, J. B.; Hourclé, J. A.; Bogart, R. S.; Tian, K.; Hill, F.; Suàrez-Sola, I.; Zarro, D. M.; Davey, A. R.; Martens, P. C.; Yoshimura, K.; Reardon, K. M.

2006-12-01

The Virtual Solar Observatory (VSO) has survived its infancy and provides metadata search and data identification for measurements from 45 instrument data sets held at 12 online archives, as well as flare and coronal mass ejection (CME) event lists. Like any toddler, the VSO is good at getting into anything and everything, and is now extending its grasp to more data sets, new missions, and new access methods using its application programming interface (API). We discuss and demonstrate recent changes, including developments for STEREO and SDO, and an IDL-callable interface for the VSO API. We urge the heliophysics community to help civilize this obstreperous youngster by providing input on ways to make the VSO even more useful for system science research in its role as part of the growing cluster of Heliophysics Virtual Observatories.

STRUCTURE AND DYNAMICS OF THE 2010 JULY 11 ECLIPSE WHITE-LIGHT CORONA

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

Pasachoff, J. M.; Rusin, V.; Saniga, M.

The white-light corona (WLC) during the total solar eclipse on 2010 July 11 was observed by several teams in the Moon's shadow stretching across the Pacific Ocean and a number of isolated islands. We present a comparison of the WLC as observed by eclipse teams located on the Tatakoto Atoll in French Polynesia and on Easter Island, 83 minutes later, combined with near-simultaneous space observations. The eclipse was observed at the beginning of the solar cycle, not long after solar minimum. Nevertheless, the solar corona shows a plethora of different features (coronal holes, helmet streamers, polar rays, very faint loopsmore » and radial-oriented thin streamers, a coronal mass ejection, and a puzzling 'curtain-like' object above the north pole). Comparing the observations from the two sites enables us to detect some dynamic phenomena. The eclipse observations are further compared with a hairy-ball model of the magnetic field and near-simultaneous images from the Atmospheric Imaging Assembly on NASA's Solar Dynamics Observatory, the Extreme Ultraviolet Imager on NASA's Solar Terrestrial Relations Observatory, the Sun Watcher, using Active Pixel System Detector and Image Processing on ESA's PRoject for Onboard Autonomy, and the Naval Research Laboratory's Large Angle and Spectrometric Coronagraph on ESA's Solar and Heliospheric Observatory. The Ludendorff flattening coefficient is 0.156, matching the expected ellipticity of coronal isophotes at 2 Rs{sub un}, for this rising phase of the solar-activity cycle.« less

NASA’s Solar Dynamics Observatory Captured Trio of Solar Flares April 2-3

NASA Image and Video Library

2017-12-08

The sun emitted a trio of mid-level solar flares on April 2-3, 2017. The first peaked at 4:02 a.m. EDT on April 2, the second peaked at 4:33 p.m. EDT on April 2, and the third peaked at 10:29 a.m. EDT on April 3. NASA’s Solar Dynamics Observatory, which watches the sun constantly, captured images of the three events. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however — when intense enough — they can disturb the atmosphere in the layer where GPS and communications signals travel. Learn more: go.nasa.gov/2oQVFju Caption: NASA's Solar Dynamics Observatory captured this image of a solar flare peaking at 10:29 a.m. EDT on April 3, 2017, as seen in the bright flash near the sun’s upper right edge. The image shows a subset of extreme ultraviolet light that highlights the extremely hot material in flares and which is typically colorized in teal. Credits: NASA/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

42 Years of Continuous Observations of the Solar Diameter - 1974 to 2015

NASA Astrophysics Data System (ADS)

Humberto Andrei, Alexandre; Calderari Boscardin, Sergio; Lousada Penna, Jucira; Vani Leister, Nelson

2015-08-01

We present an analysis of 42 years of continuous measurements of the photospheric solar diameter, taken at major national observatories, using the same fundamental method, and similar apparatus. Such a series overlap observations from the Calern Observatory/France (Solar Astrolabe in 1975-2003 to 253 obs/year lead by F. Laclare and C. Delmas; Doraysol in 2000-2005 to 3,070 obs/year lead by C. Delmas and V. Sinceac), from the IAG/USP/Brazil (Solar Astrolabe in 1974-1994 to 95 obs/year lead by N. VaniLeister, P. Benevides and M. Emilio), from the Antalya Observatory/Turkey (CCD Astrolabe in 2000-2007 to 400 obs/year lead by F. Chollet and OI. Golbasi), from the San Fernando Observatory/Spain (Solar Astrolabe in 1972-1975 to 133 obs/year lead by J. Muiños), from Observatório Nacional/Brasil (CCD Astrolabe in 1998-2009 to 1,820 obs/year lead by J. Penna, E. Reis Neto and A.H. Andrei; Heliometer 2010-2015 to 8,509 obs/year lead by S.C. Boscardin, J.L. Penna and A.H. Andrei). The Heliometer is fully automatized in its observations and continues in regular operation with no plan of stopping; it shares with the former instruments the physical/mathematical definition of the limb, and the instruments aperture and focal length. We perform a reconciliation of all these series, using the common stretches. A modulation with the 11 years cycle of solar activity is evident. However when such modulation is removed, both from the solar diameter compound series and from the solar activity series (given by the sunspots count), a very strong anti-correlation surfaces. This suggests a smaller diameter for the forthcoming cycles, in a behavior similar to that on the Minima of Dalton and Maunder. This study stresses the importance of keeping and make available such long, continuous, and uniform series of solar diameter measurements. Maybe even the more by the controversy about its magnitude and origin. This presentation is dedicated to all the teams that developed and sustained the modern solar diameter observations.

Automated Solar Flare Detection and Feature Extraction in High-Resolution and Full-Disk Hα Images

NASA Astrophysics Data System (ADS)

Yang, Meng; Tian, Yu; Liu, Yangyi; Rao, Changhui

2018-05-01

In this article, an automated solar flare detection method applied to both full-disk and local high-resolution Hα images is proposed. An adaptive gray threshold and an area threshold are used to segment the flare region. Features of each detected flare event are extracted, e.g. the start, peak, and end time, the importance class, and the brightness class. Experimental results have verified that the proposed method can obtain more stable and accurate segmentation results than previous works on full-disk images from Big Bear Solar Observatory (BBSO) and Kanzelhöhe Observatory for Solar and Environmental Research (KSO), and satisfying segmentation results on high-resolution images from the Goode Solar Telescope (GST). Moreover, the extracted flare features correlate well with the data given by KSO. The method may be able to implement a more complicated statistical analysis of Hα solar flares.

Compact clumps of dark matter near the solar surface

NASA Astrophysics Data System (ADS)

Pokrovsky, Yu. E.

2018-01-01

The solar surface oscillations observed in the Crimean Astrophysical Observatory (CrAO) at the frequency 104.1890 μHz and in the Solar and Heliospheric Observatory (SoHO) at 220.72 μHz are considered as a result of existence of Compact Clumps of Dark Matter (CCDM) at orbits near the solar surface. These CCDM have to emit Gravitational Waves (GW) which are estimated to be the most intensive ones expected in the vicinity of the Earth and can be easily detected in the near future by means of the Evolved Laser Interferometer Space Antenna (eLISA). In addition to CCDMCrAO and CCDMSoHO some other CCDM may exist in the solar structure. It is shown that GW radiated by most of these CCDM could be detected by eLISA even if the respective solar surface oscillations are too small to be observed.

The CUREA 1996 Summer Program in Astrophysics at Mount Wilson Observatory

NASA Astrophysics Data System (ADS)

Snider, Joe; Faison, Michael

1996-05-01

The Consortium for Undergraduate Research and Education in Astronomy (CUREA) will present its hands-on course in astrophysics and observational astronomy at Mount Wilson Observatory for the seventh time, from August 7-20, 1996. Students and staff live and work at the Observatory, situated in the San Gabriel Mountains above Los Angeles. This is a beautiful site at which the atmospheric seeing conditions are equal to the best in the world. This poster paper presents in text and photographs some of the highlights of past programs. During the program informal discussions led by staff members provide the necessary background for using the following facilities: the Snow Horizontal Solar Telescope, which was the first major solar telescope in the world and the first telescope to be installed on Mount Wilson when G.E.Hale founded the Observatory; a high-resolution Littrow pit spectrograph; a 6-inch diffraction-limited refractor and 24- inch reflector; a photometer and a CCD detector; a unique atomic-beam apparatus for recording solar 5-minute oscillations; and this summer for the first time, the historic 100-inch Hooker Telescope. Attention is devoted to many observable solar phenomena, such as sunspots, granulation, limb darkening, important spectral lines, Zeeman splitting of solar lines, and the measurement of solar rotation using the Doppler shift of a spectral line. Nighttime observing includes celestial objects such as the Moon, planets, variable stars, clusters, galaxies and other deep-sky objects. Students learn how to process celestial photographs and spectral plates in the darkroom. Each student works on a special project she or he has chosen, and reports on it at the end of the program. Tours of research projects on the mountain, talks by visiting astronomers and field trips to JPL, Cal Tech and Palomar are included.

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

This combined image shows the March 29, 2014, X-class flare as seen through the eyes of different observatories. SDO is on the bottom/left, which helps show the position of the flare on the sun. The darker orange square is IRIS data. The red rectangular inset is from Sacramento Peak. The violet spots show the flare's footpoints from RHESSI. -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Limb flares measurement from Langkawi National Observatory on 5th January 2016

NASA Astrophysics Data System (ADS)

Kamarudin, F.; Tahar, M. R.; Saibaka, N. R.

2017-05-01

Sun is the source of energy and has a lot of activity that will be influence the Earth. One of the solar activities is the limb flare or prominence. It release energy and expel outward the Sun surface. Langkawi National Observatory (LNO) had started photographic solar activity in Hα since 2008. LNO used the dedicated solar telescope to monitor and observed the solar activity daily. In 5th January 2016, LNO captured one limb flare at the south-west position of the Sun. The maximum height of the limb flare is 267,347 km and it increase gradually build up the velocity. Luckily, this eruption does not facing and directed towards Earth so there was no significant impact.

More than a solar cycle of synoptic solar and coronal data - A video presentation

NASA Technical Reports Server (NTRS)

Hoeksema, J. T.; Scherrer, P. H.; Herant, M.; Title, A. M.

1988-01-01

Color video movies of synoptic observations of the sun and corona can now be created. Individual analog frames on laser disks can be referenced digitally and played back at any speed. We have brought together photospheric magnetic field data from the Wilcox Solar Observatory at Stanford and the National Solar Observatory, model computations of the coronal magnetic field, and coronal data from the Sacramento Peak coronagraph and the Mauna Loa K-coronameter and made a series of movies presenting the data sets individually and in comparison with one another. This paper presents a description of each of the data sets and movies developed thus far and briefly outlines some of the more interesting and obvious features observed when viewing the movies.

Deep Learning for Space Weather Prediction

NASA Astrophysics Data System (ADS)

Pauly, M.; Shah, Y.; Cheung, C. M. M.

2016-12-01

Through the use of our current fleet of in-orbit solar observatories, we have accumulated a vast amount of high quality solar event data which has greatly helped us to understand the underlying mechanisms of how the Sun works. However, we still lack an accurate and robust system for autonomously predicting solar eruptive events, which are known to cause geomagnetic storms, disturbances in electrical grids, radio black outs, increased drag on satellites, and increased radiation exposure to astronauts. We address the need for a flare prediction system by developing deep neural networks (DNNs) trained with solar data taken by the Helioseismic & Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) instruments onboard the Solar Dynamics Observatory and X-ray flux data taken by the GOES satellites. We describe the architecture of the DNNs trained and compare the performance between different implementations.

Methods for Cloud Cover Estimation

NASA Technical Reports Server (NTRS)

Glackin, D. L.; Huning, J. R.; Smith, J. H.; Logan, T. L.

1984-01-01

Several methods for cloud cover estimation are described relevant to assessing the performance of a ground-based network of solar observatories. The methods rely on ground and satellite data sources and provide meteorological or climatological information. One means of acquiring long-term observations of solar oscillations is the establishment of a ground-based network of solar observatories. Criteria for station site selection are: gross cloudiness, accurate transparency information, and seeing. Alternative methods for computing this duty cycle are discussed. The cycle, or alternatively a time history of solar visibility from the network, can then be input to a model to determine the effect of duty cycle on derived solar seismology parameters. Cloudiness from space is studied to examine various means by which the duty cycle might be computed. Cloudiness, and to some extent transparency, can potentially be estimated from satellite data.

Inter-Comparison between July 24, 2014 EUV Data from NASA Sounding Rocket 36.289 and Concurrent Measurements from Orbital Solar Observatories

NASA Astrophysics Data System (ADS)

Didkovsky, L. V.; Wieman, S. R.; Judge, D. L.

2014-12-01

Sounding rocket mission NASA 36.289 Didkovsky provided solar EUV irradiance measurements from four instruments built at the USC Space Sciences Center: the Rare Gas Ionization Cell (RGIC), the Solar Extreme ultraviolet Monitor (SEM), the Dual Grating Spectrometer (DGS), and the Optics-Free Spectrometer (OFS), thus meeting the mission comprehensive success criteria. These sounding rocket data allow us to inter-compare the observed absolute EUV irradiance with the data taken at the same time from the SOHO and SDO solar observatories. The sounding rocket data from the two degradation-free instruments (DGS and OFS) can be used to verify the degradation rates of SOHO and SDO EUV channels and serve as a flight-proven prototypes for future improvements of degradation-free instrumentation for solar physics.

Rattlesnake Mountain Observatory (46.4° N, 119.6° W) Multispectral Optical Depth Measurements: 1979-1994 (NDP-053)

DOE Data Explorer

Larson, Nels R. [Pacific Northwest Laboratory (PNNL), Richland, WA (USA); Michalsky, Joseph J. [Atmospheric Sciences Research Center, Albany, NY (USA); LeBaron, Brock A. [Utah Bureau of Air Quality, Salt Lake City, Utah (USA)

2012-01-01

Surface measurements of solar irradiance of the atmosphere were made by a multipurpose computer-controlled scanning photometer at the Rattlesnake Mountain Observatory in eastern Washington. The observatory is located at 46.4° N, 119.6° W at an elevation of 1088 m above mean sea level. The photometer measures the attenuation of direct solar radiation for different wavelengths using 12 filters. Five of these filters (i.e., at 428 nm, 486 nm, 535 nm, 785 nm, and 1010 nm, with respective half-power widths of 2, 2, 3, 18, and 28 nm) are suitable for monitoring variations in the total optical depth of the atmosphere.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Philip H. Scherrer (left) principal investigator, Helioseismic and Magnetic Imager instrument, Stanford University in Palo Alto, speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, while colleagues Tom Woods, principal investigator, Extreme Ultraviolet Variability Experiment instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder and Madhulika Guhathakurta, SDO program scientist, NASA Headquarters (right) look on Wednesday, April 21, 2010, at the Newseum in Washington. Photo Credit: (NASA/Carla Cioffi)

Solar Flare Impulsive Phase Observations from SDO and Other Observatories

NASA Technical Reports Server (NTRS)

Chamberlin, Phillip C.; Woods, Thomas N.; Schrijver, Karel; Warren, Harry; Milligan, Ryan; Christe, Steven; Brosius, Jeffrey W.

2010-01-01

With the start of normal operations of the Solar Dynamics Observatory in May 2010, the Extreme ultraviolet Variability Experiment (EVE) and the Atmospheric Imaging Assembly (AIA) have been returning the most accurate solar XUV and EUV measurements every 10 and 12 seconds, respectively, at almost 100% duty cycle. The focus of the presentation will be the solar flare impulsive phase observations provided by EVE and AIA and what these observations can tell us about the evolution of the initial phase of solar flares. Also emphasized throughout is how simultaneous observations with other instruments, such as RHESSI, SOHO-CDS, and HINODE-EIS, will help provide a more complete characterization of the solar flares and the evolution and energetics during the impulsive phase. These co-temporal observations from the other solar instruments can provide information such as extending the high temperature range spectra and images beyond that provided by the EUV and XUV wavelengths, provide electron density input into the lower atmosphere at the footpoints, and provide plasma flows of chromospheric evaporation, among other characteristics.

Role of Private-Public Partnership in Health Education: A Survey of Current Practices in Udaipur City, Rajasthan, India

PubMed Central

Reddy, Jaddu J.; Multani, Suraj; Bhat, Nagesh; Sharma, Ashish; Singh, Sopan; Patel, Rahul

2013-01-01

Background: The concept of a public-private partnership (PPP) has been proposed as a potential model for providing education services besides public finance and public delivery. The present study was conducted to survey the current practices of Private-Public Partnership (PPP) in health education in Udaipur city, Rajasthan, India. Methods: A questionnaire survey was conducted among organizations involved exclusively and actively in health education in Udaipur city, Rajasthan, India. The pretested self designed structured questionnaire consisted of 21 items pertaining to the current practices of private-public partnership (PPP) in health education. Descriptive statistics were used to describe the data. Results: On the basis of inclusion criteria, 50 personnel from 2 private dental colleges, 1 private medical college, 2 Non Government Organizations (NGOs) and 1 health museum were selected. Only 15 (30%) of participants agreed that they have a written reference policy that outlines the services they provide to the general public. Regarding the collection of health education materials available, majority 35 (70%) had printed books followed by audio visual (AV) materials (slides, videos, audio cassettes) [22 (44%)]. 35 (70%) of participants reported that they loan only pamphlets and broachers to the public. Thirty four (68%) of participants provide information about oral health. Only 23 (46%) of participants reported that their institution/organization undergo periodic evaluation. Conclusions: Results of this survey show that that most of the PPP were involved in delivering health education, mostly concentrated on general health. Only few of them were involved in oral health education. The role of PPP in health education is integral to the effort of promoting a healthier population. This effort continues the trend and broadens the scope of involvement for further studies. PMID:24130954

Max '91 Workshop 2: Developments in Observations and Theory for Solar Cycle 22

NASA Technical Reports Server (NTRS)

Winglee, Robert M. (Editor); Dennis, Brian R. (Editor)

1989-01-01

Papers and observatory reports presented at the second workshop of the Max '91 program are compiled along with discussion group summaries and invited reviews. The four discussion groups addressed the following subjects: high-energy flare physics; coordinated magnetograph observations; flare theory and modeling; and Max '91 communications and coordination. A special session also took place on observations of Active Region 5395 and the associated flares of March 1989. Other topics covered during the workshop include the scientific objectives of solar gamma ray observations, the solar capabilities of each of the four instruments on the Gamma Ray Observatory, and access to Max '91 information.

A Comparison of Rome Observatory Sunspot Area and Sunspot Number Determinations With International Measures, 1958-1998

NASA Technical Reports Server (NTRS)

Wilson, Robert M.; Hathaway, David H.

2005-01-01

Two changes in recording the sunspot record have occurred in recent years. First, in 1976, the longer-than-100-yr daily photographic record of the Royal Greenwich Observatory (RGO), used for determination of numbers and positions of sunspot groups and sunspot areas ended, and second, at the end of 1980, after more than 130 years, Zurich s Swiss Federal Observatory stopped providing daily sunspot numbers. To extend the sunspot record beyond 1976, use of United States Air Force/National Oceanic and Atmospheric Administration (USAF/NOAA) sunspot drawing observations from the Solar Optical Observing Network began in 1977, and the combined record of sunspot activity from RGO/USAF/NOAA was made accessible at http://science.nasa.gov/ssl/PAD/SOLAR/greenwch.htm. Also, in 1981, the task of providing daily sunspot numbers was taken up by the Royal Observatory of Belgium s Solar Influences and Data analysis Center, and the combined Zurich/International sunspot number database was made available at http://sidc.oma.be/index.php3. In this study, Rome Observatory 1958-1998 photographic records of sunspot areas, numbers of groups, and derived sunspot numbers are compared against same-day international values to determine relative behaviors and to evaluate whether any potential changes might have been introduced in the overall sunspot record, due to the aforementioned changes.

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

This close-up of the sunspot underneath the March 29, 2014, flare shows incredible detail. The image was captured by the G-band camera at Sacramento Peak in New Mexico. This instrument can focus on only a small area at once, but provide very high resolution. Ground-based telescope data can be hindered by Earth's atmosphere, which blocks much of the sun's ultraviolet and X-ray light, and causes twinkling even in the light it does allow through. As it happens, the March 29 flare occurred at a time of day in New Mexico that often results in the best viewing times from the ground. Credit: Kevin Reardon (National Solar Observatory), Lucia Kleint (BAER Institute) -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

Zoom in on the flare in ultraviolet (SDO/AIA), X-rays (Hinode) and gamma-rays (RHESSI) -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Morfología de eyecciones coronales de masa: avances e interrogantes pendientes

NASA Astrophysics Data System (ADS)

Cremades, H.

2016-08-01

Coronal mass ejections (CMEs) originate in the solar atmosphere and inject large amounts of plasma and magnetic fields in the heliosphere. Moreover, they can generate geomagnetic storms and shock waves, which in turn may accelerate energetic particles. The growing interest in studying CMEs stems not only from practical reasons, given their capacity to interact with Earth's atmosphere involving undesirable technological effects for modern society, but also from scientific reasons, because CMEs are part of the solar wind and thus play a key role in coronal and interplanetary dynamics. Space missions devoted to solar monitoring such as SOHO (Solar and Heliospheric Observatory), STEREO (Solar-Terrestrial Relations Observatory), and SDO (Solar Dynamics Observatory) have meant a great step toward the understanding of CME structure and evolution. However, given the nature of the instruments used for CME observation it is still difficult to deduce aspects of their three-dimensional configuration. In this report we visit the most relevant and latest advances regarding the three-dimensional characterization of their morphology, based both on theoretical models and observations. Their relationship with aspects of their source regions at photospheric, chromospheric, and low coronal levels, as well as with their interplanetary counterparts detected in situ are additionally addressed. These correspondences are vital not only for deepening the physical understanding of CMEs, but also to constrain geometrical and propagation models of CMEs towards improving current space weather forecasts.

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

A combination of many (but not all) of the datasets which observed this flare. -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

The Malaysian Robotic Solar Observatory (P29)

NASA Astrophysics Data System (ADS)

Othman, M.; Asillam, M. F.; Ismail, M. K. H.

2006-11-01

Robotic observatory with small telescopes can make significant contributions to astronomy observation. They provide an encouraging environment for astronomers to focus on data analysis and research while at the same time reducing time and cost for observation. The observatory will house the primary 50cm robotic telescope in the main dome which will be used for photometry, spectroscopy and astrometry observation activities. The secondary telescope is a robotic multi-apochromatic refractor (maximum diameter: 15 cm) which will be housed in the smaller dome. This telescope set will be used for solar observation mainly in three different wavelengths simultaneously: the Continuum, H-Alpha and Calcium K-line. The observatory is also equipped with an automated weather station, cloud & rain sensor and all-sky camera to monitor the climatic condition, sense the clouds (before raining) as well as to view real time sky view above the observatory. In conjunction with the Langkawi All-Sky Camera, the observatory website will also display images from the Malaysia - Antarctica All-Sky Camera used to monitor the sky at Scott Base Antarctica. Both all-sky images can be displayed simultaneously to show the difference between the equatorial and Antarctica skies. This paper will describe the Malaysian Robotic Observatory including the systems available and method of access by other astronomers. We will also suggest possible collaboration with other observatories in this region.

Awareness of Consumer Protection Act among Doctors in Udaipur City, India.

PubMed

Singh, K; Shetty, S; Bhat, N; Sharda, A; Agrawal, A; Chaudhary, H

2010-01-01

To compare the awareness of provisions of consumer protection act among dental and medical professionals in Udaipur city, Rajasthan, India. In a cross sectional study, a total of 448 professionals (253 males, 195 females) belonging to dental (222) and medical (226) categories were surveyed using a self administered structured questionnaire. The questionnaire comprised of 22 questions about the awareness of consumer protection art (CPA) and whether these professionals were following the recommendations of CPA. The student's t-test, ANOVA test, and Scheffe's test were used as tests of significance. The awareness scores were significantly higher for medical professionals compared with those of dental professionals. Similarly, postgraduates showed more awareness in both the professions and it was found that private practitioners significantly have more awareness than the academic sector. Though medical professionals have more awareness of CPA compared to dental professionals, considering the present scenario, better knowledge of CPA is necessary for both professionals in order to be on the safer side.

Solar eclipses at high latitudes: ionospheric effects in the lower ionosphere

NASA Astrophysics Data System (ADS)

Cherniakov, S.

2017-12-01

The partial reflection facility of the Polar Geophysical Institute (the Tumanny observatory, 69.0N, 35.7E) has observed behavior of the high-latitude lower ionosphere during the 20 March 2015 total solar eclipse. There were several effects during the eclipse. At the heights of 60-80 km the ionosphere has shown the effect of a "short night", but at the higher altitudes local enhanced electron concentration had a wave-like form. Data received by the riometer of the Tumanny observatory have also shown wave-like behavior. The behavior can be explained by influence of acoustic-gravity waves which originated after cooling of the atmosphere during the lunar shadow supersonic movement, and transport processes during the eclipse. During the 21 August 2017 solar eclipse there was a substorm at the high latitudes. But after the end of the substorm in the region of the Tumanny observatory the observed amplitudes of the reflected waves had wave effects which could be connected with the coming waves from the region of the eclipse. The wave features were also shown in the behavior of the total electron content (TEC) of the lower ionosphere. During several solar eclipses it was implemented observations of lower ionosphere behavior by the partial reflection facility of the Tumanny observatory. The consideration of the lower ionosphere TEC had revealed common features in the TEC behavior during the eclipses. The photochemical theory of processes in the lower ionosphere is very complicated and up to now it is not completely developed. Therefore introduction of the effective coefficients determining the total speed of several important reactions has been widely adopted when modeling the D-region of the ionosphere. However, experimental opportunities for obtaining effective recombination coefficients are rather limited. One of the methods to estimate effective recombination coefficients uses the phenomenon of a solar eclipse. During solar eclipses at the partial reflection facility of the Tumanny observatory observations were carried out. It gave possibility to obtain the behavior of the electron concentration in time at the selected heights. Using the obtained experimental profiles, the effective recombination coefficients at the D-region heights of the ionosphere have been evaluated.

NASA Investigating the Life of Comet ISON

NASA Image and Video Library

2013-12-02

Comet ISON comes in from the bottom right and moves out toward the upper right, growing more faint, in this time-lapse image from the ESA/NASA Solar and Heliospheric Observatory. The image of the sun at the center is from NASA's Solar Dynamics Observatory. Credit: ESA/NASA/SOHO/SDO/GSFC After several days of fading, scientists continue to work to determine and to understand the fate of Comet ISON: There's no doubt that the comet shrank in size considerably as it rounded the sun and there's no doubt that something made it out on the other side to shoot back into space. The question remains as to whether the bright spot seen moving away from the sun was simply debris, or whether a small nucleus of the original ball of ice was still there. Regardless, it is likely that it is now only dust. Comet ISON, which began its journey from the Oort Cloud some 3 million years ago, made its closest approach to the sun on Nov. 28, 2013. The comet was visible in instruments on NASA's Solar Terrestrial Relations Observatory, or STEREO, and the joint European Space Agency/NASA Solar and Heliospheric Observatory, or SOHO, via images called coronagraphs. Coronagraphs block out the sun and a considerable distance around it, in order to better observe the dim structures in the sun's atmosphere, the corona. As such, there was a period of several hours when the comet was obscured in these images, blocked from view along with the sun. During this period of time, NASA's Solar Dynamics Observatory could not see the comet, leading many scientists to surmise that the comet had disintegrated completely. However, something did reappear in SOHO and STEREO coronagraphs some time later – though it was significantly less bright. Read more: 1.usa.gov/18hGYag NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Abilities of Celestial Observations in Astronomical Observatory of Physics Institute in Opole

NASA Astrophysics Data System (ADS)

Godłowski, W.; Szpanko, M.

2010-12-01

We present possibilities of astronomical investigation in Astronomical Observatory in Opole. Our observatory uses two telescopes: Celestron CGE-1400 XLT (35 cm) and Meade LX200 (30 cm) with spectrograph and CCD Camera. Main topic of our observational investigation is connected with observations of variable stars, minor bodies of the solar system, blazers and the Sun.

Semi-annual Sq-variation in solar activity cycle

NASA Astrophysics Data System (ADS)

Pogrebnoy, V.; Malosiev, T.

The peculiarities of semi-annual variation in solar activity cycle have been studied. The data from observatories having long observational series and located in different latitude zones were used. The following observatories were selected: Huancayo (magnetic equator), from 1922 to 1959; Apia (low latitudes), from 1912 to 1961; Moscow (middle latitudes), from 1947 to 1965. Based on the hourly values of H-components, the average monthly diurnal amplitudes (a difference between midday and midnight values), according to five international quiet days, were computed. Obtained results were compared with R (relative sunspot numbers) in the ranges of 0-30R, 40-100R, and 140-190R. It was shown, that the amplitude of semi-annual variation increases with R, from minimum to maximum values, on average by 45%. At equatorial Huancayo observatory, the semi-annual Sq(H)-variation appears especially clearly: its maximums take place at periods of equinoxes (March-April, September-October), and minimums -- at periods of solstices (June-July, December-January). At low (Apia observatory) and middle (Moscow observatory) latitudes, the character of semi-annual variation is somewhat different: it appears during the periods of equinoxes, but considerably less than at equator. Besides, with the growth of R, semi-annual variation appears against a background of annual variation, in the form of second peaks (maximum in June). At observatories located in low and middle latitudes, second peaks become more appreciable with an increase of R (March-April and September-October). During the periods of low solar activity, they are insignificant. This work has been carried out with the support from International Scientific and Technology Center (Project #KR-214).

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Madhulika Guhathakurta, SDO Program Scientist at NASA Headquarters in Washington, speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, Wednesday, April 21, 2010, at the Newseum in Washington. Launched on Feb. 11, 2010, SDO is the most advanced spacecraft ever designed to study the sun. During its five-year mission, it will examine the sun's magnetic field and also provide a better understanding of the role the sun plays in Earth's atmospheric chemistry and climate. Photo Credit: (NASA/Carla Cioffi)

The Goddard program of gamma ray transient astronomy

NASA Technical Reports Server (NTRS)

Cline, T. L.; Desai, U. D.; Teegarden, B. J.

1980-01-01

Gamma ray burst studies are reviewed. The past results, present status and future expectations are outlined regarding endeavors using experiments on balloons, IMP-6 and -7, OGO-3, ISEE-1 and -3, Helios-2, Solar Maximum Mission, the Einstein Observatory, Solar Polar and the Gamma Ray Observatory, and with the interplanetary gamma ray burst networks, to which some of these spacecraft sensors contribute. Additional emphasis is given to the recent discovery of a new type of gamma ray transient, detected on 1979 March 5.

Solar Dynamics Observatory (SDO) HGAS Induced Jitter

NASA Technical Reports Server (NTRS)

Liu, Alice; Blaurock, Carl; Liu, Kuo-Chia; Mule, Peter

2008-01-01

This paper presents the results of a comprehensive assessment of High Gain Antenna System induced jitter on the Solar Dynamics Observatory. The jitter prediction is created using a coupled model of the structural dynamics, optical response, control systems, and stepper motor actuator electromechanical dynamics. The paper gives an overview of the model components, presents the verification processes used to evaluate the models, describes validation and calibration tests and model-to-measurement comparison results, and presents the jitter analysis methodology and results.

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

Hernandez, G.; Roble, R.G.; Ridley, E.C.

Nightime thermospheric winds and temperatures have been measured over Fritz Peak Observatory, Colorado (39.9 /sup 0/N, 105.5 /sup 0/W), with a high resolution Fabry-Perot spectrometer. The winds and temperatures are obtained from the Doppler shifts and line profiles of the (O 1) 15,867K (630 nm) line emission. Measurements made during two large geomagnetic storm periods near solar cycle maximum reveal a thermospheric response to the heat and momentum sources associated with these storms that is more complex than the ones measured near solar cycle minimum. In the earlier measurements made during solar cycle minimum, the winds to the north ofmore » Fritz Peak Observatory had an enhanced equatorward component and the winds to the south were also equatorward, usually with smaller velocities. The winds measured to the east and west of the observatory both had an enhanced westward wind component. For the two large storms near the present solar cycle maximum period converging winds are observed in each of the cardinal directions from Fritz Peak Observatory. These converging winds with speeds of hundreds of meters per second last for several hours. The measured neutral gas temperature in each of the directions also increases several hundred degrees Kelvin. Numerical experiments done with the NCAR thermospheric general circulation model (TGCM) suggest that the winds to the east and north of the station are driven by high-latitude heating and enhanced westward ion drag associated with magnetospheric convection. The cause of the enhanced poleward and eastward winds measured to the south and west of Fritz Peak Observatory, respectively, is not known. During geomagnetic quiet conditions the circulation is typically from the soutwest toward the northeast in the evening hours.« less

Secular trends in storm-level geomagnetic activity

USGS Publications Warehouse

Love, J.J.

2011-01-01

Analysis is made of K-index data from groups of ground-based geomagnetic observatories in Germany, Britain, and Australia, 1868.0-2009.0, solar cycles 11-23. Methods include nonparametric measures of trends and statistical significance used by the hydrological and climatological research communities. Among the three observatory groups, German K data systematically record the highest disturbance levels, followed by the British and, then, the Australian data. Signals consistently seen in K data from all three observatory groups can be reasonably interpreted as physically meaninginful: (1) geomagnetic activity has generally increased over the past 141 years. However, the detailed secular evolution of geomagnetic activity is not well characterized by either a linear trend nor, even, a monotonic trend. Therefore, simple, phenomenological extrapolations of past trends in solar and geomagnetic activity levels are unlikely to be useful for making quantitative predictions of future trends lasting longer than a solar cycle or so. (2) The well-known tendency for magnetic storms to occur during the declining phase of a sunspot-solar cycles is clearly seen for cycles 14-23; it is not, however, clearly seen for cycles 11-13. Therefore, in addition to an increase in geomagnetic activity, the nature of solar-terrestrial interaction has also apparently changed over the past 141 years. ?? Author(s) 2011.

Comparison of potential field solutions for Carrington Rotation 2144

NASA Astrophysics Data System (ADS)

Hayashi, Keiji; Yang, Shangbin; Deng, Yuagyong

2016-02-01

We examined differences among the coronal magnetic field structures derived with the potential field source surface (PFSS) model for Carrington Rotation 2144, from 21 November to 19 December 2013. We used the synoptic maps of solar photospheric magnetic field from four observatories, the Huairou Solar Observing Station (HSOS), Global Oscillation Network Group (GONG), Helioseismic Magnetic Imager (HMI), and Wilcox Solar Observatory (WSO). We tested two smoothing methods, Gaussian and boxcar averaging, and correction of unbalanced net magnetic flux. The solutions of three-dimensional coronal magnetic field are significantly different each other. An open-field region derived with HSOS data agrees best with the corresponding coronal hole observed by Solar Dynamics Observatories/Atmospheric Imaging Assembly, while HMI data yielded best agreements with the near-Earth OMNI database. The GONG data overall gave agreements as good as the HMI. The PFSS calculations using WSO data were least sensitive to the choices we examined in this work. Differences in PFSS solutions using different choices and parameters in smoothing imply that the photospheric magnetic field distributions with size of several degrees at midlatitude and low-latitude regions can be decisive, at least, in the examined period. To better determine the global solar corona, therefore, further evaluation of influences from compact bipolar magnetic field is needed.

Calibration of Solar Radio Spectrometer of the Purple Mountain Observatory

NASA Astrophysics Data System (ADS)

Lei, LU; Si-ming, LIU; Qi-wu, SONG; Zong-jun, NING

2015-10-01

Calibration is a basic and important job in solar radio spectral observations. It not only deduces the solar radio flux as an important physical quantity for solar observations, but also deducts the flat field of the radio spectrometer to display the radio spectrogram clearly. In this paper, we first introduce the basic method of calibration based on the data of the solar radio spectrometer of Purple Mountain Observatory. We then analyze the variation of the calibration coefficients, and give the calibrated results for a few flares. These results are compared with those of the Nobeyama solar radio polarimeter and the hard X-ray observations of the RHESSI (Reuven Ramaty High Energy Solar Spectroscopic Imager) satellite, it is shown that these results are consistent with the characteristics of typical solar flare light curves. In particular, the analysis on the correlation between the variation of radio flux and the variation of hard X-ray flux in the pulsing phase of a flare indicates that these observations can be used to study the relevant radiation mechanism, as well as the related energy release and particle acceleration processes.

Ssalmon - The Solar Simulations For The Atacama Large Millimeter Observatory Network

NASA Astrophysics Data System (ADS)

Wedemeyer, Sven; Ssalmon Group

2016-07-01

The Atacama Large Millimeter/submillimeter Array (ALMA) provides a new powerful tool for observing the solar chromosphere at high spatial, temporal, and spectral resolution, which will allow for addressing a wide range of scientific topics in solar physics. Numerical simulations of the solar atmosphere and modeling of instrumental effects are valuable tools for constraining, preparing and optimizing future observations with ALMA and for interpreting the results. In order to co-ordinate related activities, the Solar Simulations for the Atacama Large Millimeter Observatory Network (SSALMON) was initiated on September 1st, 2014, in connection with the NA- and EU-led solar ALMA development studies. As of April, 2015, SSALMON has grown to 83 members from 18 countries (plus ESO and ESA). Another important goal of SSALMON is to promote the scientific potential of solar science with ALMA, which has resulted in two major publications so far. During 2015, the SSALMON Expert Teams produced a White Paper with potential science cases for Cycle 4, which will be the first time regular solar observations will be carried out. Registration and more information at http://www.ssalmon.uio.no.

First Results of the Near Real-Time Imaging Reconstruction System at Big Bear Solar Observatory

NASA Astrophysics Data System (ADS)

Yang, G.; Denker, C.; Wang, H.

2003-05-01

The Near Real-Time Imaging Reconstruction system (RTIR) at Big Bear Solar Observatory (BBSO) is designed to obtain high spatial resolution solar images at a cadence of 1 minute utilizing the power of parallel processing. With this system, we can compute near diffraction-limited images without saving huge amounts of data that are involved in the speckle masking reconstruction algorithm. It enables us to monitor active regions and give fast response to the solar activity. In this poster we present the first results of our new 32-CPU Beowulf cluster system. The images are 1024 x 1024 and the field of view (FOV) is 80'' x 80''. Our target is an active region with complex magnetic configuration. We focus on pores and small spots in the active region with the goal of better understanding the formation of penumbra structure. In addition we expect to study evolution of active regions during solar flares.

The Solar Connections Observatory for Planetary Environments

NASA Astrophysics Data System (ADS)

Oliversen, R. J.; Harris, W. M.

2002-05-01

The NASA Sun-Earth Connection theme roadmap calls for comparative studies of planetary, cometary, and local interstellar medium (LISM) interaction with the Sun and solar variability. Through such studies, we advance our understanding of basic physical plasma and gas dynamic processes, thus increasing our predictive capabilities for the terrestrial, planetary, and interplanetary environments where future remote and human exploration will occur. Because the other planets have lacked study initiatives comparable to the STP, LWS, and EOS programs, our understanding of the upper atmospheres and near space environments on these worlds is far less detailed than our knowledge of the Earth. To close this gap, we propose a mission to study the solar interaction with bodies throughout our solar system and the heliopause with a single remote sensing space observatory, the Solar Connections Observatory for Planetary Environments (SCOPE). SCOPE consists of a binocular EUV/UV telescope operating from a heliocentric, Earth-trailing orbit that provides high observing efficiency, sub-arcsecond imaging and broadband medium resolution spectro-imaging over the 55-290 nm bandpass, and high resolution (R>105) H Ly-α emission line profile measurements of small scale planetary and wide field diffuse solar system structures. A key to the SCOPE approach is to include Earth as a primary science target. The other planets and comets will be monitored in long duration campaigns centered, when possible, on solar opposition when interleaved terrestrial-planet observations can be used to directly compare the response of both worlds to the same solar wind stream and UV radiation field. Using the combination of SCOPE observations and models including MHD, general circulation, and radiative transfer, we will isolate the different controlling parameters in each planet system and gain insight into the underlying physical processes that define the solar connection.

Improvement of solar-cycle prediction: Plateau of solar axial dipole moment

NASA Astrophysics Data System (ADS)

Iijima, H.; Hotta, H.; Imada, S.; Kusano, K.; Shiota, D.

2017-11-01

Aims: We report the small temporal variation of the axial dipole moment near the solar minimum and its application to the solar-cycle prediction by the surface flux transport (SFT) model. Methods: We measure the axial dipole moment using the photospheric synoptic magnetogram observed by the Wilcox Solar Observatory (WSO), the ESA/NASA Solar and Heliospheric Observatory Michelson Doppler Imager (MDI), and the NASA Solar Dynamics Observatory Helioseismic and Magnetic Imager (HMI). We also use the SFT model for the interpretation and prediction of the observed axial dipole moment. Results: We find that the observed axial dipole moment becomes approximately constant during the period of several years before each cycle minimum, which we call the axial dipole moment plateau. The cross-equatorial magnetic flux transport is found to be small during the period, although a significant number of sunspots are still emerging. The results indicate that the newly emerged magnetic flux does not contribute to the build up of the axial dipole moment near the end of each cycle. This is confirmed by showing that the time variation of the observed axial dipole moment agrees well with that predicted by the SFT model without introducing new emergence of magnetic flux. These results allow us to predict the axial dipole moment at the Cycle 24/25 minimum using the SFT model without introducing new flux emergence. The predicted axial dipole moment at the Cycle 24/25 minimum is 60-80 percent of Cycle 23/24 minimum, which suggests the amplitude of Cycle 25 is even weaker than the current Cycle 24. Conclusions: The plateau of the solar axial dipole moment is an important feature for the longer-term prediction of the solar cycle based on the SFT model.

70 Years of Sunspot Observations at Kanzelhoehe Observatory

NASA Astrophysics Data System (ADS)

Pötzi, W.; Veronig, A.; Temmer, M.; Baumgartner, D. J.; Freislich, H.; Strutzmann, H.

During World War II the German Airforce established a network of observatories, among them the Kanzelhöhe Observatory (KSO), which would provide information on solar activity in order to investigate the conditions of the Earth's ionosphere in terms of radio-wave propagation. Solar observations began already in 1943 with photographs of the photosphere and drawings of sunspots, plage regions and faculae, as well as patrol observations of the solar corona. Since 1944 relative sunspot numbers were derived, these relative numbers agree with the new International Sunspot Number tep[ISN,][]{SIDC,Clette2014} within ≈ 10%. However, revisiting the historical data, we also find periods with larger deviations. There were two main reasons for these deviations. On the one hand major instrumental changes took place and the instrument was relocated to another observation tower. On the other hand there were periods of frequent replacements of personnel. In the long term, the instrumental improvements led to better image quality, and a trend towards better seeing conditions since the year 2000 was found.

Coordinated study of Solar-Terrestrial Observatory (STO) payloads on space station

NASA Technical Reports Server (NTRS)

Wu, S. T.

1988-01-01

Since the publication of the final report of the science study group in October 1984 on the Solar Terrestrial Observatory (STO), its science goals and objectives have been clearly defined and a conceptual design and analysis was carried out by MSFC/NASA. Plans for the possible placing of the STO aboard the Space Station were made. A series of meetings for the STO science study group were held to review the instruments to be placed on the initial STO at Space Station IOC, and the placement of these instruments on the manned space station, polar platform, and the co-orbiting platform. A summary of these initial STO instruments is presented in Section 2. A brief description of the initial plan for the placement of STO instruments is included in Section 3. Finally, in Section 4, the scenario for the operation of the STO is discussed. These results were obtained from the report of the Solar Terrestrial Observatory mini-workshop held at MSFC on 6 June 1985.

Hinode Satellite Captures Total Solar Eclipse Video Aug. 21

NASA Image and Video Library

2017-08-21

The Japan Aerospace Exploration Agency, the National Astronomical Observatory of Japan and NASA released this video of Aug. 21 total solar eclipse taken by the X-ray telescope aboard the Hinode joint solar observation satellite as it orbited high above the Pacific Ocean.

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

Zhu, Bei; Liu, Ying D.; Hu, Huidong

We study the solar energetic particle (SEP) event associated with the 2012 July 23 extreme solar storm, for which Solar Terrestrial Relations Observatory (STEREO) and the spacecraft at L1 provide multi-point remote sensing and in situ observations. The extreme solar storm, with a superfast shock and extremely enhanced ejecta magnetic fields observed near 1 au at STEREO A , was caused by the combination of successive coronal mass ejections (CMEs). Meanwhile, energetic particles were observed by STEREO and near-Earth spacecraft such as the Advanced Composition Explorer and SOlar and Heliospheric Observatory , suggesting a wide longitudinal spread of the particlesmore » at 1 au. Combining the SEP observations with in situ plasma and magnetic field measurements, we investigate the longitudinal distribution of the SEP event in connection with the associated shock and CMEs. Our results underscore the complex magnetic configuration of the inner heliosphere formed by solar eruptions. Examination of particle intensities, proton anisotropy distributions, element abundance ratios, magnetic connectivity, and spectra also gives important clues for particle acceleration, transport, and distribution.« less

The Final Results from the Sudbury Neutrino Observatory

ScienceCinema

Bellerive, Alain

2017-12-15

The Sudbury Neutrino Observatory (SNO) was a water Cherenkov detector dedicated to investigate elementary particles called neutrinos. It successfully took data between 1999 and 2006. The detector was unique in its use of heavy water as a detection medium, permitting it to make a solar model-independent test of solar neutrino mixing. In fact, SNO conclusively showed that solar neutrinos oscillate on their way from the core of the Sun to the Earth. This groundbreaking observation was made during three independent phases of the experiment. Even if data taking ended, SNO is still in a mode of precise determination of the solar neutrino oscillation parameters because all along SNO had developed several methods to tell charged-current events apart from neutral-current events. This ability is crucial for the final and ultimate data analysis of all the phases. The physics reach of a combined three-phase solar analysis will be reviewed together with results and subtleties about solar neutrino physics.

Solar Triumvirate

NASA Image and Video Library

2016-02-09

The magnetic field lines of three active regions in close proximity to one another interacted with each other over two and a half days Feb. 8-10, 2016. This image is from NASA Solar Dynamics Observatory.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Madhulika Guhathakurta, far right, SDO Program Scientist at NASA Headquarters in Washington, speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, Wednesday, April 21, 2010, at the Newseum in Washington. Pictured from left of Dr. Guhathakurta's are: Tom Woods, principal investigator, Extreme Ultraviolet Variability Experiment instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder; Philip H. Scherrer, principal investigator, Helioseismic and Magnetic Imager instrument, Stanford University in Palo Alto; Alan Title, principal investigator, Atmospheric Imaging Assembly instrument, Lockheed Martin Solar and Astrophysics Laboratory in Palo Alto and Dean Pesnell, SDO project scientist, Goddard Space Flight Center in Greenbelt, Md. Photo Credit: (NASA/Carla Cioffi)

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Scientists involved in NASA's Solar Dynamics Observatory (SDO) mission attend a press conference to discuss recent images captured by the SDO spacecraft Wednesday, April 21, 2010, at the Newseum in Washington. Pictured right to left are: Madhulika Guhathakurta, SDO program scientist, NASA Headquarters in Washington; Tom Woods, principal investigator, Extreme Ultraviolet Variability Experiment instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder; Philip H. Scherrer, principal investigator, Helioseismic and Magnetic Imager instrument, Stanford University in Palo Alto; Alan Title, principal investigator, Atmospheric Imaging Assembly instrument, Lockheed Martin Solar and Astrophysics Laboratory in Palo Alto and Dean Pesnell, SDO project scientist, Goddard Space Flight Center in Greenbelt, Md. Photo Credit: (NASA/Carla Cioffi)

The stellar and solar tracking system of the Geneva Observatory gondola

NASA Technical Reports Server (NTRS)

Huguenin, D.

1974-01-01

Sun and star trackers have been added to the latest version of the Geneva Observatory gondola. They perform an image motion compensation with an accuracy of plus or minus 1 minute of arc. The structure is held in the vertical position by gravity; the azimuth is controlled by a torque motor in the suspension bearing using solar or geomagnetic references. The image motion compensation is performed by a flat mirror, located in front of the telescope, controlled by pitch and yaw servo-loops. Offset pointing is possible within the solar disc and in a 3 degree by 3 degree stellar field. A T.V. camera facilitates the star identification and acquisition.

Secchi, Angelo (1818-78)

NASA Astrophysics Data System (ADS)

Murdin, P.

2000-11-01

Born in Reggio Emilia, became a Jesuit and was exiled with the rest of the order by Mazzini's Roman Republic. After a period at Georgetown Observatory, he returned to Italy in 1849 as director of the Roman College Observatory, constructing a new observatory dome on top of the main pillars of the incomplete church of Saint Ignazio. Secchi used its telescopes for solar and stellar research, one of ...

Laboratory studies in ultraviolet solar physics

NASA Technical Reports Server (NTRS)

Parkinson, W. H.; Kohl, J. L.; Gardner, L. D.; Raymond, J. C.; Smith, P. L.

1991-01-01

The research activity comprised the measurement of basic atomic processes and parameters which relate directly to the interpretation of solar ultraviolet observations and to the development of comprehensive models of the component structures of the solar atmosphere. The research was specifically directed towards providing the relevant atomic data needed to perform and to improve solar diagnostic techniques which probe active and quiet portions of the solar chromosphere, the transition zone, the inner corona, and the solar wind acceleration regions of the extended corona. The accuracy with which the physical conditions in these structures can be determined depends directly on the accuracy and completeness of the atomic and molecular data. These laboratory data are used to support the analysis programs of past and current solar observations (e.g., the Orbiting solar Observatories, the Solar Maximum Mission, the Skylab Apollo Telescope Mount, and the Naval Research Laboratory's rocket-borne High Resolution Telescope and Spectrograph). In addition, we attempted to anticipate the needs of future space-borne solar studies such as from the joint ESA/NASA Solar and Heliospheric Observatory (SOHO) spacecraft. Our laboratory activities stressed two categories of study: (1) the measurement of absolute rate coefficients for dielectronic recombination and electron impact excitation; and (2) the measurement of atomic transition probabilities for solar density diagnostics. A brief summary of the research activity is provided.

Calcium II K Line as a Measure of Activity: Meshing Sac Peak and Solis Measurements

NASA Astrophysics Data System (ADS)

Urbach, Elana; Earley, J.; Keil, S.

2012-05-01

The Calcium II K line is an important indicator of solar and stellar activity. Disk integrated Ca K measurements have been taken at the Evans Solar Facility at Sacramento Peak Observatory since 1976. This instrument will be shut down by the end of the year, and the observations will be continued by the Solis Integrated Sunlight Spectrometer (ISS), which has been taking measurements since 2006. We attempt to regress the measurements from Sacramento Peak and ISS. In addition, we compare the Ca K measurements with disk averaged line of sight magnetic field measurements, which will help us predict the magnetic field of other stars. We also compare the measurements with Lyman α, allowing us to use Ca K as an extreme ultraviolet (EUV) proxy. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) [or Research Experiences for Teachers (RET)] site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU/RET Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation.

NASA's SDO Sees Lunar Transit

NASA Image and Video Library

2017-12-08

NASA's Solar Dynamics Observatory captured this image of the moon crossing in front of its view of the sun on Jan. 30, 2014, at 9:00 a.m. EST. -- On Jan 30, 2014, beginning at 8:31 a.m EST, the moon moved between NASA’s Solar Dynamics Observatory, or SDO, and the sun, giving the observatory a view of a partial solar eclipse from space. Such a lunar transit happens two to three times each year. This one lasted two and one half hours, which is the longest ever recorded. When the next one will occur is as of yet unknown due to planned adjustments in SDO's orbit. Note in the picture how crisp the horizon is on the moon, a reflection of the fact that the moon has no atmosphere around it to distort the light from the sun. Credit: NASA/Goddard/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

MAGNETIC FLUX TRANSPORT AND THE LONG-TERM EVOLUTION OF SOLAR ACTIVE REGIONS

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

Ugarte-Urra, Ignacio; Upton, Lisa; Warren, Harry P.

2015-12-20

With multiple vantage points around the Sun, Solar Terrestrial Relations Observatory (STEREO) and Solar Dynamics Observatory imaging observations provide a unique opportunity to view the solar surface continuously. We use He ii 304 Å data from these observatories to isolate and track ten active regions and study their long-term evolution. We find that active regions typically follow a standard pattern of emergence over several days followed by a slower decay that is proportional in time to the peak intensity in the region. Since STEREO does not make direct observations of the magnetic field, we employ a flux-luminosity relationship to infermore » the total unsigned magnetic flux evolution. To investigate this magnetic flux decay over several rotations we use a surface flux transport model, the Advective Flux Transport model, that simulates convective flows using a time-varying velocity field and find that the model provides realistic predictions when information about the active region's magnetic field strength and distribution at peak flux is available. Finally, we illustrate how 304 Å images can be used as a proxy for magnetic flux measurements when magnetic field data is not accessible.« less

Lomnický štít Observatory - meteorology and solar astrophysics. (Slovak Title: Observatórium Lomnický štít - meteorológia a slnečná astrofyzika)

NASA Astrophysics Data System (ADS)

Rybák, J.; Mačura, R.; Bendík, P.; Bochníček, O.; Horecká, V.

2010-12-01

The paper presents statistical results obtained in the analysis of long-term series of meteorological observations of temperature, wind speed and wind direction, and daylight length that were measured in the period 1964-2009 at the SHMI Meteorological Observatory located at the Lomnický štít mountain peak. In relation to these meteorological data, the contribution also presents statistical results for time scales of various types of solar prominence and solar corona observations at the Lomnický štít Astronomical Observatory in the period 1980-2009. The obtained results were used to characterize the observatory from meteorological perspective presenting mainly the range and quality of observing conditions suitable for solar activity observations. The results show that observing conditions allow for observation of prominences in approximately one third of the days in a year, and observation of the emission corona in approximately one fifth of the days in a year. The contribution also documents the use of the obtained results in preparation of new post-focal instruments for solar corona monitoring, i. e. the coronal multipolarimeter (COMP-S) that is at present under construction. Effects of local warming of the Earth's atmosphere are tested in a statistical analysis of the meteorological data collected in the period 1964-2009. In this period, a marked local warming occured at Lomnický štít with increases in the minimal daily temperature 0.90°C and maximal daily temperature 1.84°C, and the mean value of these quantities raising by 1.21°C.

South Pole of the Sun, March 20, 2007

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. .

North Pole of the Sun, March 20, 2007

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting.

VizieR Online Data Catalog: Complex network for solar active regions (Daei+, 2017)

NASA Astrophysics Data System (ADS)

Daei, F.; Safari, H.; Dadashi, N.

2018-03-01

The solar monitor (www.solarmonitor.org) records the solar data observed by several solar space observatories and missions (e.g., GOES, GONG, ACE, STEREO, SDO, etc.). 4227 solar active regions (ARs) during 1999 January 1 to 2017 April 14 used for building the AR network are listed in table 1. See section 2 for further details. (1 data file).

Teaching and sharing about the Sun in the United States and with Spanish language resources

NASA Astrophysics Data System (ADS)

Peticolas, L. M.; Craig, N.; Hawkins, I.; Walker, C.

2007-05-01

The United States has many different scientific agencies that fund research on solar science, including the National Aeronautics and Space Agency (NASA) and the National Science Foundation (NSF). Because there is a large population of Spanish-speaking people in the US, some of the resources developed by the education components of research projects take into account broader cultural perspectives on science and are developed in Spanish. We will describe the education and outreach programs of three solar programs funded by NASA and NSF, the Solar TErrestrial RElations Observatory (STEREO) program, the "We Are One Under the Sun" Program, and the National Optical Astronomy Observatory (NOAO) education program. The STEREO program aims to teach about the Sun through different venues including teacher workshops and courses, teacher materials, turning solar data from STEREO into sound, working with museums, and creating solar posters, CDs, DVDs, and lenticulars. The "We are One Under the Sun" program focuses on Native Americans and Hispanics of Native heritage. It works by merging culture, ancient observatories, and the latest NASA solar science to engage children, youth, and the general public in science and technology through solar traditions in their own indigenous culture. The NOAO Educational Outreach Program was established to make the science and scientists of NOAO more accessible to the K-12 and college-level communities. We will focus on the NOAO solar projects and Spanish-Language Astronomy Materials Educational Center program, which provides multiple types of Spanish- language materials for teachers. These programs have had different levels of outreach in Spanish-speaking countries, namely Mexico (STEREO and "We are One Under the Sun") and Chile (NOAO). We will describe these efforts and give links to the Spanish and English resources available to learn and teach about the Sun.

SAO During the Whipple Years: The Origins of Project Celescope

NASA Astrophysics Data System (ADS)

Devorkin, David

2005-01-01

In 1955, the moribund Astrophysical Observatory of the Smithsonian Institution closed its doors on the south lawn of the Smithsonian Castle. Vestiges of its 60-year old legacy of monitoring solar radiation were transferred to Cambridge under a new name, the Smithsonian Astrophysical Observatory, and became housed within the Harvard College Observatory complex under the direction of Fred Whipple. Whipple, restarting the SAO almost from scratch, worked within the Smithsonian's ancient tradition of maintaining a world-wide network of solar observation stations by morphing it into a similar network of satellite tracking facilities for the IGY, quickly and quietly phasing out the solar work. Under the SAO name, however, Whipple did much more, vastly expanding his interests in meteor research and hyperballistic studies, deftly orchestrated to parallel his tracking facility empire which in time included aeroballistic studies, atomic time standards, and other associated technological and scientific campaigns. He also made sure SAO played a prominent role in NASA's emerging `observatory class' series of scientific satellites and used it to create a theoretical astrophysics unit. It is this last activity that we will introduce here, showing how Project Celescope fitted into Whipple's plan for SAO, and how it contributed to make the combined Harvard-Smithsonian Center for Astrophysics the largest astronomical organization on the planet by the 1970s.

New Platforms for Suborbital Astronomical Observations and In Situ Atmospheric Measurements: Spacecraft, Instruments, and Facilities

NASA Astrophysics Data System (ADS)

Rodway, K.; DeForest, C. E.; Diller, J.; Vilas, F.; Sollitt, L. S.; Reyes, M. F.; Filo, A. S.; Anderson, E.

2014-12-01

Suborbital astronomical observations have over 50 years' history using NASA's sounding rockets and experimental space planes. The new commercial space industry is developing suborbital reusable launch vehicles (sRLV's) to provide low-cost, flexible, and frequent access to space at ~100 km altitude. In the case of XCOR Aerospace's Lynx spacecraft, the vehicle design and capabilities work well for hosting specially designed experiments that can be flown with a human-tended researcher or alone with the pilot on a customized mission. Some of the first-generation instruments and facilities that will conduct solar observations on dedicated Lynx science missions include the SwRI Solar Instrument Pointing Platform (SSIPP) and Atsa Suborbital Observatory, as well as KickSat sprites, which are picosatellites for in situ atmospheric and solar phenomena measurements. The SSIPP is a demonstration two-stage pointed solar observatory that operates inside the Lynx cockpit. The coarse pointing stage includes the pilot in the feedback loop, and the fine stage stabilizes the solar image to achieve arcsecond class pointing. SSIPP is a stepping-stone to future external instruments that can operate with larger apertures and shorter wavelengths in the solar atmosphere. The Planetary Science Institute's Atsa Suborbital Observatory combines the strengths of ground-based observatories and space-based observing to create a facility where a telescope is maintained and used interchangeably with either in-house facility instruments or user-provided instruments. The Atsa prototype is a proof of concept, hand-guided camera that mounts on the interior of the Lynx cockpit to test target acquisition and tracking for human-operated suborbital astronomy. KickSat sprites are mass-producible, one inch printed circuit boards (PCBs) populated by programmable off the shelf microprocessors and radios for real time data transmission. The sprite PCBs can integrate chip-based radiometers, magnetometers, accelerometers, etc. This low-cost, customizable platform provides researchers the ability to design immediately responsive, repeatable, high resolution experiments.

The 2012 Transit of Venus for Cytherean Atmospheric Studies and as an Exoplanet Analog

NASA Astrophysics Data System (ADS)

Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Reardon, K. P.; Widemann, T.; Tanga, P.; Dantowitz, R.; Willson, R.; Kopp, G.; Yurchyshyn, V.; Sterling, A.; Scherrer, P.; Schou, J.; Golub, L.; Reeves, K.

2012-10-01

We worked to assemble as complete a dataset as possible for the Cytherean atmosphere in collaboration with Venus Express in situ and to provide an analog of spectral and total irradiance exoplanet measurements. From Haleakala, the whole transit was visible in coronal skies; our B images showed the evolution of the visibility of Venus's atmosphere and of the black-drop effect, as part of the Venus Twilight Experiment's 9 coronagraphs distributed worldwide with BVRI. We imaged the Cytherean atmosphere over two minutes before first contact, with subarcsecond resolution, with the coronagraph and a separate refractor. The IBIS imaging spectrometer at Sacramento Peak Observatory at H-alpha and carbon-dioxide also provided us high-resolution imaging. The NST of Big Bear Solar Observatory also provided high-resolution vacuum observations of the Cytherean atmosphere and black drop evolution. Our liaison with UH's Mees Solar Observatory scientists provided magneto-optical imaging at calcium and potassium. Spaceborne observations included the Solar Dynamics Observatory's AIA and HMI, and the Solar Optical Telescope (SOT) and X-ray Telescope (XRT) on Hinode, and total-solar-irradiance measurements with ACRIMSAT and SORCE/TIM, to characterize the event as an exoplanet-transit analog. Our expedition was sponsored by the Committee for Research and Exploration/National Geographic Society. Some of the funds for the carbon-dioxide filter for IBIS were provided by NASA through AAS's Small Research Grant Program. We thank Rob Lucas, Aram Friedman, and Eric Pilger '82 for assistance with Haleakala observing, Rob Ratkowski of Haleakala Amateur Astronomers for assistance with equipment and with the site, Stan Truitt for the loan of his Paramount ME, and Steve Bisque/Software Bisque for TheSky X controller. We thank Joseph Gangestad '06 of Aerospace Corp., a veteran of our 2004 expedition, for assistance at Big Bear. We thank the Lockheed Martin Solar and Astrophysics Laboratory and Hinode science and operations teams for planning and support.

Multi-Wave Station of Solar Monitoring

NASA Astrophysics Data System (ADS)

Korokhin, V.; Akimov, L.; Beletsky, S.; Belkina, I.; Velikodsky, Y.; Marchenko, G.; Shaparenko, E.

A technical description of the contemporary solar telescope of the Kharkov Astronomical Observatory (http://khassm.virtualave.net) is given, and the plan to future development is sketched. A wide range monitoring of solar activity including observations near UV range in Balmer continuum and the IR line of He 1083 nm is presented.

Image Quality of the Helioseismic and Magnetic Imager (HMI) Onboard the Solar Dynamics Observatory (SDO)

NASA Technical Reports Server (NTRS)

Wachter, R.; Schou, Jesper; Rabello-Soares, M. C.; Miles, J. W.; Duvall, T. L., Jr.; Bush, R. I.

2011-01-01

We describe the imaging quality of the Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO) as measured during the ground calibration of the instrument. We describe the calibration techniques and report our results for the final configuration of HMI. We present the distortion, modulation transfer function, stray light,image shifts introduced by moving parts of the instrument, best focus, field curvature, and the relative alignment of the two cameras. We investigate the gain and linearity of the cameras, and present the measured flat field.

KSC-06pd1799

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers check the mating of the two STEREO observatories, which is the launch configuration. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

Adaptive optics system for the IRSOL solar observatory

NASA Astrophysics Data System (ADS)

Ramelli, Renzo; Bucher, Roberto; Rossini, Leopoldo; Bianda, Michele; Balemi, Silvano

2010-07-01

We present a low cost adaptive optics system developed for the solar observatory at Istituto Ricerche Solari Locarno (IRSOL), Switzerland. The Shack-Hartmann Wavefront Sensor is based on a Dalsa CCD camera with 256 pixels × 256 pixels working at 1kHz. The wavefront compensation is obtained by a deformable mirror with 37 actuators and a Tip-Tilt mirror. A real time control software has been developed on a RTAI-Linux PC. Scicos/Scilab based software has been realized for an online analysis of the system behavior. The software is completely open source.

KSC-06pd1529

NASA Image and Video Library

2006-07-07

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., one of the covered STEREO observatories is being transferred to the Hazardous Processing Facility for fueling. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than Aug. 1. Photo credit: NASA/George Shelton

Comparative studies of the interaction between the Sun and planetary near space environments with the Solar Connections Observatory for Planetary Environments (SCOPE)

NASA Astrophysics Data System (ADS)

Harris, W. M.; Scope Team

2003-04-01

The Solar Connections Observatory for Planetary Environments (SCOPE) is a remote sensing facility designed to probe the nature of the relationship of planetary bodies and the local interstellar medium to the solar wind and UV-EUV radiation field. In particular, the SCOPE program seeks to comparatively monitor the near space environments and thermosphere/ionospheres of planets, planetesimals, and satellites under different magnetospheric configurations and as a function of heliocentric distance and solar activity. In addition, SCOPE will include the Earth as a science target, providing new remote observations of auroral and upper atmospheric phenomena and utilizing it as baseline for direct comparison with other planetary bodies. The observatory will be scheduled into discrete campaigns interleaving Target-Terrestrial observations to provide a comparative annual activity map over the course of a solar half cycle. The SCOPE science instrument consists of binocular UV (115-310 nm) and EUV (500-120 nm) telescopes and a side channel sky-mapping interferometer on a spacecraft stationed in a remote orbit. The telescope instruments provide a mix of capabilities including high spatial resolution narrow band imaging, moderate resolution broadband spectro-imaging, and high-resolution line spectroscopy. The side channel instrument will be optimized for line profile measurements of diagnostic terrestrial upper atmospheric, comet, interplanetary, and interstellar extended emissions.

The 2016 Transit of Mercury Observed from Major Solar Telescopes and Satellites

NASA Astrophysics Data System (ADS)

Pasachoff, Jay M.; Schneider, Glenn; Gary, Dale; Chen, Bin; Sterling, Alphonse C.; Reardon, Kevin P.; Dantowitz, Ronald; Kopp, Greg A.

2016-10-01

We report observations from the ground and space of the 9 May 2016 transit of Mercury. We build on our explanation of the black-drop effect in transits of Venus based on spacecraft observations of the 1999 transit of Mercury (Schneider, Pasachoff, and Golub, Icarus 168, 249, 2004). In 2016, we used the 1.6-m New Solar Telescope at the Big Bear Solar Observatory with active optics to observe Mercury's transit at high spatial resolution. We again saw a small black-drop effect as 3rd contact neared, confirming the data that led to our earlier explanation as a confluence of the point-spread function and the extreme solar limb darkening (Pasachoff, Schneider, and Golub, in IAU Colloq. 196, 2004). We again used IBIS on the Dunn Solar Telescope of the Sacramento Peak Observatory, as A. Potter continued his observations, previously made at the 2006 transit of Mercury, at both telescopes of the sodium exosphere of Mercury (Potter, Killen, Reardon, and Bida, Icarus 226, 172, 2013). We imaged the transit with IBIS as well as with two RED Epic IMAX-quality cameras alongside it, one with a narrow passband. We show animations of our high-resolution ground-based observations along with observations from XRT on JAXA's Hinode and from NASA's Solar Dynamics Observatory. Further, we report on the limit of the transit change in the Total Solar Irradiance, continuing our interest from the transit of Venus TSI (Schneider, Pasachoff, and Willson, ApJ 641, 565, 2006; Pasachoff, Schneider, and Willson, AAS 2005), using NASA's SORCE/TIM and the Air Force's TCTE/TIM. See http://transitofvenus.info and http://nicmosis.as.arizona.edu.Acknowledgments: We were glad for the collaboration at Big Bear of Claude Plymate and his colleagues of the staff of the Big Bear Solar Observatory. We also appreciate the collaboration on the transit studies of Robert Lucas (Sydney, Australia) and Evan Zucker (San Diego, California). JMP appreciates the sabbatical hospitality of the Division of Geosciences and Planetary Sciences of the California Institute of Technology, and of Prof. Andrew Ingersoll there. The solar observations lead into the 2017 eclipse studies, for which JMP is supported by grants from the NSF AGS and National Geographic CRE.

Evolution of the solar radius during the solar cycle 24 rise time

NASA Astrophysics Data System (ADS)

Meftah, Mustapha

2015-08-01

One of the real motivations to observe the solar radius is the suspicion that it might be variable. Possible temporal variations of the solar radius are important as an indicator of internal energy storage and as a mechanism for changes in the total solar irradiance. Measurements of the solar radius are of great interest within the scope of the debate on the role of the Sun in climate change. Solar energy input dominates the surface processes (climate, ocean circulation, wind, etc.) of the Earth. Thus, it appears important to know on what time scales the solar radius and other fundamental solar parameters, like the total solar irradiance, vary in order to better understand and assess the origin and mechanisms of the terrestrial climate changes. The current solar cycle is probably going to be the weakest in 100 years, which is an unprecedented opportunity for studying the variability of the solar radius during this period. This paper presents more than four years of solar radius measurements obtained with a satellite and a ground-based observatory during the solar cycle 24 rise time. Our measurements show the benefit of simultaneous measurements obtained from ground and space observatories. Space observations are a priori most favourable, however, space entails also technical challenges, a harsh environment, and a finite mission lifetime. The evolution of the solar radius during the rising phase of the solar cycle 24 show small variations that are out of phase with solar activity.

An international campaign of the 19th century to determine the solar parallax. The US Naval expedition to the southern hemisphere 1849-1852

NASA Astrophysics Data System (ADS)

Schrimpf, Andreas

2014-04-01

In 1847 Christian Ludwig Gerling, Marburg (Germany), suggested the solar parallax to be determined by measuring the position of Venus close to its inferior conjunction, especially at the stationary points, from observatories on nearly the same meridian but widely differing in latitude. James M. Gilliss, astronomer at the newly founded U.S. Naval Observatory, enthusiastically adopted this idea and procured a grant for the young astronomical community of the United States for an expedition to Chile. There they were to observe several conjunctions of Venus and oppositions of Mars, while the accompanying measurements were to be taken at the US Naval Observatory in Washington D.C. and the Harvard College Observatory at Cambridge, USA. This expedition was supported by A.V. Humboldt, C.F. Gauß, J.F. Encke, S.C. Walker, A.D. Bache, B. Peirce and others. From 1849 to 1852 not only were astronomical, but also meteorological and magnetic observations and measurements recorded, mainly in Santa Lucia close to Santiago, Chile. By comparing these measurements with those taken simultaneously at other observatories around the world the solar parallax could be calculated, although incomplete data from the corresponding northern observatories threatened the project's success. In retrospect this expedition can be recognized as the foundation of the Chilean astronomy. The first director of the new National Astronomical Observatory of Chile was Dr. C.W. Moesta, a Hessian student of Christian Ludwig Gerling's. The exchange of data between German, American and other astronomers during this expedition was well mediated by J.G. Flügel, consul of the United States of America and representative of the Smithsonian Institution in Europe, who altogether played a major role in nurturing the relationship between the growing scientific community in the U.S. and the well established one in Europe at that time.

Solar X-Ray and Gamma-Ray Imaging Spectroscopy

NASA Astrophysics Data System (ADS)

Dennis, B. R.; Christe, S. D.; Shih, A. Y.; Holman, G. D.; Emslie, A. G.; Caspi, A.

2018-02-01

X-ray and gamma-ray Sun observations from a lunar-based observatory would provide unique information on solar atmosphere thermal and nonthermal processes. EUV and energetic neutral atom imaging spectroscopy would augment the scientific value.

Left Limb of North Pole of the Sun, March 20, 2007

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting.

Right Limb of the South Pole of the Sun, March 18, 2007

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting.

Closer View of the Equatorial Region of the Sun, March 24, 2007

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting.

Terrestrial Planet Finder Coronagraph Observatory summary

NASA Technical Reports Server (NTRS)

Ford, Virginia; Levine-Westa, Marie; Kissila, Andy; Kwacka, Eug; Hoa, Tim; Dumonta, Phil; Lismana, Doug; Fehera, Peter; Cafferty, Terry

2005-01-01

Creating an optical space telescope observatory capable of detecting and characterizing light from extra-solar terrestrial planets poses technical challenges related to extreme wavefront stability. The Terrestrial Planet Finder Coronagraph design team has been developing an observatory based on trade studies, modeling and analysis that has guided us towards design choices to enable this challenging mission. This paper will describe the current flight baseline design of the observatory and the trade studies that have been performed. The modeling and analysis of this design will be described including predicted performance and the tasks yet to be done.

The Aula Espazio Gela Observatory: A tool for Solar System Education and Outreach

NASA Astrophysics Data System (ADS)

Rojas, J. F.; Perez-Hoyos, S.; Hueso, R.; Mendikoa, I.; Sanchez-Lavega, A.

2011-10-01

We present a summary of the activities undertaken over the first year of operations of the "Aula Espazio Gela Observatory", with teaching and astronomy outreach purposes. The observatory belongs to the Universidad del País Vasco and is a fundamental part of the "Master en Ciencia y Tecnología Espacial" (Space Science and Technology master). It is an urban observatory with the dome located on the roof of the School of Engineering at the Universidad del Pais Vasco in Bilbao (Spain).

The Sun's Seismic Radius as Measured from the Fundamental Modes of Oscillations and Its Implications for the TSI Variations

NASA Astrophysics Data System (ADS)

Jain, Kiran; Tripathy, S. C.; Hill, F.

2018-05-01

In this Letter we explore the relationship between the solar seismic radius and total solar irradiance (TSI) during the last two solar cycles using the uninterrupted data from space-borne instruments on board the Solar and Heliospheric Observatory (SoHO) and the Solar Dynamics Observatory (SDO). The seismic radius is calculated from the fundamental (f) modes of solar oscillations utilizing the observations from SoHO/Michelson Doppler Imager (MDI) and SDO/Helioseismic and Magnetic Imager (HMI), and the TSI measurements are obtained from SoHO/VIRGO. Our study suggests that the major contribution to the TSI variation arises from the changes in magnetic field, while the radius variation plays a secondary role. We find that the solar irradiance increases with decreasing seismic radius; however, the anti-correlation between them is moderately weak. The estimated maximum change in seismic radius during a solar cycle is about 5 km, and is consistent in both solar cycles 23 and 24. Previous studies ;suggest a radius change at the surface of the order of 0.06 arcsec to explain the 0.1% variation in the TSI values during the solar cycle; however, our inferred seismic radius change is significantly smaller, hence the TSI variations cannot be fully explained by the temporal changes in seismic radius.

The detection of global convection on the sun by an analysis of line shift data of the John M. Wilcox Solar Observatory at Stanford University

NASA Technical Reports Server (NTRS)

Yoshimura, Hirokazu

1987-01-01

Signatures of the existence of the global convection in the sun were found in the absorption line shift data of the John M. Wilcox Solar Observatory at Stanford University. The signatures are characterized by persistent periodic time variations in the east-west component of the velocity fields defined by fitting a slope to the line shift data in a certain longitude window at a specified latitude and longitude by a least square method. The variations indicate that the amplitude of the velocity fields is about 100 m/s. It is suggested that several modes of global convection are coexisting in the solar convection zone.

Utilization of space technology for terrestrial solar power applications

NASA Technical Reports Server (NTRS)

Yasui, R. K.; Patterson, R. E.

1974-01-01

A description is given of the evolution of photovoltaic power systems designed and built for terrestrial applications, giving attention to problem areas which are currently impeding the further development of such systems. The rooftop testing of surplus solar panels is considered along with solar powered seismic observatories, solar powered portable radio sets, and design considerations identified from past experience. Present activities discussed are related to a solar powered on-shore beacon flasher system, a solar powered buoy, and a solar powered beacon flasher buoy.

Photospheric magnetic fields in six magnetographs

NASA Astrophysics Data System (ADS)

Virtanen, Ilpo; Mursula, Kalevi

2016-10-01

Photospheric magnetic field has been routinely observed since 1950s, but calibrated digital data exist only since 1970s. The longest uniform data set is measured at the Wilcox Solar Observatory (WSO), covering 40 years from 1976 onwards. However, the WSO instrument operates in very low spatial resolution and suffers from saturation of strong fields. Other, higher resolution instruments like those at NSO Kitt Peak (KP) offer a more detailed view of the solar magnetic field, but several instrument updates make the data less uniform. While the different observatories show a similar large scale structure of the photospheric field, the measured magnetic field intensities differ significantly between the observatories. In this work we study the photospheric magnetic fields and, especially, the scaling of the magnetic field intensity between six independent data sets. We use synoptic maps constructed from the measurements of the photospheric magnetic field at Wilcox Solar Observatory, Mount Wilson Observatory (MWO), Kitt Peak (KP), SOLIS, SOHO/MDI and SDO/HMI. We calculate the harmonic expansion of the magnetic field from all six data sets and investigate the scaling of harmonic coefficients between the observations. We investigate how scaling depends on latitude and field strength, as well as on the solar cycle phase, and what is the effect of polar field filling in KP, SOLIS and MDI. We find that scaling factors based on harmonic coefficients are in general smaller than scaling factors based on pixel-by-pixel comparison or histogram techniques. This indicates that a significant amount of total flux is contained in the high harmonics of the higher resolution observations that are beyond the resolution of WSO. We note that only scaling factors based on harmonic coefficients should be used when using the PFSS-model, since the other methods tend to lead to overestimated values of the magnetic flux. The scaling of the low order harmonic coefficients is typically different than for higher terms. The most problematic harmonic is the axial quadrupole term, which is known to be noisy and to suffer from observational limitations (e.g., the vantage point effect). We did not find significant solar cycle variation in the scaling factors.

William E. Wilson and his contemporaries

NASA Astrophysics Data System (ADS)

Elliott, I.

Although he never attended school or university, William E. Wilson FRS, of Daramona, County Westmeath, made pioneering contributions to solar physics, celestial photography and stellar photometry. His well-equipped observatory attracted collaborators who included George Francis FitzGerald of Trinity College Dublin and Arthur Rambaut of Dunsink Observatory.

Newly found evidence of Sun-climate relationships

NASA Technical Reports Server (NTRS)

Kim, Hongsuk H.; Huang, Norden E.

1993-01-01

Solar radiation cycles drive climatic changes intercyclically. These interdecadal changes were detected as variations in solar total irradiances over the time period of recorded global surface-air-temperature (SAT) and have been restored utilizing Earth Radiation Budget Channel 10C measurements (1978-1990), Greenwich Observatory faculae data (1874-1975), and Taipei Observatory Active Region data (1964-1991). Analysis of the two separate events was carried out by treating each as a discrete time series determined by the length of each solar cycle. The results show that the global SAT responded closely to the input of solar cyclical activities, S, with a quantitative relation of T = 1.62 * S with a correlation coefficient of 0.61. This correlation peaks at 0.71 with a built-in time lag of 32 months in temperature response. Solar forcing in interannual time scale was also detected and the derived relationship of T = 0.17 * S with a correlation coefficient of 0.66 was observed. Our analysis shows derived climate sensitivities approximately fit the theoretical feedback slope, 4T(sup 3).

High resolution solar observations from first principles to applications

NASA Astrophysics Data System (ADS)

Verdoni, Angelo P.

2009-10-01

The expression "high-resolution observations" in Solar Physics refers to the spatial, temporal and spectral domains in their entirety. High-resolution observations of solar fine structure are a necessity to answer many of the intriguing questions related to solar activity. However, a researcher building instruments for high-resolution observations has to cope with the fact that these three domains often have diametrically opposed boundary conditions. Many factors have to be considered in the design of a successful instrument. Modern post-focus instruments are more closely linked with the solar telescopes that they serve than in past. In principle, the quest for high-resolution observations already starts with the selection of the observatory site. The site survey of the Advanced Technology Solar Telescope (ATST) under the stewardship of the National Solar Observatory (NSO) has identified Big Bear Solar Observatory (BBSO) as one of the best sites for solar observations. In a first step, the seeing characteristics at BBSO based on the data collected for the ATST site survey are described. The analysis will aid in the scheduling of high-resolution observations at BBSO as well as provide useful information concerning the design and implementation of a thermal control system for the New Solar Telescope (NST). NST is an off-axis open-structure Gregorian-style telescope with a 1.6 m aperture. NST will be housed in a newly constructed 5/8-sphere ventilated dome. With optics exposed to the surrounding air, NST's open-structure design makes it particularly vulnerable to the effects of enclosure-related seeing. In an effort to mitigate these effects, the initial design of a thermal control system for the NST dome is presented. The goal is to remediate thermal related seeing effects present within the dome interior. The THermal Control System (THCS) is an essential component for the open-telescope design of NST to work. Following these tasks, a calibration routine for the polarization optics for the Visible-light Imaging Magnetograph (VIM) is presented. VIM uses a set of two Liquid Crystal Variable Retarders (LCVRs) as the main components of its Stokes analyzer. Calibration of these components is a crucial step in providing reliable polarimetric measurements of the Sun using VIM. On 2007 July 15, using the Dunn Solar Telescope (DST) at the National Solar Observatory at Sacramento Peak (NSO/SP), New Mexico, the first polarimetric measurements using VIM were made. As a final step, illustrating an application of high-resolution solar observations, the results of a two-dimensional time-series acquired on 2006 June 11, using the DST at NSOP is presented. The data is used in a study of upflow events that are observed to occur in the Halpha 656.3 nm and Na D2 589.0 nm chromospheric absorption lines.

South Pole of the Sun, March 20, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

North Pole of the Sun, March 20, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

Spotless Sun

NASA Image and Video Library

2017-03-20

NASA Solar Dynamics Observatory sees the sun has been virtually spotless, as in no sunspots, a 11-day spotless stretch not seen since the last solar minimum many years ago. Movies are available at https://photojournal.jpl.nasa.gov/catalog/PIA21582

Spacelab Lyman Alpha-White Light Coronagraph Program

NASA Technical Reports Server (NTRS)

Kohl, J. L.

1986-01-01

The Spacelab Lyman Alpha Coronagraph (SLAC) of the Smithsonian Astrophysical Observatory (SAO) and the White Light Coronagraph (WLC) to be provided by the High Altitude Observatory (HAO) are two separate coronagraphs which would be operated in a joint fashion during Spacelab missions to be flown by the Space Shuttle. The two instruments would be used to perform joint observations of solar coronal structures from 1.2 to 8.0 solar radii from sun-center in vacuum ultraviolet and visible radiations. Temperatures, densities, and flow velocities throughout the solar wing acceleration region of the inner solar corona were measured. The Phase I Definition activity resulted in the successful definition and preliminary design of the experiment/instrumentation subsystem and associated software, ground support equipment and interfaces to the extended required to accurately estimate the scope of the investigation and prepare an Investigational Development Plan; the performance of the necessary functional, operations, and safety analyses necessary to complete the Experiment Requirements document.

Solar physics at the Einstein Tower

NASA Astrophysics Data System (ADS)

Denker, C.; Heibel, C.; Rendtel, J.; Arlt, K.; Balthasar, Juergen H.; Diercke, A.; González Manrique, S. J.; Hofmann, A.; Kuckein, C.; Önel, H.; Senthamizh Pavai, V.; Staude, J.; Verman, M.

2016-11-01

The solar observatory Einstein Tower ({Einsteinturm}) at the Telegrafenberg in Potsdam is both a landmark of modern architecture and an important place for solar physics. Originally built for high-resolution spectroscopy and measuring the gravitational redshift, research shifted over the years to understanding the active Sun and its magnetic field. Nowadays, telescope and spectrographs are used for research and development, i.e., testing instruments and in particular polarization optics for advanced instrumentation deployed at major European and international astronomical and solar telescopes. In addition, the Einstein Tower is used for educating and training of the next generation astrophysicists as well as for education and public outreach activities directed at the general public. This article comments on the observatory's unique architecture and the challenges of maintaining and conserving the building. It describes in detail the characteristics of telescope, spectrographs, and imagers; it portrays some of the research and development activities.

Retrospective Conversion of Solar Data Printed in "Synoptic Maps of the Solar Chromosphere": A Scientific and Librarianship Project

NASA Astrophysics Data System (ADS)

Laurenceau, A.; Aboudarham, J.; Renié, C.

2015-04-01

Between 1928 and 2003, the Observatoire de Paris published solar activity maps and their corresponding data tables, first in the Annals of the Meudon Observatory, then in the Synoptic Maps of the Solar Chromosphere. These maps represent the main solar structures in a single view and spread out on a complete Carrington rotation as well as tables of associated data, containing various information on these structures such as positions, length, morphological characteristics, and behavior. Since 2003, these maps and data tables have not been released in print, as they are only published on the online BASS2000 database, the solar database maintained by LESIA (Laboratory for space studies and astrophysical instruments). In order to make the first 80 years of observations which were available only in paper accessible and usable, the LESIA and the Library of the Observatory have started a project to digitize the publications, enter the data with the assistance of a specialized company, and then migrate the files obtained in BASS2000 and in the Heliophysics Features Catalog created in the framework of the European project HELIO.

A Solar Data Model for Use in Virtual Observatories

NASA Astrophysics Data System (ADS)

Reardon, K. P.; Bentley, R. D.; Messerotti, M.; Giordano, S.

2004-05-01

The creation of a virtual solar observatories relies heavily on the merging of the metadata describing different datasets into a common form so that it can be handled in a standard way for all associated resources. In order to bring together the varied data descriptions that already exist, it is necessary to have a common framework on which all the different datasets can be represented. The definition of this framework is done through a data model which attempts to provide a simplified but realistic description of the various entities that make up a data set or solar resource. We present the solar data model which has been developed as part of the European Grid of Solar Observations (EGSO) project. This model attempts to include many of the different elements in the field of solar physics, including data producers, data sets, event lists, and data providers. This global picture can then be used to focus on the particular elements required for a specific implementation. We present the different aspects of the model and describe some systems in which portions of this model have been implemented.

Influence of Extraterrestrial Radiation on Radiation Portal Monitors

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

Keller, Paul E.; Kouzes, Richard T.

2009-06-01

Cosmic radiation and solar flares can be a major source of background radiation at the Earth’s surface. This paper examines the relationship between extraterrestrial radiation and the detectable background in radiation portal monitors used for homeland security applications. Background radiation data from 13 radiation portal monitor facilities are examined and compared against external sources of data related to extraterrestrial radiation, including measurements at neutron monitors located at 53 cosmic-ray observatories around the Earth, four polar orbiting satellites, three geostationary satellites, ground-based geomagnetic field data from observatories around the Earth, a solar magnetic index, solar radio flux data, and sunspot activitymore » data. Four-years (January 2003 through December 2006) of data are used in this study, which include the latter part of Solar Cycle 23 as solar activity was on the decline. The analysis shows a significant relationship between some extraterrestrial radiation and the background detected in the radiation portal monitors. A demonstrable decline is shown in the average gamma ray and neutron background at the radiation portal monitors as solar activity declined over the period of the study.« less

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

The March 29, 2014, X-class flare appears as a bright light on the upper right in this image from SDO, showing light in the 304 Angstrom wavelength. This wavelength shows material on the sun in what's called the transition region, where the chromosphere transitions into the upper solar atmosphere, the corona. Some light of the flare is clearly visible, but the flare appears brighter in other images that show hotter temperature material. Credit: NASA/SDO/AIA -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Great Ball of Fire - Activity from August 1 CME Subsides

NASA Image and Video Library

2010-08-06

NASA image release August 6, 2010 On August 1, 2010, almost the entire Earth-facing side of the sun erupted in a tumult of activity. This image from the Solar Dynamics Observatory of the news-making solar event on August 1 shows the C3-class solar flare (white area on upper left), a solar tsunami (wave-like structure, upper right), multiple filaments of magnetism lifting off the stellar surface, large-scale shaking of the solar corona, radio bursts, a coronal mass ejection and more. This multi-wavelength extreme ultraviolet snapshot from the Solar Dynamics Observatory shows the sun's northern hemisphere in mid-eruption. Different colors in the image represent different gas temperatures. Earth's magnetic field is still reverberating from the solar flare impact on August 3, 2010, which sparked aurorae as far south as Wisconsin and Iowa in the United States. Analysts believe a second solar flare is following behind the first flare and could re-energize the fading geomagnetic storm and spark a new round of Northern Lights. Credit: NASA/SDO/AIA NASA Goddard Space Flight Center is home to the nation's largest organization of combined scientists, engineers and technologists that build spacecraft, instruments and new technology to study the Earth, the sun, our solar system, and the universe. Follow us on Twitter Join us on Facebook

The SOAR Telescope Project Southern Observatory for Astronomical Research (SOAR)

DTIC Science & Technology

2003-03-21

completed SOAR dome and facility. 2. Dome The preliminary design of the dome was handled by M3 (US). A Brazilian firm, Equatorial Sistemas led the...for the Gemini Telescope during construction, now Project Manager at the National Solar Observatory • Robert Shelton, Provost of the University on

Welcome to AURA

Science.gov Websites

Astronomy in FY2019 May 24, 2018 AURA Welcomes New Mexico Tech as New Member Institution May 24, 2018 Keck Northeast Astronomy Consortium Approved as New Member of AURA May 15, 2018 Jeremy Weirich joins AURA as VP Telescope National Optical Astronomy Observatory National Solar Observatory Space Telescope Science

Orbiting solar observatory 8 high resolution ultraviolet spectrometer experiment

NASA Technical Reports Server (NTRS)

1980-01-01

Oscillations, physical properties of the solar atmosphere, motions in the quiet solar atmosphere, coronal holes, motions in solar active regions, solar flares, the structure of plage regions, an atlas, and aeronomy are summarized. Photometric sensitivity, scattered light, ghosts, focus and spectral resolution, wavelength drive, photometric sensitivity, and scattered light, are also summarized. Experiments are described according to spacecraft made and experiment type. Some of the most useful data reduction programs are described.

NASA's Best-Observed X-Class Flare of All Time

NASA Image and Video Library

2014-05-07

IBIS can focus in on different wavelengths of light, and so reveal different layers at different heights in the sun's lower atmosphere, the chromosphere. This image shows a region slightly higher than the former one. Credit: Lucia Kleint (BAER Institute), Paul Higgins (Trinity College Dublin, Ireland) -- On March 29, 2014 the sun released an X-class flare. It was observed by NASA's Interface Region Imaging Spectrograph, or IRIS; NASA's Solar Dynamics Observatory, or SDO; NASA's Reuven Ramaty High Energy Solar Spectroscopic Imager, or RHESSI; the Japanese Aerospace Exploration Agency's Hinode; and the National Solar Observatory's Dunn Solar Telescope located at Sacramento Peak in New Mexico. To have a record of such an intense flare from so many observatories is unprecedented. Such research can help scientists better understand what catalyst sets off these large explosions on the sun. Perhaps we may even some day be able to predict their onset and forewarn of the radio blackouts solar flares can cause near Earth - blackouts that can interfere with airplane, ship and military communications. Read more: 1.usa.gov/1kMDQbO Join our Google+ Hangout on May 8 at 2:30pm EST: go.nasa.gov/1mwbBEZ Credit: NASA Goddard NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Nikolaev (Mykolayiv) Astronomical Observatory as the Object of the Ukrainian Tentative List WH UNESCO

NASA Astrophysics Data System (ADS)

Pinigin, Gennadiy; Pozhalova, Zhanna

2012-09-01

Nikolaev Astronomical Observatory (NAO), one of the oldest scientific institutions of the South-Eastern Europe, was founded as a naval observatory in 1821 for providing the needs of the Russian Black Sea Navy. It is a historical and astronomical complex with a reserved territory of total area 7.1 hectares, situated in the central part of Mykolaiv city, Ukraine. The beginning of scientific research at the Observatory is connected with the activity of Karl Knorre, its first director. From 1912 up to 1991, NAO was one of the Southern departments of Pulkovo Observatory with the main purpose to spread the system of absolute catalogs to the Southern hemisphere and to carry out regular observations of the Solar system bodies. Since 1992 NAO has become an independent leading institution of Ukraine in the field of positional astronomy, dynamics of Solar system bodies, research of near-Earth space, astronomical instrumentation. In 2007, it was inscribed in the Tentative UNESCO List of WH (#5116). The most significant part of the complex is the Main building, which was built in the style of Classicism in 1821--1829 (the monument of architecture #535 in the state registry). Also, the astronomical pavilions (1875, 1913, 1955, etc.) and instruments were preserved. Among them three Repsold instruments: meridian circle (1834), portable circle (1868) and vertical circle (1897). The unique astronomical and navigational devices, the collection of astronomical clocks are present in the observatory museum and the paper archive since the foundation of observatory is preserved.

Solar-Terrestrial Ontology Development

NASA Astrophysics Data System (ADS)

McGuinness, D.; Fox, P.; Middleton, D.; Garcia, J.; Cinquni, L.; West, P.; Darnell, J. A.; Benedict, J.

2005-12-01

The development of an interdisciplinary virtual observatory (the Virtual Solar-Terrestrial Observatory; VSTO) as a scalable environment for searching, integrating, and analyzing databases distributed over the Internet requires a higher level of semantic interoperability than here-to-fore required by most (if not all) distributed data systems or discipline specific virtual observatories. The formalization of semantics using ontologies and their encodings for the internet (e.g. OWL - the Web Ontology Language), as well as the use of accompanying tools, such as reasoning, inference and explanation, open up both a substantial leap in options for interoperability and in the need for formal development principles to guide ontology development and use within modern, multi-tiered network data environments. In this presentation, we outline the formal methodologies we utilize in the VSTO project, the currently developed use-cases, ontologies and their relation to existing ontologies (such as SWEET).

The COronal Solar Magnetism Observatory (COSMO) Large Aperture Coronagraph

NASA Astrophysics Data System (ADS)

Tomczyk, Steve; Gallagher, Dennis; Wu, Zhen; Zhang, Haiying; Nelson, Pete; Burkepile, Joan; Kolinksi, Don; Sutherland, Lee

2013-04-01

The COSMO is a facility dedicated to observing coronal and chromospheric magnetic fields. It will be located on a mountaintop in the Hawaiian Islands and will replace the current Mauna Loa Solar Observatory (MLSO). COSMO will provide unique observations of the global coronal magnetic fields and its environment to enhance the value of data collected by other observatories on the ground (e.g. SOLIS, BBO NST, Gregor, ATST, EST, Chinese Giant Solar Telescope, NLST, FASR) and in space (e.g. SDO, Hinode, SOHO, GOES, STEREO, Solar-C, Solar Probe+, Solar Orbiter). COSMO will employ a fleet of instruments to cover many aspects of measuring magnetic fields in the solar atmosphere. The dynamics and energy flow in the corona are dominated by magnetic fields. To understand the formation of CMEs, their relation to other forms of solar activity, and their progression out into the solar wind requires measurements of coronal magnetic fields. The large aperture coronagraph, the Chromospheric and Prominence Magnetometer and the K-Coronagraph form the COSMO instrument suite to measure magnetic fields and the polarization brightness of the low corona used to infer electron density. The large aperture coronagraph will employ a 1.5 meter fuse silica singlet lens, birefringent filters, and a spectropolarimeter to cover fields of view of up to 1 degree. It will observe the corona over a wide range of emission lines from 530.3 nm through 1083.0 nm allowing for magnetic field measurements over a wide range of coronal temperatures (e.g. FeXIV at 530.3 nm, Fe X at 637.4 nm, Fe XIII at 1074.7 and 1079.8 nm. These lines are faint and require the very large aperture. NCAR and NSF have provided funding to bring the large aperture coronagraph to a preliminary design review state by the end of 2013. As with all data from Mauna Loa, the data products from COSMO will be available to the community via the Mauna Loa website: http://mlso.hao.ucar.edu

Explosive events on the Sun.

PubMed

Harra, Louise K

2002-12-15

I describe two of the most dynamic and highly energetic phenomena in the Solar System--the explosive flares that can occur when plasma is confined by magnetic fields and the large-scale ejections of material known as 'coronal mass ejections'. These explosive events are poorly understood and yet occur in a variety of contexts in the Universe, ranging from planetary magnetospheres to active galactic nuclei. Understanding why flares and coronal mass ejections occur is a major goal across a wide range of space physics and astrophysics. Although explosive events from the Sun have dramatic effects on Earth, flares in other stars, for example, can be vastly more energetic and have an even more profound effect on their environment. We are now in the unprecedented position of having access to a number of space observatories dedicated to the Sun: the Yohkoh spacecraft, the Solar and Heliospheric Observatory, the Transition Region and Coronal Explorer and the Ramaty High Energy Solar Spectroscopic Imager. These cover a wide wavelength range from white light to gamma rays with both spectroscopy and imaging, and allow huge progress to be made in understanding the processes involved in such large explosions. The high-resolution data show dramatic and complex explosions of material on all spatial scales on the Sun. They have revealed that the Sun is constantly changing everywhere on its surface--something that was never imagined before. One of the mechanisms that has been proposed to account for the large energy release is magnetic reconnection. Recent observations from space increasingly support this view. This article will discuss those observations that support this model and also those that suggest different processes. The current space missions have given us an excellent insight into the actual explosive processes in the Sun. However, they have provided us with only a tantalizing glimpse of what causes the elusive trigger. Future missions such as Solar-B (the follow-on to Yohkoh), the Solar Terrestrial Relations Observatory, the Solar Dynamics Observatory and the Solar Orbiter mission will allow us to probe the trigger in a way that was not dreamt of a decade ago, by providing stereo views, measurements from Sun-grazing orbit, and much higher spatial, temporal and spectral resolution. It is an exciting time for solar physics and everything that we learn about the Sun will improve our ability to understand other magnetic phenomena in the Universe.

Dental caries experience and treatment needs of green marble mine laborers in Udaipur district, Rajasthan, India.

PubMed

Duraiswamy, Prabu; Kumar, T Santhosh; Dagli, Rushabh J; Kulkarni, Suhas

2008-01-01

The study was undertaken at Kesariyaji, located in Udaipur district of Rajasthan. There are about 3 million workers who marble mine at Rajasthan. Living conditions of these workers are substandard and most of them are immigrant workers living in tiny shacks. Majority of them belong to lower socioeconomic status with poor educational background. The present study was carried out to estimate dental caries prevalence and treatment needs of laborers working in the green marble mines of Udaipur district. The data was collected using the methods and standards recommended by the WHO. Dentition status and treatment needs along with decayed, missing, and filled teeth (DMFT) index, and decayed, missing, and filled surfaces score were recorded. Standard error of mean was calculated for all the mean values of treatment needs. There were three examiners, who were trained before the survey for inter-examiner variability, and the reliability was tested by means of weighted kappa statistics, which was 90%. The study population comprised 513 men in four age groups of 18-25, 26-34, 35-44, and 45-54 years, respectively. The mean DMFT for all age groups was 3.13 with highest mean of 4.0 for the age group of 45-54 years. Mean decayed teeth were 2.60, 3.33, 1.46, and 1.5 for the age groups 15-24, 25-34, 35-44, and 45-54 years, respectively. Filled component was nil for all age groups. Most of the subjects required one surface filling with a very less proportion needing pulp care. The missing component constituted the major part of DMFT index in the 45-54 years age group and the absence of filled component in the whole study population implies that the treatment needs of the study population are unmet. Thus, intervention in the form of oral health promotion and curative services are the need of the hour.

The Solar Dynamics Observatory (SDO) Education and Outreach (E/PO) Program: Changing Perceptions One Program at a Time

NASA Technical Reports Server (NTRS)

Drobnes, Emilie; Littleton, A.; Pesnell, William D.; Beck, K.; Buhr, S.; Durscher, R.; Hill, S.; McCaffrey, M.; McKenzie, D. E.; Myers, D.;

METEOSPACE, solar monitoring and space weather at Calern observatory

NASA Astrophysics Data System (ADS)

Corbard, T.; Malherbe, J.-M.; Crussaire, D.; Morand, F.; Ruty, F.; Biree, L.; Aboudarham, J.; Fuller, N.; Renaud, C.; Meftah, M.

2016-12-01

METEOSPACE is a new partnership project between the Paris Observatory (OP), the Observatoire de la Côte d'Azur (OCA), the French Air Force and a service company (LUNA technology) for the development and operation of a set of small telescopes Hα / Ca II K / Ca II H / G band to be installed at on the Calern plateau (OCA). The objective is to monitor solar activity for both research and its applications in space weather through continuous optical observations of the dynamic phenomena that are visible in the chromosphere: eruptions, destabilization of the filaments triggering coronal mass ejections and associated Moreton waves.

KSC-06pd1858

NASA Image and Video Library

2006-08-10

KENNEDY SPACE CENTER, FLA. - Technicians inside the Astrotech facility in Titusville, Florida, move the STEREO spacecraft to the spin table. The twin observatories will undergo a spin test to check balance and alignment in preparation for flight. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1802

NASA Image and Video Library

2006-08-09

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers look at the Delta third stage, or upper stage booster. In the background are the recently mated STEREO observatories, which is the launch configuration. STEREO, which stands for Solar Terrestrial Relations Observatory, is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket from Launch Pad 17-B at Cape Canaveral Air Force Station on Aug. 31. Photo credit: NASA/George Shelton

KSC-06pd1854

NASA Image and Video Library

2006-08-10

KENNEDY SPACE CENTER, FLA. - The STEREO spacecraft sits on a test stand inside the Astrotech facility in Titusville, Florida. The twin observatories will undergo a spin test to check balance and alignment in preparation for flight. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off on Aug. 31, from Launch Pad 17-B on Cape Canaveral Air Force Station in Florida. Photo credit: NASA/George Shelton.

KSC-06pd1541

NASA Image and Video Library

2006-07-10

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., technicians are ready to wrap more plastic around STEREO's Observatory B before its transfer to the hazardous processing facility where it will be weighed and fueled. STEREO stands for Solar Terrestrial Relations Observatory. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. STEREO is expected to lift off aboard a Boeing Delta II rocket no earlier than Aug. 1. Photo credit: NASA/George Shelton

Search for Life Beyond the Solar System. Exoplanets, Biosignatures & Instruments

NASA Astrophysics Data System (ADS)

Apai, Daniel; Gabor, Pavel

2014-03-01

Motivated by the rapidly increasing number of known Earth-sized planets, the increasing range of extreme conditions in which life on Earth can persist, and the progress toward a technology that will ultimately enable the search for life on exoplanets, the Vatican Observatory and the Steward Observatory announce a major conference entitled The Search for Life Beyond the Solar System: Exoplanets, Biosignatures & Instruments. The goal of the conference is to bring together the interdisciplinary community required to address this multi-faceted challenge: experts on exoplanet observations, early and extreme life on Earth, atmospheric biosignatures, and planet-finding telescopes.

KSC-06pd1527

NASA Image and Video Library

2006-07-07

KENNEDY SPACE CENTER, FLA. - At Astrotech Space Operations in Titusville, Fla., workers move one of the covered STEREO observatories on its portable stand . It is being transferred to the Hazardous Processing Facility for fueling. STEREO, which stands for Solar Terrestrial Relations Observatory, consists of two spacecraft whose mission is to take measurements of the sun and solar wind in 3-D, for the first time. This new view will improve our understanding of space weather and its impact on the Earth. Preparations are under way for a liftoff aboard a Delta rocket no earlier than Aug. 1. Photo credit: NASA/George Shelton

Solar Demon: near real-time solar eruptive event detection on SDO/AIA images

NASA Astrophysics Data System (ADS)

Kraaikamp, Emil; Verbeeck, Cis

Solar flares, dimmings and EUV waves have been observed routinely in extreme ultra-violet (EUV) images of the Sun since 1996. These events are closely associated with coronal mass ejections (CMEs), and therefore provide useful information for early space weather alerts. The Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) generates such a massive dataset that it becomes impossible to find most of these eruptive events manually. Solar Demon is a set of automatic detection algorithms that attempts to solve this problem by providing both near real-time warnings of eruptive events and a catalog of characterized events. Solar Demon has been designed to detect and characterize dimmings, EUV waves, as well as solar flares in near real-time on SDO/AIA data. The detection modules are running continuously at the Royal Observatory of Belgium on both quick-look data and synoptic science data. The output of Solar Demon can be accessed in near real-time on the Solar Demon website, and includes images, movies, light curves, and the numerical evolution of several parameters. Solar Demon is the result of collaboration between the FP7 projects AFFECTS and COMESEP. Flare detections of Solar Demon are integrated into the COMESEP alert system. Here we present the Solar Demon detection algorithms and their output. We will focus on the algorithm and its operational implementation. Examples of interesting flare, dimming and EUV wave events, and general statistics of the detections made so far during solar cycle 24 will be presented as well.

The mean magnetic field of the sun - Method of observation and relation to the interplanetary magnetic field

NASA Technical Reports Server (NTRS)

Scherrer, P. H.; Wilcox, J. M.; Kotov, V.; Severnyi, A. B.; Howard, R.

1977-01-01

The mean solar magnetic field as measured in integrated light has been observed since 1968. Since 1970 it has been observed both at Hale Observatories and at the Crimean Astrophysical Observatory. The observing procedures at both observatories and their implications for mean field measurements are discussed. A comparison of the two sets of daily observations shows that similar results are obtained at both observatories. A comparison of the mean field with the interplanetary magnetic polarity shows that the IMF sector structure has the same pattern as the mean field polarity.

Accessing eSDO Solar Image Processing and Visualization through AstroGrid

NASA Astrophysics Data System (ADS)

Auden, E.; Dalla, S.

2008-08-01

The eSDO project is funded by the UK's Science and Technology Facilities Council (STFC) to integrate Solar Dynamics Observatory (SDO) data, algorithms, and visualization tools with the UK's Virtual Observatory project, AstroGrid. In preparation for the SDO launch in January 2009, the eSDO team has developed nine algorithms covering coronal behaviour, feature recognition, and global / local helioseismology. Each of these algorithms has been deployed as an AstroGrid Common Execution Architecture (CEA) application so that they can be included in complex VO workflows. In addition, the PLASTIC-enabled eSDO "Streaming Tool" online movie application allows users to search multi-instrument solar archives through AstroGrid web services and visualise the image data through galleries, an interactive movie viewing applet, and QuickTime movies generated on-the-fly.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Scientists involved in NASA's Solar Dynamics Observatory (SDO) mission attend a press conference to discuss recent images captured by the SDO spacecraft Wednesday, April 21, 2010, at the Newseum in Washington. On Feb. 11, 2010, NASA launched the SDO spacecraft, which is the most advanced spacecraft ever designed to study the sun. Seated left to right are: Dean Pesnell, SDO project scientist, Goddard Space Flight Center in Greenbelt, Md.; Alan Title, principal investigator, Atmospheric Imaging Assembly instrument, Lockheed Martin Solar and Astrophysics Laboratory in Palo Alto; Philip H. Scherrer, principal investigator, Helioseismic and Magnetic Imager instrument, Stanford University in Palo Alto; Tom Woods, principal investigator, Extreme Ultraviolet Variability Experiment Instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder and Madhulika Guhathakurta, SDO program scientist, NASA Headquarters in Washington. Photo Credit: (NASA/Carla Cioffi)

The Plasma and Suprathermal Ion Composition (PLASTIC) Investigation on the STEREO Observatories

NASA Astrophysics Data System (ADS)

Galvin, A. B.; Kistler, L. M.; Popecki, M. A.; Farrugia, C. J.; Simunac, K. D. C.; Ellis, L.; Möbius, E.; Lee, M. A.; Boehm, M.; Carroll, J.; Crawshaw, A.; Conti, M.; Demaine, P.; Ellis, S.; Gaidos, J. A.; Googins, J.; Granoff, M.; Gustafson, A.; Heirtzler, D.; King, B.; Knauss, U.; Levasseur, J.; Longworth, S.; Singer, K.; Turco, S.; Vachon, P.; Vosbury, M.; Widholm, M.; Blush, L. M.; Karrer, R.; Bochsler, P.; Daoudi, H.; Etter, A.; Fischer, J.; Jost, J.; Opitz, A.; Sigrist, M.; Wurz, P.; Klecker, B.; Ertl, M.; Seidenschwang, E.; Wimmer-Schweingruber, R. F.; Koeten, M.; Thompson, B.; Steinfeld, D.

2008-04-01

The Plasma and Suprathermal Ion Composition (PLASTIC) investigation provides the in situ solar wind and low energy heliospheric ion measurements for the NASA Solar Terrestrial Relations Observatory Mission, which consists of two spacecraft (STEREO-A, STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is a time-of-flight/energy mass spectrometer designed to determine the elemental composition, ionic charge states, and bulk flow parameters of major solar wind ions in the mass range from hydrogen to iron. PLASTIC has nearly complete angular coverage in the ecliptic plane and an energy range from ˜0.3 to 80 keV/e, from which the distribution functions of suprathermal ions, including those ions created in pick-up and local shock acceleration processes, are also provided.

Magnetic flux transport of decaying active regions and enhanced magnetic network. [of solar supergranulation

NASA Technical Reports Server (NTRS)

Wang, Haimin; Zirin, Harold; Ai, Guoxiang

1991-01-01

Several series of coordinated observations on decaying active regions and enhanced magnetic network regions on the sun were carried out jointly at Big Bear Solar Observatory and at the Huairou Solar Observing Station of the Bejing Astronomical Observatory in China. The magnetic field evolution in several regions was followed closely for three to seven days. The magnetic flux transport from the remnants of decayed active regions was studied, along with the evolution and lifetime of the magnetic network which defines the boundaries of supergranules. The magnetic flux transport in an enhanced network region was studied in detail and found to be negative. Also briefly described are some properties of moving magnetic features around a sunspot. Results of all of the above studies are presented.

The detection of global convection on the sun by an analysis of line shift data of the John M. Wilcox Solar Observatory at Stanford University

NASA Technical Reports Server (NTRS)

Yoshimura, Hirokazu

1987-01-01

An analysis of the absorption line shift data of the John M. Wilcox Solar Observatory at Stanford University has yielded signatures of the existence of global convection on the sun. These include persistent periodic time variations in the east-west component of the velocity fields defined by fitting a slope to the line shift data in a certain longitude window at a specified latitude and longitude by the least squares method. The amplitude of the velocity fields estimated from these variations is of the order of 100 m/s. The results of the analysis also suggest that several modes of global convection coexist in the solar convection zone. Details of the analysis are given.

Global Oscillation Network Group

NASA Astrophysics Data System (ADS)

Murdin, P.

2000-11-01

The Global Oscillation Network Group (GONG) is an international, community-based project, operated by the NATIONAL SOLAR OBSERVATORY for the US National Science Foundation, to conduct a detailed study of the internal structure and dynamics of the Sun over an 11 year solar cycle using helioseismology. 10 242 velocity images are obtained by a six-station network located at Big Bear Solar Observato...

Right Limb of the South Pole of the Sun, March 18, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

Left Limb of North Pole of the Sun, March 20, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

Closer View of the Equatorial Region of the Sun, March 24, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

Designing Solar Data Archives: Practical Considerations

NASA Astrophysics Data System (ADS)

Messerotti, M.

The variety of new solar observatories in space and on the ground poses the stringent problem of an efficient storage and archiving of huge datasets. We briefly address some typical architectures and consider the key point of data access and distribution through networking.

Solar Demon: near real-time Flare, Dimming and EUV wave monitoring

NASA Astrophysics Data System (ADS)

Kraaikamp, Emil; Verbeeck, Cis

Dimmings and EUV waves have been observed routinely in EUV images since 1996. They are closely associated with coronal mass ejections (CMEs), and therefore provide useful information for early space weather alerts. On the one hand, automatic detection and characterization of dimmings and EUV waves can be used to gain better understanding of the underlying physical mechanisms. On the other hand, every dimming and EUV wave provides extra information on the associated front side CME, and can improve estimates of the geo-effectiveness and arrival time of the CME. Solar Demon has been designed to detect and characterize dimmings, EUV waves, as well as solar flares in near real-time on Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) data. The detection modules are running continuously at the Royal Observatory of Belgium on both quick-look data, as well as synoptic science data. The output of Solar Demon can be accessed in near real-time on the Solar Demon website, and includes images, movies, light curves, and the numerical evolution of several parameters. Solar Demon is the result of collaboration between the FP7 projects AFFECTS and COMESEP. Flare detections of Solar Demon are integrated into the COMESEP alert system. Here we present the Solar Demon detection algorithms and their output. We will show several interesting flare, dimming and EUV wave events, and present general statistics of the detections made so far during solar cycle 24.

Skylab and the Sun

NASA Technical Reports Server (NTRS)

1973-01-01

Articles pertaining to the solar studies and the Skylab program are presented, with emphasis on the usefulness of the Apollo Telescope Mount (ATM) program. A description of Skylab objectives and key mission events is included along with articles about the sun. Skylab solar studies which are reported include these topics: ATM solar observatory, scientific instruments, crew operations and crew training, and the joint observing program. The Skylab associated solar programs are also reported.

Amateur observations of solar eclipses and derivation of scientific data

NASA Astrophysics Data System (ADS)

Stoev, A. D.; Stoeva, P. V.

2008-12-01

This work presents the educational approach of using total solar eclipse occurrences as a scientific process learning aid. The work reviews the basic scientific aims and experiments included in the observational programs "Total solar eclipse 1999 and 2006" (Stoev, A., Kiskinova, N., Muglova, P. et al. Complex observational programme of the Yuri Gagarin Public Astronomical Observatory and STIL, BAS, Stara Zagora Department for the August 11, 1999 total solar eclipse, in: Total Solar Eclipse 1999 - Observational Programmes and Coordination, Proceedings, Recol, Haskovo, pp. 133-137, 1999a (in Bulgarian); Stoeva, P.V., Stoev, A.D., Kostadinov, I.N. et al. Solar Corona and Atmospheric Effects during the March 29, 2006 Total Solar Eclipse, in: 11th International Science Conference SOLAR-Terrestrial Influences, Sofia, November 24-25, pp. 69-72, 2005). Results from teaching and training the students in the procedures, methods and equipment necessary for the observation of a total solar eclipse (TSE) at the Yuri Gagarin Public Astronomical Observatory (PAO) in Stara Zagora, Bulgaria, as well as the selection process used in determining participation in the different observational teams are discussed. The final stages reveal the special methodology used to investigate the level of "pretensions", the levels of ambition displayed by the students in achieving each independent goal, and the setting of goals in context with their problem solving capabilities and information gathering abilities in the scientific observation process. Results obtained from the observational experiments are interpreted mainly in the following themes: Investigation of the structure of the white-light solar corona and evolution of separate coronal elements during the total phase of the eclipse; Photometry of the white-light solar corona and specific emission lines; Meteorological, actinometrical and optical atmospheric investigations; Astrometry of the Moon during the phase evolution of the eclipse and Biological and behavioral reactions of highly organized colonies (ants and bats) during the eclipse. It is also shown that the students benefit from the activities of processing data, observational results and their interpretation, and preparation of summary reports. This exercise is intended to provide the basic training necessary to develop the creativity of the students and amateur astronomers involved. This will enable the students from the Astronomy schools at Public Astronomical Observatories and Planetaria (PAOP) to further develop their creative skills, emotional-volitional personal qualities with an orientation towards scientific analysis, using observations and experiments, to build an effective scientific style of thinking. Students of the Yuri Gagarin Public Astronomical Observatory, whom are already being nurtured in this manner, should be able to participate with great success in Scientific Research Programs devoted to the International Heliophysical Year.

The Solar Connections Observatory for Planetary Environments

NASA Technical Reports Server (NTRS)

Oliversen, Ronald J.; Harris, Walter M.; Oegerle, William R. (Technical Monitor)

2002-01-01

The NASA Sun-Earth Connection theme roadmap calls for comparative study of how the planets, comets, and local interstellar medium (LISM) interact with the Sun and respond to solar variability. Through such a study we advance our understanding of basic physical plasma and gas dynamic processes, thus increasing our predictive capabilities for the terrestrial, planetary, and interplanetary environments where future remote and human exploration will occur. Because the other planets have lacked study initiatives comparable to the terrestrial ITM, LWS, and EOS programs, our understanding of the upper atmospheres and near space environments on these worlds is far less detailed than our knowledge of the Earth. To close this gap we propose a mission to study {\\it all) of the solar interacting bodies in our planetary system out to the heliopause with a single remote sensing space observatory, the Solar Connections Observatory for Planetary Environments (SCOPE). SCOPE consists of a binocular EUV/FUV telescope operating from a remote, driftaway orbit that provides sub-arcsecond imaging and broadband medium resolution spectro-imaging over the 55-290 nm bandpass, and high (R>10$^{5}$ resolution H Ly-$\\alpha$ emission line profile measurements of small scale planetary and wide field diffuse solar system structures. A key to the SCOPE approach is to include Earth as a primary science target. From its remote vantage point SCOPE will be able to observe auroral emission to and beyond the rotational pole. The other planets and comets will be monitored in long duration campaigns centered when possible on solar opposition when interleaved terrestrial-planet observations can be used to directly compare the response of both worlds to the same solar wind stream and UV radiation field. Using a combination of observations and MHD models, SCOPE will isolate the different controlling parameters in each planet system and gain insight into the underlying physical processes that define the solar connection.

The disturbed geomagnetic field at European observatories. Sources and significance

NASA Astrophysics Data System (ADS)

Greculeasa, Razvan; Dobrica, Venera; Demetrescu, Crisan

2014-05-01

The disturbed geomagnetic field recorded at Earth's surface is given by the effects of electric current systems in the magnetosphere and ionosphere, as a result of the interaction of geomagnetic field with the solar wind and the interplanetary magnetic field. In this paper the geomagnetic disturbance recorded at European observatories has been investigated as regards its sources, for the time interval August 1-10, 2010, in which a moderate storm (Dstmin= -70 nT) occurred (August 3-4). The disturbance has been evidenced against the solar quiet daily variation, for each of the 29 observatories with minute data in the mentioned time interval. Data have been downloaded from the INTERMAGNET web page. The contribution of the magnetospheric ring current and of the auroral electrojet to the observed disturbance field in the X, Z, and D geomagnetic elements is discussed and the corresponding geographical distribution is presented.

Arctic Haze: A Chemical, Physical, Optical and Meteorological Study

DTIC Science & Technology

1976-08-01

Interior 01-31-77 Alaska 03-6-022-35154 Radiation NOA 02-01-76 $18,485 3 mos. Studies at Mauna Loa 01-31-77 Observatory -P6’- Title Agen Period Amou i...Pending Ainlications Radiation Studies at Mauna Loa NOA I year $21,069 Observatory Study of Non-Resonant NSF 1 year $I1,5 99 Scattered Sunlight at...Shaw, G.E. Solar radiation research being carried out at the Mauna Loa Observatory. Presented at the conference on Global Monitoring for Climatic Change

Close-up View of an Active Region of the Sun, March 23, 2007 Anaglyph

NASA Image and Video Library

2007-04-27

NASA Solar TErrestrial RElations Observatory satellites have provided the first 3-dimensional images of the Sun. This view will aid scientists ability to understand solar physics to improve space weather forecasting. 3D glasses are necessary.

The Legacy of the Georgetown College Observatory (D.C.)

NASA Astrophysics Data System (ADS)

Caron, Laura; Maglieri, Grace; Seitzer, Patrick

2018-01-01

Founded in 1841 as part of a nascent worldwide network of Jesuit-run astronomical observatories, the Georgetown College Observatory of Georgetown University in Washington, D.C. has been home to more than 125 years of astronomical research, from Father Curley’s calculations of the latitude and longitude of D.C. to Father McNally’s award-winning solar eclipse photography. But the impact of the Georgetown astronomy program was not limited to the observatory itself: it reached much further, into the local community and schools, and into the lives of everyone involved. This was never more apparent than under the directorship of Father Francis J Heyden, S.J., who arrived at Georgetown after World War II and stayed for almost three decades. He started a graduate program with over 90 graduates, hosting student researchers from local high schools and colleges, teaching graduate and undergraduate astronomy courses, and speaking at schools in the area, all while simultaneously managing Georgetown’s student radio station and hosting astronomical conferences on campus. Father Heyden’s research focused mainly on solar eclipses for geodetic purposes and planetary spectroscopy. But perhaps even more than research, Father Heyden dedicated his time and energy to the astronomy students, the notable of which include Vera Rubin, John P. Hagen of Project Vanguard, and a generation of Jesuit astronomers including Martin McCarthy, George Coyne, and Richard Boyle. Following the closure of the astronomy department in 1972, Father Heyden returned to Manila, where he had begun his astronomical career, to become Chief of the Solar Division at the Manila Observatory. His dedication to his work and to students serves as an inspiration for academic researchers across fields, and for the Georgetown University Astronomical Society, which, even in the absence of a formal astronomy program at Georgetown, continues his work in education and outreach today. In 1987, almost 150 years after its founding, Georgetown College Observatory was rededicated in Father Heyden’s name.

The Mercury Transit 2016: educational activities from CESAR

NASA Astrophysics Data System (ADS)

Pérez-Ayúcar, Miguel; Breitfelner, Michel

2017-04-01

A transit of Mercury in front of the solar disk as seen from Earth is a rare astronomical event which occurs only about every 13-14 times per century. Although its historic scientific importance, e.g. to measure the distances in the solar system, has diminished since humanity roams our solar system with robotic spacecrafts, a Mercury Transit remains a spectacular astronomical event that is used very effectively to engage general public and students to Science and Space in general. The educational project CESAR (Cooperation through Education in Science and Astronomy Research) , working upon previous experience (Venus transit 2012, live Sun transmissions ..), prepared a dual observation of the transit from two separate locations: the CESAR Solar Observatory at ESAC (European Space Astronomy Center), Madrid, Spain, and a twin portable telescope set-up in Cerro Paranal, Chile, achieving a ground baseline parallax of 10.000km. CESAR organized an educational and outreach event in collaboration with several Spanish schools/universities, the ESA Education and Communications offices, the Teide observatory and the ESA projects Bepi Colombo and Solar Orbiter. The driving activity was a continuous 10h interactive Google hangout that connected students in Spain (Ciudad de las Artes y las Ciencias, CAC in Valencia), students in observatories in Chile, the remote observing teams, and scientists at ESAC. Live images were transmitted via a specific web in two bands (h-alpha and visible). Experts in the fields of Solar and Planetary Physics gave presentations related to the Sun and Mercury. Questions and answers sessions were performed so that world-wide audience could interact with the scientists and engineers. In this paper we explain how this public educational and outreach event was created, what activities it comprised, and the follow up activities.

Design and Construction of a Solar Observatory in a Liberal Arts Environment: Austin College’s Gnomon and Meridian Line

NASA Astrophysics Data System (ADS)

Baker, David; Salisbury, D.

2014-01-01

Austin College’s indoor solar observatory is one of the most distinctive features in its new IDEA Center science building. Patterned after 16th and 17th century solar observatories in European cathedrals, the IDEA Center solar facility will be used extensively for public events, introductory astronomy courses, and reproductions of important historical scientific measurements. A circular aperture, or gnomon hole, on the roof with diameter 32 mm allows a beam of sunlight to trace a path across the atrium floor 15.37 meters below. At local solar noon, the Sun’s image falls directly on a brass meridian line. Special markers for solstices and equinoxes highlight western, eastern, and indigenous cultural contributions to astronomy: Macedonian symbol of the Sun marks summer solstice, Chinese Sun symbol showcases the equinoxes, and the Mayan symbol of the Sun celebrates winter solstice. The location directly beneath the gnomon hole is marked by the universal scientific symbol of the Sun. Direct solar measurements and mathematical models were used in design and implementation of the meridian line. During IDEA Center building construction in Fall 2012, undergraduate students measured the Sun’s position at various times. The finished floor was set in February 2013, well before a full year’s worth of measurements could be recorded. A mathematical model including the effects of aperture size and atmospheric refraction was needed to predict the size and location of the Sun on the meridian line throughout the year. Confirmation of the meridian line occurred on Summer Solstice 2013 when the Sun’s image precisely hit the Macedonian marker at the correct time.

Low-Latitude Solar Coronal Hole Formation

NASA Astrophysics Data System (ADS)

Haislmaier, Karl; Petrie, G.

2013-01-01

Little is known about the origin of low-latitude solar coronal holes (CHs) and their relation to the magnetic flux distribution of the underlying Solar Photosphere. Two recent reports (Karachik et al. 2010, Wang et al. 2010) suggest that CH formation might be correlated with the decay of active regions (ARs) in the photosphere. In order to explore the nature and extent of such correlations, we surveyed GONG (Global Oscillations Network Group) synoptic magnetograms and STEREO (Solar TErrestrial RElations Observatory) synoptic extreme ultraviolet images of Carrington rotations 2047-2112. From these two data sets, 41 AR-CH pairs were identified, accounting for ~34% of all ARs that appeared during the surveyed rotations. Each of these AR-CH pairs fell into one of two general classes: 1) those where the CHs were associated with the leading polarity fluxes of decaying ARs whose lagging fluxes largely decayed away, and 2) those where the CHs were associated with the lagging fluxes of surviving ARs. Perhaps surprisingly, the positive and negative fluxes of the ARs generally remained well balanced after their CHs developed. Extrapolated coronal potential-field source-surface (PFSS) models linked the CH creation and development to changes in magnetic connectivity with the surroundings as the AR flux became more diffuse over time. These considerations lead us to conclude that CHs are associated with low intensity, unipolar magnetic flux regions in the photosphere, which are most readily created by the turbulent diffusion and decay of AR flux. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation.

Building for the Future: China’s Progress in Space Technology During the Tenth 5-Year Plan and the U.S. Response

DTIC Science & Technology

2008-03-01

solar telescope to study solar physics. — Develop technologies for a three-satellite constellation called Kua Fu to study solar activity that will...consist of one satellite to monitor solar activity and two others to study the aurora. • International cooperation. Participate in the Sino...Russian Mars environment exploration plan, the World Space Observatory Ultraviolet Project,50 and the Sino-French Small Satellite Solar Flare Exploration

Skylab

NASA Image and Video Library

1974-07-26

In this photograph, a skylab-4 astronaut performs Extra Vehicular Activities (EVA) outside of the lab. The third crew (Skylab-4) spent 84 days in the orbiting laboratory. The solar observatory was designed for full exposure to the Sun throughout most of the Skylab mission. Solar energy was transformed into electrical power for operation of all spacecraft systems. The proper operation of these solar arrays was vital to the mission.

Skylab

NASA Image and Video Library

1974-01-01

This photograph was taken as the third crew (Skylab-4) departed the space station. The solar observatory was designed for full exposure to the Sun throughout most of the Skylab mission. Solar energy was transformed into electrical power for operation of all spacecraft systems. The proper operation of these solar arrays was vital to the mission. This Skylab in orbit view was taken by the Skylab-4 crew.

Simultaneous Observation of Solar Neutrons at the ISS and High Mountain Observatories as Evidence for two Different Acceleration Mechanisms Associated to a Flare on July 8,2014

NASA Astrophysics Data System (ADS)

Valdes-Galicia, J. F.; González, L. X.; Watanabe, K.; Muraki, Y.; Matsubara, Y.; Lopez, D.; Koga, K.; Kakimoto, F.; Sako, T.; Salinas, J., Sr.; Ticona, R.; Shibata, S.; Masuda, S.; Tunesada, S.

2016-12-01

An M 6.5-class flare was observed at N12E56 of the solar surface at 16:06 UT on July 8, 2014. In association with the flare, two neutron detectors located at high mountains: Mt. Sierra Negra in Mexico (4600m asl) and Mt. Chacaltaya in Bolivia (5200m asl) recorded two neutron pulses, separated approximately 30 minutes. Enhancements were also observed in the neutral channel detector onboard the International Space Station. We analyzed these data combined with solar images from the Atompspheric ImagingAssembly (AIA) onboard the SolarDynamicalObservatory (SDO). From our analysis we conclude that the production mechanism of neutrons cannot be explained by a single model: one of the enhancements may be explained by an electric field generated by the collision of magnetic loops, and the other by a shock acceleration mechanism at the front side of the observed CME. To the best of our knowledge, this is the first time that evidence is found for two different mechanisms present in a solar eruption leading to energetic solar neutron production.

Astrophysical Sources of Cosmic Rays and Related Measurements with the Pierre Auger Observatory

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

Abraham, : J.; Abreu, P.; Aglietta, M.

2009-06-01

These are presentations to be presented at the 31st International Cosmic Ray Conference, in Lodz, Poland during July 2009. It consists of the following presentations: (1) Correlation of the highest energy cosmic rays with nearby extragalactic objects in Pierre Auger Observatory data; (2) Discriminating potential astrophysical sources of the highest energy cosmic rays with the Pierre Auger Observatory; (3) Intrinsic anisotropy of the UHECR from the Pierre Auger Observatory; (4) Ultra-high energy photon studies with the Pierre Auger Observatory; (5) Limits on the flux of diffuse ultra high energy neutrinos set using the Pierre Auger Observatory; (6) Search for siderealmore » modulation of the arrival directions of events recorded at the Pierre Auger Observatory; (7) Cosmic Ray Solar Modulation Studies in the Pierre Auger Observatory; (8) Investigation of the Displacement Angle of the Highest Energy Cosmic Rays Caused by the Galactic Magnetic Field; (9) Search for coincidences with astrophysical transients in Pierre Auger Observatory data; and (10) An alternative method for determining the energy of hybrid events at the Pierre Auger Observatory.« less

Electron beams in solar flares

NASA Technical Reports Server (NTRS)

Aschwanden, Markus J.; Dennis, Brian R.; Benz, Arnold O.

1994-01-01

A list of publications resulting from this program includes 'The Timing of Electron Beam Signatures in Hard X-Ray and Radio: Solar Flare Observations by BATSE/Compton Gamma-Ray Observatory and PHOENIX'; 'Coherent-Phase or Random-Phase Acceleration of Electron Beams in Solar Flares'; 'Particle Acceleration in Flares'; 'Chromospheric Evaporation and Decimetric Radio Emission in Solar Flares'; 'Sequences of Correlated Hard X-Ray and Type 3 Bursts During Solar Flares'; and 'Solar Electron Beams Detected in Hard X-Rays and Radiowaves.' Abstracts and reprints of each are attached to this report.

Estimation of the state of solar activity type stars by virtual observations of CrAVO

NASA Astrophysics Data System (ADS)

Dolgov, A. A.; Shlyapnikov, A. A.

2012-05-01

The results of precosseing of negatives with direct images of the sky from CrAO glass library are presented in this work, which became a part of on-line archive of the Crimean Astronomical Virtual Observatory (CrAVO). Based on the obtained data, the parameters of dwarf stars have been estimated, included in the catalog "Stars with solar-type activity" (GTSh10). The following matters are considered: searching methodology of negatives with positions of studied stars and with calculated limited magnitude; image viewing and reduction with the facilities of the International Virtual Observatory; the preliminary results of the photometry of studied objects.

Accessing SDO data in a pipeline environment using the VSO WSDL/SOAP interface

NASA Astrophysics Data System (ADS)

Suarez Sola, F. I.; Hourcle, J. A.; Amezcua, A.; Bogart, R.; Davey, A. R.; Gurman, J. B.; Hill, F.; Hughitt, V. K.; Martens, P. C.; Spencer, J.; Vso Team

2010-12-01

As part of the Virtual Solar Observatory (VSO) effort to support the Solar Dynamics Observatory (SDO) data, the VSO has worked on bringing up to date its WSDL document and SOAP interface to make it compatible with most widely used web services core engines. (E.g. axis2, jws, etc.) In this presentation we will explore the possibilities available for searching and/or fetching data within pipeline code. We will explain some of the WSDL/VSO-SDO interface intricacies and show how the vast amount of data that is available via the VSO can be tapped via IDL, Java, Perl or C in an uncomplicated way.

Mechanisms and Observations of Coronal Dimming for the 2010 August 7 Event

NASA Technical Reports Server (NTRS)

Mason, James P.; Woods, Thomas N.; Caspi, Amir; Thompson, Barbara J.; Hock, Rachel A.

2014-01-01

Coronal dimming of extreme ultraviolet (EUV) emission has the potential to be a useful forecaster of coronal mass ejections (CMEs). As emitting material leaves the corona, a temporary void is left behind which can be observed in spectral images and irradiance measurements. The velocity and mass of the CMEs should impact the character of those observations. However, other physical processes can confuse the observations. We describe these processes and the expected observational signature, with special emphasis placed on the differences. We then apply this understanding to a coronal dimming event with an associated CME that occurred on 2010 August 7. Data from the Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA) and EUV Variability Experiment (EVE) are used for observations of the dimming, while the Solar and Heliospheric Observatory's (SoHO) Large Angle and Spectrometric Coronagraph (LASCO) and the Solar Terrestrial Relations Observatory's (STEREO) COR1 and COR2 are used to obtain velocity and mass estimates for the associated CME. We develop a technique for mitigating temperature effects in coronal dimming from full-disk irradiance measurements taken by EVE. We find that for this event, nearly 100% of the dimming is due to mass loss in the corona.

The MEXART ips observations in route to the next solar maximum

NASA Astrophysics Data System (ADS)

Carrillo-Vargas, Armando; Gonzalez-Esparza, Americo; Andrade, Ernesto; Perez-Enriquez, Roman; Aguilar-Rodriguez, Ernesto; Casillas-Perez, Gilberto; Jeyakumar, Solai; Kurtz, Stanley; Sierra, Pablo; Vazquez, Samuel

We report the status of the Mexican Array Radio Telescope (MEXART) in preparation for the next solar maximum. During this epoch, the MEXART will be one of the four dedicated radio telescopes (with the ORT in India; STEL in Japan; and MWA in Australia) to track large-scale structures in the solar wind using the interplanetary scintillation (IPS) technique. This network of IPS observatories would produce, for the first time four g maps of the sky showing the size and shape of disturbances between the Sun and the Earth. We describe the operation and current observations of the first IPS radio sources at 140 MHz detected by the MEXART. These observations use a plane dipole array of 1024 elements (16 lines with 64 dipoles each one), feeding a Butler matrix of 16x16 ports. This system generates a 16 lobes at fixed declinations covering 120 degrees (from 40 degrees South to 80 degrees North). The beam fan uses the Earth's rotation to cover the whole sky. The observations that will be made with the network of observatories of interplanetary flashing will complement the observations of other observatories, instruments in situ, space probes, satellite, among others.

First Simultaneous Views of the Axial and Lateral Perspectives of a Coronal Mass Ejection

NASA Astrophysics Data System (ADS)

Cabello, I.; Cremades, H.; Balmaceda, L.; Dohmen, I.

2016-08-01

The different appearances exhibited by coronal mass ejections (CMEs) are believed to be in part the result of different orientations of their main axis of symmetry, consistent with a flux-rope configuration. There are observational reports of CMEs seen along their main axis (axial perspective) and perpendicular to it (lateral perspective), but no simultaneous observations of both perspectives from the same CME have been reported to date. The stereoscopic views of the telescopes onboard the Solar-Terrestrial Relations Observatory (STEREO) twin spacecraft, in combination with the views from the Solar and Heliospheric Observatory (SOHO) and the Solar Dynamics Observatory (SDO), allow us to study the axial and lateral perspectives of a CME simultaneously for the first time. In addition, this study shows that the lateral angular extent ( L) increases linearly with time, while the angular extent of the axial perspective ( D) presents this behavior only from the low corona to {≈} 5 R_{⊙}, where it slows down. The ratio L/D ≈ 1.6 obtained here as the average over several points in time is consistent with measurements of L and D previously performed on events exhibiting only one of the perspectives from the single vantage point provided by SOHO.

All About EVE: Education and Public Outreach for the Extreme Ultraviolet Variability Experiment (EVE) of the NASA Solar Dynamic Observatory

NASA Astrophysics Data System (ADS)

Eparvier, F. G.; McCaffrey, M. S.; Buhr, S. M.

2008-12-01

With the aim of meeting NASA goals for education and public outreach as well as support education reform efforts including the National Science Education Standards, a suite of education materials and strategies have been developed by the Cooperative Institute for Environmental Sciences (CIRES) with the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado for the Extreme Ultraviolet Variability Experiment (EVE), which is an instrument aboard the Solar Dynamic Observatory. This paper will examine the education materials that have been developed for teachers in the classroom and scientists who are conducting outreach, including handouts, a website on space weather for teachers, a slideshow presentation about the overall Solar Dynamic Observatory mission, and a DVD with videos explaining the construction and goals of the EVE instrument, a tour of LASP, and an overview of space science careers. The results and potential transferability of a pilot project developed through this effort that engaged English Second Language learners in a semester-long course on space weather that incorporated the used of a Sudden Ionospheric Disturbance (SID) Monitor will be highlighted.

Mechanisms and observations of coronal dimming for the 201 August 7 event

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

Mason, James Paul; Woods, T. N.; Caspi, A.

2014-07-01

Coronal dimming of extreme ultraviolet (EUV) emission has the potential to be a useful forecaster of coronal mass ejections (CMEs). As emitting material leaves the corona, a temporary void is left behind which can be observed in spectral images and irradiance measurements. The velocity and mass of the CMEs should impact the character of those observations. However, other physical processes can confuse the observations. We describe these processes and the expected observational signature, with special emphasis placed on the differences. We then apply this understanding to a coronal dimming event with an associated CME that occurred on 2010 August 7.more » Data from the Solar Dynamics Observatory's Atmospheric Imaging Assembly and EUV Variability Experiment (EVE) are used for observations of the dimming, while the Solar and Heliospheric Observatory's Large Angle and Spectrometric Coronagraph and the Solar Terrestrial Relations Observatory's COR1 and COR2 are used to obtain velocity and mass estimates for the associated CME. We develop a technique for mitigating temperature effects in coronal dimming from full-disk irradiance measurements taken by EVE. We find that for this event, nearly 100% of the dimming is due to mass loss in the corona.« less

Computer Vision for the Solar Dynamics Observatory (SDO)

NASA Astrophysics Data System (ADS)

Martens, P. C. H.; Attrill, G. D. R.; Davey, A. R.; Engell, A.; Farid, S.; Grigis, P. C.; Kasper, J.; Korreck, K.; Saar, S. H.; Savcheva, A.; Su, Y.; Testa, P.; Wills-Davey, M.; Bernasconi, P. N.; Raouafi, N.-E.; Delouille, V. A.; Hochedez, J. F.; Cirtain, J. W.; Deforest, C. E.; Angryk, R. A.; de Moortel, I.; Wiegelmann, T.; Georgoulis, M. K.; McAteer, R. T. J.; Timmons, R. P.

2012-01-01

In Fall 2008 NASA selected a large international consortium to produce a comprehensive automated feature-recognition system for the Solar Dynamics Observatory (SDO). The SDO data that we consider are all of the Atmospheric Imaging Assembly (AIA) images plus surface magnetic-field images from the Helioseismic and Magnetic Imager (HMI). We produce robust, very efficient, professionally coded software modules that can keep up with the SDO data stream and detect, trace, and analyze numerous phenomena, including flares, sigmoids, filaments, coronal dimmings, polarity inversion lines, sunspots, X-ray bright points, active regions, coronal holes, EIT waves, coronal mass ejections (CMEs), coronal oscillations, and jets. We also track the emergence and evolution of magnetic elements down to the smallest detectable features and will provide at least four full-disk, nonlinear, force-free magnetic field extrapolations per day. The detection of CMEs and filaments is accomplished with Solar and Heliospheric Observatory (SOHO)/ Large Angle and Spectrometric Coronagraph (LASCO) and ground-based Hα data, respectively. A completely new software element is a trainable feature-detection module based on a generalized image-classification algorithm. Such a trainable module can be used to find features that have not yet been discovered (as, for example, sigmoids were in the pre- Yohkoh era). Our codes will produce entries in the Heliophysics Events Knowledgebase (HEK) as well as produce complete catalogs for results that are too numerous for inclusion in the HEK, such as the X-ray bright-point metadata. This will permit users to locate data on individual events as well as carry out statistical studies on large numbers of events, using the interface provided by the Virtual Solar Observatory. The operations concept for our computer vision system is that the data will be analyzed in near real time as soon as they arrive at the SDO Joint Science Operations Center and have undergone basic processing. This will allow the system to produce timely space-weather alerts and to guide the selection and production of quicklook images and movies, in addition to its prime mission of enabling solar science. We briefly describe the complex and unique data-processing pipeline, consisting of the hardware and control software required to handle the SDO data stream and accommodate the computer-vision modules, which has been set up at the Lockheed-Martin Space Astrophysics Laboratory (LMSAL), with an identical copy at the Smithsonian Astrophysical Observatory (SAO).

MLSO Mark III K-Coronameter Observations of the CME Rate from 1989-1996

NASA Technical Reports Server (NTRS)

St Cyr, O. C.; Flint, Q. A.; Xie, H.; Webb, D. F.; Burkepile, J. T.; Lecinski, A. R.; Quirk, C.; Stanger, A. L.

2015-01-01

We report here an attempt to fill the 1990-1995 gap in the CME (coronal mass ejection) rate using the Mauna Loa Solar Observatory (MLSO)'s Mark III (Mk3) K-coronameter. The Mk3 instrument observed routinely several hours most days beginning in 1980 until it was upgraded to Mk4 in 1999. We describe the statistical properties of the CMEs detected during 1989-1996, and we determine a CME rate for each of those years. Since spaceborne coronagraphs have more complete duty cycles than a ground-based instrument at a single location, we compare the Mk3-derived CME rate from 1989 with the SMM C/P (Solar Maximum Mission Coronagraph/Polarimeter) coronagraph, and from 1996 with the SOHO (Solar and Hellospheric Observatory) LASCO (Large Angle and Spectrometric COronagraph) coronagraphs.

Virtual Solar Observatory Distributed Query Construction

NASA Technical Reports Server (NTRS)

Gurman, J. B.; Dimitoglou, G.; Bogart, R.; Davey, A.; Hill, F.; Martens, P.

2003-01-01

Through a prototype implementation (Tian et al., this meeting) the VSO has already demonstrated the capability of unifying geographically distributed data sources following the Web Services paradigm and utilizing mechanisms such as the Simple Object Access Protocol (SOAP). So far, four participating sites (Stanford, Montana State University, National Solar Observatory and the Solar Data Analysis Center) permit Web-accessible, time-based searches that allow browse access to a number of diverse data sets. Our latest work includes the extension of the simple, time-based queries to include numerous other searchable observation parameters. For VSO users, this extended functionality enables more refined searches. For the VSO, it is a proof of concept that more complex, distributed queries can be effectively constructed and that results from heterogeneous, remote sources can be synthesized and presented to users as a single, virtual data product.

Astronomy and astrophysics communication in the UCM Observatory

NASA Astrophysics Data System (ADS)

Crespo-Chacón, I.; de Castro, E.; Díaz, C.; Gallego, J.; Gálvez, M. C.; Hernán-Obispo, M.; López-Santiago, J.; Montes, D.; Pascual, S.; Verdet, A.; Villar, V.; Zamorano, J.

We present a summary of the last activities of science communication that have taken place in the Observatorio de la Universidad Complutense de Madrid (UCM Observatory) on the occasion of the Third Science Week of the Comunidad Autónoma de Madrid (3-16 November 2003), including guided tours through the observatory facilities, solar observations, and several talks. Moreover the current telescopes, instruments and tools of the UCM Observatory have allowed us to organize other communicating activities such as the live observation, together with its internet broadcast, of total lunar eclipses and other exceptional astronomical events as the Venus transit that took place in 8 June 2004.

The BATSE experiment on the Gamma Ray Observatory: Solar flare hard x ray and gamma-ray capabilities

NASA Technical Reports Server (NTRS)

Fishman, G. J.; Meegan, C. A.; Wilson, R. B.; Parnell, T. A.; Paciesas, W. S.; Pendleton, G. N.; Hudson, H. S.; Matteson, J. L.; Peterson, L. E.; Cline, T. L.

1989-01-01

The Burst and Transient Source Experiment (BATSE) for the Gamma Ray Observatory (GRO) consists of eight detector modules that provide full-sky coverage for gamma-ray bursts and other transient phenomena such as solar flares. Each detector module has a thin, large-area scintillation detector (2025 sq cm) for high time-resolution studies, and a thicker spectroscopy detector (125 sq cm) to extend the energy range and provide better spectral resolution. The total energy range of the system is 15 keV to 100 MeV. These 16 detectors and the associated onboard data system should provide unprecedented capabilities for observing rapid spectral changes and gamma-ray lines from solar flares. The presence of a solar flare can be detected in real-time by BATSE; a trigger signal is sent to two other experiments on the GRO. The launch of the GRO is scheduled for June 1990, so that BATSE can be an important component of the Max '91 campaign.

CME Dynamics Using STEREO and LASCO Observations: The Relative Importance of Lorentz Forces and Solar Wind Drag

NASA Astrophysics Data System (ADS)

Sachdeva, Nishtha; Subramanian, Prasad; Vourlidas, Angelos; Bothmer, Volker

2017-09-01

We seek to quantify the relative contributions of Lorentz forces and aerodynamic drag on the propagation of solar coronal mass ejections (CMEs). We use Graduated Cylindrical Shell (GCS) model fits to a representative set of 38 CMEs observed with the Solar and Heliospheric Observatory (SOHO) and the Solar and Terrestrial Relations Observatory (STEREO) spacecraft. We find that the Lorentz forces generally peak between 1.65 and 2.45 R⊙ for all CMEs. For fast CMEs, Lorentz forces become negligible in comparison to aerodynamic drag as early as 3.5 - 4 R⊙. For slow CMEs, however, they become negligible only by 12 - 50 R⊙. For these slow events, our results suggest that some of the magnetic flux might be expended in CME expansion or heating. In other words, not all of it contributes to the propagation. Our results are expected to be important in building a physical model for understanding the Sun-Earth dynamics of CMEs.

Economic and technical aspects of repair, servicing, and retrieval of low earth orbit free flying spacecraft

NASA Technical Reports Server (NTRS)

Cepollina, F. J.

1982-01-01

The economic and technical aspects of the Solar Maximum Observatory Repair Mission at NASA are presented, in an effort to demonstrate the Space Shuttle capability to rendezvous with and repair on-orbit the Solar Maximum Observatory (SMM). A failure in the Attitude Control Subsystem (ACS) after 10 months of operation caused a loss in precision pointing capability. The Multimission Modular Spacecraft (MMS) used for the mission, was designed with on-orbit repairability, and to correct various instrument anomalies, repiar kits such as an electronics box, a thermal aperture closure, and a high energy particle reflection baffle will be used. In addition, a flight support system will be used to berth, electrically safe, and support all the repair activities. A two year effort is foreseen, and the economic return on SMM will be $176 M, in addition to two to three years of solar observation. The mission will eventually conduct studies on flare as a function of solar cycle.

A brief history of Regional Warning Center China (RWC-China)

NASA Astrophysics Data System (ADS)

He, Han; Wang, Huaning; Du, Zhanle; Huang, Xin; Yan, Yan; Dai, Xinghua; Guo, Juan; Wang, Jialong

2018-03-01

Solar-terrestrial prediction services in China began in 1969 at the Beijing Astronomical Observatory (BAO), Chinese Academy of Sciences (CAS). In 1990, BAO joined the International URSIgram and World Days Service (IUWDS) and started solar-terrestrial data and prediction interchanges with other members of IUWDS. The short-term solar activity prediction service with standard URSIgram codes began in January 1991 at BAO, and forecasts have been issued routinely every weekday from then on. The Regional Warning Center Beijing (RWC-Beijing) of IUWDS was officially approved in China in 1991 and was formally established in February 1992. In 1996, the IUWDS was changed to the current name, the International Space Environment Service (ISES). In 2000, the RWC-Beijing was renamed RWC-China according to ISES requirements. In 2001, the National Astronomical Observatories, CAS (NAOC) was established. All the solar-terrestrial data and prediction services of BAO were taken up by NAOC. The headquarters of RWC-China is located on the campus of NAOC.

Automated Feature and Event Detection with SDO AIA and HMI Data

NASA Astrophysics Data System (ADS)

Davey, Alisdair; Martens, P. C. H.; Attrill, G. D. R.; Engell, A.; Farid, S.; Grigis, P. C.; Kasper, J.; Korreck, K.; Saar, S. H.; Su, Y.; Testa, P.; Wills-Davey, M.; Savcheva, A.; Bernasconi, P. N.; Raouafi, N.-E.; Delouille, V. A.; Hochedez, J. F..; Cirtain, J. W.; Deforest, C. E.; Angryk, R. A.; de Moortel, I.; Wiegelmann, T.; Georgouli, M. K.; McAteer, R. T. J.; Hurlburt, N.; Timmons, R.

The Solar Dynamics Observatory (SDO) represents a new frontier in quantity and quality of solar data. At about 1.5 TB/day, the data will not be easily digestible by solar physicists using the same methods that have been employed for images from previous missions. In order for solar scientists to use the SDO data effectively they need meta-data that will allow them to identify and retrieve data sets that address their particular science questions. We are building a comprehensive computer vision pipeline for SDO, abstracting complete metadata on many of the features and events detectable on the Sun without human intervention. Our project unites more than a dozen individual, existing codes into a systematic tool that can be used by the entire solar community. The feature finding codes will run as part of the SDO Event Detection System (EDS) at the Joint Science Operations Center (JSOC; joint between Stanford and LMSAL). The metadata produced will be stored in the Heliophysics Event Knowledgebase (HEK), which will be accessible on-line for the rest of the world directly or via the Virtual Solar Observatory (VSO) . Solar scientists will be able to use the HEK to select event and feature data to download for science studies.

Virtual Energetic Particle Observatory for the Heliospheric Data Environment

NASA Technical Reports Server (NTRS)

Cooper, J. F.; Armstrong, T. P.; Hill, M. E.; Lal, N.; McGuire, R. E.; McKibben, R. B.; Narock, T. W.; Szabo, A.; Tranquille, C.

2007-01-01

The heliosphere is pervaded by interplanetary energetic particles, traditionally also called cosmic rays, from solar, internal heliospheric, and galactic sources. The particles species of interest to heliophysics extend from plasma energies to the GeV energies of galactic cosmic rays still measurably affected by heliospheric modulation and the still higher energies contributing to atmospheric ionization. The NASA and international Heliospheric Network of operational and legacy spacecraft measures interplanetary fluxes of these particles. Spatial coverage extends from the inner heliosphere and geospace to the heliosheath boundary region now being traversed by Voyager 1 and soon by Voyager 2. Science objectives include investigation of solar flare and coronal mass ejection events, acceleration and transport of interplanetary particles within the inner heliosphere, cosmic ray interactions with planetary surfaces and atmospheres, sources of suprathermal and anomalous cosmic ray ions in the outer heliosphere, and solar cycle modulation of galactic cosmic rays. The Virtual Energetic Particle Observatory (VEPO) will improve access and usability of selected spacecraft and sub-orbital NASA heliospheric energetic particle data sets as a newly approved effort within the evolving heliophysics virtual observatory environment. In this presentation, we will describe current VEPO science requirements, our initial priorities and an overview of our strategy to implement VEPO rapidly and at minimal cost by working within the high-level framework of the Virtual Heliospheric Observatory (VHO). VEPO will also leverage existing data services of NASA's Space Physics Data Facility and other existing capabilities of the U.S. and international heliospheric research communities.

An Observatory to Enhance the Preparation of Future California Teachers

NASA Astrophysics Data System (ADS)

Connolly, L.; Lederer, S.

2004-12-01

With a major grant from the W. M. Keck Foundation, California State University, San Bernardino is establishing a state-of-the-art teaching astronomical observatory. The Observatory will be fundamental to an innovative undergraduate physics and astronomy curriculum for Physics and Liberal Studies majors and will be integrated into our General Education program. The critical need for a research and educational observatory is linked to changes in California's Science Competencies for teacher certification. Development of the Observatory will also complement a new infusion of NASA funding and equipment support for our growing astronomy education programs and the University's established Strategic Plan for excellence in education and teacher preparation. The Observatory will consist of two domed towers. One tower will house a 20" Ritchey-Chretien telescope equipped with a CCD camera in conjunction with either UBVRI broadband filters or a spectrometer for evening laboratories and student research projects. The second tower will house the university's existing 12" Schmidt-Cassegrain optical telescope coupled with a CCD camera and an array of filters. A small aperture solar telescope will be attached to the 12" for observing solar prominences while a milar filter can be attached to the 12" for sunspot viewing. We have been very fortunate to receive a challenge grant of \\600,000 from the W. M. Keck Foundation to equip the two domed towers; we continue to seek a further \\800,000 to meet our construction needs. Funding also provided by the California State University, San Bernardino.

Metrology of the Solar Spectral Irradiance at the Top Of Atmosphere in the Near Infrared using Ground Based Instruments. Final results of the PYR-ILIOS campaign (Mauna Loa Observatory, June-July 2016).

NASA Astrophysics Data System (ADS)

Cessateur, G.; Bolsée, D.; Pereira, N.; Sperfeld, P.; Pape, S.

2017-12-01

The availability of reference spectra for the Solar Spectral Irradiance (SSI) is important for the solar physics, the studies of planetary atmospheres and climatology. The near infrared (NIR) part of these spectra is of great interest for its main role for example, in the Earth's radiative budget. Until recently, some large and unsolved discrepancies (up to 10 %) were observed in the 1.6 μm region between space instruments, models and ground-based measurements. We designed a ground-based instrumentation for SSI measurements at the Top Of Atmosphere (TOA) through atmospheric NIR windows using the Bouguer-Langley technique. The main instrument is a double NIR spectroradiometer designed by Bentham (UK), radiometrically characterized at the Royal Belgian Institute for Space Aeronomy. It was absolute calibrated against a high-temperature blackbody as primary standard for spectral irradiance at the Physikalisch-Technische Bundesanstalt (Germany). The PYR-ILIOS campaign was carried out in June to July 2016 at the Mauna Loa Observatory (Hawaii, USA, 3396 m a.s.l.) follows the four-month IRESPERAD campaign which was carried out in the summer 2011 at the Izaña Atmospheric Observatory (Canary Islands, 2367 m a.s.l.). We present here the results of the 3'week PYR-ILIOS campaign and compare them with the ATLAS 3 spectrum as well as from recently reprocessed NIR solar spectra obtained with SOLAR/SOLSPEC on ISS and SCIAMACHY on ENVISAT. The uncertainty budget of the PYR-ILIOS results will be discussed.

A New Observatory for Eastern College: A Dream Realized

NASA Astrophysics Data System (ADS)

Bradstreet, D. H.

1996-12-01

The Eastern College Observatory began as a rooftop observing deck with one Celestron 8 telescope in 1976 as the workhorse instrument of the observational astronomy lab within the core curriculum. For 20 years the observing deck served as the crude observatory, being augmented through the years by other computerized Celestron 8's and a 17.5" diameter Dobsonian with computerized setting circles. The lab consisted primarily of visual observations and astrophotography. In 1987 plans were set into motion to raise money to build a permanent Observatory on the roof of the main classroom building. Fundraising efforts included three Jog-A-Thons (raising more than $40,000) and many donations from individuals and foundations. The fundraising was completed in 1996 and a two telescope observatory was constructed in the summer of 1996 complete with warm room, CCD cameras, computers, spectrograph, video network, and computerized single channel photometer. The telescopes are computerized 16" diameter Meade LX200 Schmidt-Cassegrains, each coupled to Gateway Pentium Pro 200 MHz computers. SBIG ST-8 CCD cameras were also secured for each telescope and an Optec SSP-7 photometer and Optomechanics Research 10C Spectrograph were also purchased. A Daystar H-alpha solar filter and Thousand Oaks visual light solar filter have expanded the Observatory's functionality to daytime observing as well. This is especially useful for the thousands of school children who frequent the Planetarium each year. The Observatory primarily serves the core astronomy lab where students must observe and photograph a prescribed number of celestial objects in a semester. Advanced students can take directed studies where they conduct photometry on eclipsing binaries or other variable stars or search for new asteroids. In addition, the Observatory and Planetarium are open to the public. Interested members of the community can reserve time on the telescopes and receive training and supervision from lab assistants. The lessons learned from building the Observatory as well as structural plans, equipment and curriculum development will be discussed in this poster.

Line Asymmetries and Vertical Velocities Observed with a Narrow-Band Filter

DTIC Science & Technology

1990-06-20

dr,AMonrh, day) 1.PAGE COUNT Reprint FROM _ TO 1990 June 20 14 16 SUPPLEMENTARY NOTATION *Instituto di Astronomia , Firenze, Italy **National Solar... Astronomia , Firenze, Italy Peter Tamblyn and Larry November National Solar Observatory. Sacramento Peak, Sunspot, NM 88349, USA Abstract Fabry-Perot filter

Pulses from the Sun

NASA Image and Video Library

2014-02-11

The dark region seen on the face of the sun at the end of March 2013 is a coronal hole just above and to the right of the middle of the picture, which is a source of fast solar wind leaving the sun in this image from NASA Solar Dynamic Observatory.

An Eruptive Complex Solar Flare and Events in its Aftermath

NASA Astrophysics Data System (ADS)

Luoni, M. L.; Francile, C.; Mandrini, C. H.; Cremades, H.

2017-10-01

We present a study of the M6.6 flare that occurred on 13 February 2011 in AR 11158. The flare was accompanied by a CME and EUV waves. We use multiwavelength observations from the ground: H-alpha Solar Telescope for Argentina (HASTA), and space: Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA), both onboard the Solar and Dynamic Observatory (SDO).

Solar forecast and real-time monitoring needs of the Study of Energy Release in Flares (SERF)

NASA Technical Reports Server (NTRS)

Rust, D. M.

1979-01-01

Complementary, simultaneous observations of flares from as many observatories, both ground based and orbiting, as possible planned for the Solar Maximum Year are considered. The need for forecasts of solar activity on long term, one week, and two day intervals is described. Real time reporting is not needed, but daily summaries of activity and permanent records are important.

Solar Observations on Magneto-Convection

DTIC Science & Technology

1989-05-31

Technical Library National Solar Observatory Sunspot, NM 88349 Karl - Schwarzschild -Strasse 1 8046 Garching bei Mundhen Solar Observations On Magneto...Schmidt, Hermann-Ulrich Schmidt, Hans-Christoph Thomas (eds.) Max-Planck-Institut fir Physik und Astrophysik Institut fiur Astrophysik Karl ... Schwarzschild -St-. 1 D-8046 Garching, FklG 14TIS CRiA.&l DTIC TA. U~Jar,iou8:ed B ......... ... Distribution I -- Availability COcý----- Avail and or Dist special

Solar Environmental Disturbances

DTIC Science & Technology

2007-11-02

like stars were examined, extending the previous 7–12 year time series to 13–20 years by combining Strömgren b, y photometry from Lowell Observatory...per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and...explanations for how these physical processes affect the production of solar activity, both on short and long time scales. Solar cycle variation

Polarization Observations of the Total Solar Eclipse of August 21, 2017

NASA Astrophysics Data System (ADS)

Burkepile, J.; Boll, A.; Casini, R.; de Toma, G.; Elmore, D. F.; Gibson, K. L.; Judge, P. G.; Mitchell, A. M.; Penn, M.; Sewell, S. D.; Tomczyk, S.; Yanamandra-Fisher, P. A.

2017-12-01

A total solar eclipse offers ideal sky conditions for viewing the solar corona. Light from the corona is composed of three components: the E-corona, made up of spectral emission lines produced by ionized elements in the corona; the K-corona, produced by photospheric light that is Thomson scattered by coronal electrons; and the F-corona, produced by sunlight scattered from dust particles in the near Sun environment and in interplanetary space. Polarized white light observations of the corona provide a way of isolating the K-corona to determine its structure, brightness, and density. This work focuses on broadband white light polarization observations of the corona during the upcoming solar eclipse from three different instruments. We compare coronal polarization brightness observations of the August 21, 2017 total solar eclipse from the NCAR/High Altitude Observatory (HAO) Rosetta Stone experiment using the 4-D Technology PolarCam camera with the two Citizen PACA_CATE17Pol telescopes that will acquire linear polarization observations of the eclipse and the NCAR/HAO K-Cor white light coronagraph observations from the Mauna Loa Solar Observatory in Hawaii. This comparison includes a discussion of the cross-calibration of the different instruments and reports the results of the coronal polarization brightness and electron density of the corona. These observations will be compared with results from previous coronal measurements taken at different phases of the solar cycle. In addition, we report on the performance of the three different polarimeters. The 4-D PolarCam uses a linear polarizer array, PACA_CATE17Pol uses a nematic liquid crystal retarder in a single beam configuration and K-Cor uses a pair of ferroelectric liquid crystal retarders in a dual-beam configuration. The use of the 4-D PolarCam camera in the Rosetta Stone experiment is to demonstrate the technology for acquiring high cadence polarization measurements. The Rosetta Stone experiment is funded through the NASA award NNH16ZDA001N-ISE. The Citizen Science approach to measuring the polarized solar corona during the eclipse is funded through NASA award NNX17AH76G. The NCAR Mauna Loa Solar Observatory is funded by the National Science Foundation.

The proposed NRAO millimeter array and its use for solar studies

NASA Technical Reports Server (NTRS)

Kundu, Mukul R.

1986-01-01

A brief summary is given of the proposed National Radio Astronomy Observatory (NRAO) Millimeter Array discussed at a workshop held in Green Bank, W. Va., September 30 to October 2, 1985. A brief description of the solar studies that can be made with such an array is provided.

Earth Observatory Satellite system definition study. Report 5: System design and specifications. Volume 4: Mission peculiar spacecraft segment and module specifications

NASA Technical Reports Server (NTRS)

1974-01-01

The specifications for the Earth Observatory Satellite (EOS) peculiar spacecraft segment and associated subsystems and modules are presented. The specifications considered include the following: (1) wideband communications subsystem module, (2) mission peculiar software, (3) hydrazine propulsion subsystem module, (4) solar array assembly, and (5) the scanning spectral radiometer.

System design and specifications. Earth Observatory Satellite system definition study (EOS)

NASA Technical Reports Server (NTRS)

1974-01-01

A design summary of the Earth Observatory Satellite (EOS) is presented. The systems considered in the summary are: (1) the spacecraft structure, (2) electrical power modules, (3) communications and data handling module, (4) attitude determination module, (5) actuation module, and (6) solar array and drive module. The documents which provide the specifications for the systems and the equipment are identified.

Getting NuSTAR on target: predicting mast motion

NASA Astrophysics Data System (ADS)

Forster, Karl; Madsen, Kristin K.; Miyasaka, Hiromasa; Craig, William W.; Harrison, Fiona A.; Rana, Vikram R.; Markwardt, Craig B.; Grefenstette, Brian W.

2016-07-01

The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first focusing high energy (3-79 keV) X-ray observatory operating for four years from low Earth orbit. The X-ray detector arrays are located on the spacecraft bus with the optics modules mounted on a flexible mast of 10.14m length. The motion of the telescope optical axis on the detectors during each observation is measured by a laser metrology system and matches the pre-launch predictions of the thermal flexing of the mast as the spacecraft enters and exits the Earths shadow each orbit. However, an additional motion of the telescope field of view was discovered during observatory commissioning that is associated with the spacecraft attitude control system and an additional flexing of the mast correlated with the Solar aspect angle for the observation. We present the methodology developed to predict where any particular target coordinate will fall on the NuSTAR detectors based on the Solar aspect angle at the scheduled time of an observation. This may be applicable to future observatories that employ optics deployed on extendable masts. The automation of the prediction system has greatly improved observatory operations efficiency and the reliability of observation planning.

Getting NuSTAR on Target: Predicting Mast Motion

NASA Technical Reports Server (NTRS)

Forster, Karl; Madsen, Kristin K.; Miyasaka, Hiroshima; Craig, William W.; Harrison, Fiona A.; Rana, Vikram R.; Markwardt, Craig B.; Grenfenstette, Brian W.

2017-01-01

The Nuclear Spectroscopic Telescope Array (NuSTAR) is the first focusing high energy (3-79 keV) X-ray observatory operating for four years from low Earth orbit. The X-ray detector arrays are located on the spacecraft bus with the optics modules mounted on a flexible mast of 10.14m length. The motion of the telescope optical axis on the detectors during each observation is measured by a laser metrology system and matches the pre-launch predictions of the thermal flexing of the mast as the spacecraft enters and exits the Earths shadow each orbit. However, an additional motion of the telescope field of view was discovered during observatory commissioning that is associated with the spacecraft attitude control system and an additional flexing of the mast correlated with the Solar aspect angle for the observation. We present the methodology developed to predict where any particular target coordinate will fall on the NuSTAR detectors based on the Solar aspect angle at the scheduled time of an observation. This may be applicable to future observatories that employ optics deployed on extendable masts. The automation of the prediction system has greatly improved observatory operations efficiency and the reliability of observation planning.

Solar physics in the space age

NASA Technical Reports Server (NTRS)

1989-01-01

A concise and brief review is given of the solar physics' domain, and how its study has been affected by NASA Space programs which have enabled space based observations. The observations have greatly increased the knowledge of solar physics by proving some theories and challenging others. Many questions remain unanswered. To exploit coming opportunities like the Space Station, solar physics must continue its advances in instrument development, observational techniques, and basic theory. Even with the Advance Solar Observatory, other space based observation will still be required for the sure to be ensuing questions.

SDO Pick of the Week

NASA Image and Video Library

2017-12-08

Magnetic arcs of solar material spewing from our favorite sphere of hot plasma, the sun. Magnetic arcs of solar material held their shapes fairly well as they spiraled above two solar active regions over 18 hours on Jan. 11-12, 2017. The charged solar material, called plasma, traces out the magnetic field lines above the active regions when viewed in wavelengths of extreme ultraviolet light, captured here by NASA’s Solar Dynamics Observatory. Extreme ultraviolet light is typically invisible to our eyes, but is colorized here in gold for easy viewing. Credit: NASA/SDO

Reaching to the Star

NASA Astrophysics Data System (ADS)

Ruzhitskaya, Lanika; Speck, A.; Baldridge, S.; Briggs, J.

2014-01-01

The 2017 solar eclipse will pass over the Midwest and right over the University of Missouri in Columbia. This event presents us with a wonderful opportunity for science outreach and education programs. In preparation for this event, we use our Coronado solar telescope as a portable solar viewing observatory roving all over our campus. During these solar viewing events, students, faculty and staff have a chance to look through the telescope to discover for themselves-- and learn about-- the most prominent features of the Sun: limb darkening, sunspots, granulations, flares, prominences and filaments. Astronomy undergraduate and graduate students are on hand to answer questions and to hand out leaflets explaining the science behind these solar features. These solar observations represent excellent opportunities for those who want to know more about the Sun and its role in our lives: from solar activity to global warming; from the formation of the Sun, our planet and the entire Solar System down to the end of our Sun’s life. These events also benefit the volunteering students who learn how to explain complicated science concepts in a simple way to the general public. In addition, the portable solar observatory makes people aware about other science talks and events on our campus. These events are a great way to make people on campus aware about the upcoming solar eclipse. Over the course of the next four years we expect to have generated enough interest to be able to accomplish our goal of hosting solar eclipse festivities in August of 2017 in our football stadium in front of a massive crowd of interested observers and potential astronomy students.

Astronomy in Georgia - Present Status and Perspectives

NASA Astrophysics Data System (ADS)

Todua, M.

2016-09-01

Astronomy in Georgia is generally represented in Abastumani Astrophysical Observatory found in 1932. It is one of the leading scientific institutes in the country. Main fields of research are solar system bodies (including near-Earth asteroids), various aspects of solar physics, stellar astronomy (including binary stars and open clusters), extragalactic objects (AGNs), theoretical astrophysics, cosmology, atmospheric and solar-terrestrial physics. Several telescopes are operational today, as well as the instruments for atmospheric studies. In 2007 the Observatory was integrated with Ilia State University, merging scientific research and education which facilitated the growth of a new generation of researchers. There are groups of astronomers and astrophysicists in other Georgian universities and institutions as well. Georgian scientists collaborate with research centers and universities worldwide. Research groups participate in various international scientific projects. The interest in astronomy in Georgia has been growing, which increases future perspectives of its development in the country.

NASA's Solar Dynamics Observatory Unveils New Images

NASA Image and Video Library

2010-04-20

Alan Title, second from left, principal investigator, Atmospheric Imaging Assembly instrument, Lockheed Martin Solar and Astrophysics Laboratory in Palo Alto, speaks during a briefing to discuss recent images from NASA's Solar Dynamics Observatory, or SDO, Wednesday, April 21, 2010, at the Newseum in Washington. Launched on Feb. 11, 2010, SDO is the most advanced spacecraft ever designed to study the sun. During its five-year mission, it will examine the sun's magnetic field and also provide a better understanding of the role the sun plays in Earth's atmospheric chemistry and climate. Pictured from left to right: Dean Pesnell, SDO project scientist, Goddard Space Flight Center in Greenbelt, Md., Alan Title, Philip H. Scherrer, principal investigator, Helioseismic and Magnetic Imager instrument, Stanford University in Palo Alto, Tom Woods, principal investigator, Extreme Ultraviolet Variability Experiment instrument, Laboratory for Atmospheric and Space Physics, University of Colorado in Boulder and Madhulika Guhathakurta, SDO program scientist, NASA Headquarters in Washington. Photo Credit: (NASA/Carla Cioffi)

Ionospheric wave signature of the American solar eclipse on 21 August 2017 in Europe

NASA Astrophysics Data System (ADS)

Verhulst, Tobias G. W.; Stankov, Stanimir M.

2018-05-01

A total solar eclipse occurred on 21 August 2017, with the path of totality starting over the North Pacific Ocean, crossing North-America and ending over the Mid-Atlantic Ocean slightly North of the equator. As a result, a partial solar eclipse was observed as far away as the Western Europe. The ionospheric observatory in Dourbes, Belgium, was right on the edge of the partial eclipse and was exposed for a very short period of only few minutes just before the local sunset. High-resolution ionospheric measurements were carried out at the observatory with collocated digital ionosonde and GNSS receivers. The data analysis revealed a clear wave-like pattern in the ionosphere that can be seen arriving before the local onset of the eclipse. The paper details the analysis and provides a possible explanation of the observed phenomenon.

NASA's search for the solar connection. I. [OSO Skylab, Solar Maximum Mission

NASA Technical Reports Server (NTRS)

Chapman, R. W.

1979-01-01

NASA's solar research, which leans toward the study of the sun as a star, is surveyed. The Orbiting Solar Observatory (OSO) program is covered, which yielded data such as spectras of 140-400 A wavelength of the entire solar disk. Attention is also given to the results obtained by Skylab, such as data showing that whenever a large coronal hole exists near the sun's equator, a stream of high-speed solar wind will be observed at the earth. Finally areas of future research, such as a concerted study of flare phenomenon, are discussed.

Destruction of Sun-Grazing Comet C-2011 N3 (SOHO) Within the Low Solar Corona

NASA Technical Reports Server (NTRS)

Schrijver, C. J.; Brown, J. C.; Battams, K.; Saint-Hilaire, P.; Liu, W.; Hudson, H.; Pesnell, W. D.

2012-01-01

Observations of comets in Sun-grazing orbits that survive solar insolation long enough to penetrate into the Suns inner corona provide information on the solar atmosphere and magnetic field as well as on the makeup of the comet. On 6 July 2011, the Solar Dynamics Observatory (SDO) observed the demise of comet C2011 N3 (SOHO) within the low solar corona in five wavelength bands in the extreme ultraviolet (EUV). The comet penetrated to within 0.146 solarradius (100,000 kilometers) of the solar surface before its EUV signal disappeared.

20th National Solar Physics Meeting

NASA Astrophysics Data System (ADS)

Dorotovic, Ivan

2010-12-01

These proceedings (ISBN: 978-80-85221-68-8) provide an overview of current research on solar physics, geophysics and space weather in the astronomical, geophysical and space physics institutions in the Slovak Republic and the Czech Republic. Several researchers from other countries participated in the meeting as well. The different parts address: solar interior, solar photosphere, chromosphere, corona, total solar eclipses, space weather, instrumentation. Most of the papers are published in Slovak and Czech, respectively. The proceedings are intended for researchers, graduate and PhD. students, workers of astronomical observatories interested in solar physics, geophysics and space weather.

The Virtual Space Physics Observatory: Quick Access to Data and Tools

NASA Technical Reports Server (NTRS)

Cornwell, Carl; Roberts, D. Aaron; McGuire, Robert E.

2006-01-01

The Virtual Space Physics Observatory (VSPO; see http://vspo.gsfc.nasa.gov) has grown to provide a way to find and access about 375 data products and services from over 100 spacecraft/observatories in space and solar physics. The datasets are mainly chosen to be the most requested, and include most of the publicly available data products from operating NASA Heliophysics spacecraft as well as from solar observatories measuring across the frequency spectrum. Service links include a "quick orbits" page that uses SSCWeb Web Services to provide a rapid answer to questions such as "What spacecraft were in orbit in July 1992?" and "Where were Geotail, Cluster, and Polar on 2 June 2001?" These queries are linked back to the data search page. The VSPO interface provides many ways of looking for data based on terms used in a registry of resources using the SPASE Data Model that will be the standard for Heliophysics Virtual Observatories. VSPO itself is accessible via an API that allows other applications to use it as a Web Service; this has been implemented in one instance using the ViSBARD visualization program. The VSPO will become part of the Space Physics Data Facility, and will continue to expand its access to data. A challenge for all VOs will be to provide uniform access to data at the variable level, and we will be addressing this question in a number of ways.

Contributions of the "Great" X-Ray Observatories (XMM-Newton and Chandra) to Astronomy and Astrophysics

NASA Technical Reports Server (NTRS)

Weisskopf, Martin

2011-01-01

NASA s Chandra X-ray Observatory and ESA s XMM-Newton made their first observations over a decade ago. The unprecedented and complementary capabilities of these observatories to detect, image, and measure the energy of cosmic X-rays, achieved less than 50 years after the first detection of an extra-solar X-ray source, represent an increase in sensitivity comparable in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. In this presentation we highlight some of the many discoveries made using these powerful X-ray observatories that have transformed 21st century astronomy. We briefly discuss future prospects for this truly exciting field.

The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

NASA Astrophysics Data System (ADS)

Pierre Auger Collaboration; Abreu, P.; Aglietta, M.; Ahn, E. J.; Allard, D.; Allekotte, I.; Allen, J.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Ambrosio, M.; Aminaei, A.; Anchordoqui, L.; Andringa, S.; Antičić, T.; Anzalone, A.; Aramo, C.; Arganda, E.; Arisaka, K.; Arqueros, F.; Asorey, H.; Assis, P.; Aublin, J.; Ave, M.; Avenier, M.; Avila, G.; Bäcker, T.; Badagnani, D.; Balzer, M.; Barber, K. B.; Barbosa, A. F.; Bardenet, R.; Barroso, S. L. C.; Baughman, B.; Beatty, J. J.; Becker, B. R.; Becker, K. H.; Bellétoile, A.; Bellido, J. A.; BenZvi, S.; Berat, C.; Bergmann, T.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanco, F.; Blanco, M.; Bleve, C.; Blümer, H.; Boháčová, M.; Boncioli, D.; Bonifazi, C.; Bonino, R.; Borodai, N.; Brack, J.; Brogueira, P.; Brown, W. C.; Bruijn, R.; Buchholz, P.; Bueno, A.; Burton, R. E.; Busca, N. G.; Caballero-Mora, K. S.; Caramete, L.; Caruso, R.; Castellina, A.; Catalano, O.; Cataldi, G.; Cazon, L.; Cester, R.; Chauvin, J.; Chiavassa, A.; Chinellato, J. A.; Chou, A.; Chudoba, J.; Clay, R. W.; Colombo, E.; Coluccia, M. R.; Conceição, R.; Contreras, F.; Cook, H.; Cooper, M. J.; Coppens, J.; Cordier, A.; Cotti, U.; Coutu, S.; Covault, C. E.; Creusot, A.; Criss, A.; Cronin, J.; Curutiu, A.; Dagoret-Campagne, S.; Dallier, R.; Dasso, S.; Daumiller, K.; Dawson, B. R.; de Almeida, R. M.; De Domenico, M.; De Donato, C.; de Jong, S. J.; De La Vega, G.; de Mello Junior, W. J. M.; de Mello Neto, J. R. T.; De Mitri, I.; de Souza, V.; de Vries, K. D.; Decerprit, G.; del Peral, L.; Deligny, O.; Della Selva, A.; Dembinski, H.; Denkiewicz, A.; Di Giulio, C.; Diaz, J. C.; Díaz Castro, M. L.; Diep, P. N.; Dobrigkeit, C.; D'Olivo, J. C.; Dong, P. N.; Dorofeev, A.; dos Anjos, J. C.; Dova, M. T.; D'Urso, D.; Dutan, I.; Ebr, J.; Engel, R.; Erdmann, M.; Escobar, C. O.; Etchegoyen, A.; Facal San Luis, P.; Falcke, H.; Farrar, G.; Fauth, A. C.; Fazzini, N.; Ferguson, A. P.; Ferrero, A.; Fick, B.; Filevich, A.; Filipčič, A.; Fleck, I.; Fliescher, S.; Fracchiolla, C. E.; Fraenkel, E. D.; Fröhlich, U.; Fuchs, B.; Fulgione, W.; Gamarra, R. F.; Gambetta, S.; García, B.; García Gámez, D.; Garcia-Pinto, D.; Garrido, X.; Gascon, A.; Gelmini, G.; Gemmeke, H.; Gesterling, K.; Ghia, P. L.; Giaccari, U.; Giller, M.; Glass, H.; Gold, M. S.; Golup, G.; Gomez Albarracin, F.; Gómez Berisso, M.; Gonçalves, P.; Gonzalez, D.; Gonzalez, J. G.; Gookin, B.; Góra, D.; Gorgi, A.; Gouffon, P.; Gozzini, S. R.; Grashorn, E.; Grebe, S.; Grigat, M.; Grillo, A. F.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Hague, J. D.; Hansen, P.; Harari, D.; Harmsma, S.; Harton, J. L.; Haungs, A.; Hebbeker, T.; Heck, D.; Herve, A. E.; Hojvat, C.; Holmes, V. C.; Homola, P.; Hórandel, J. R.; Horneffer, A.; Hrabovský, M.; Huege, T.; Insolia, A.; Ionita, F.; Italiano, A.; Jiraskova, S.; Kadija, K.; Kaducak, M.; Kampert, K. H.; Karhan, P.; Karova, T.; Kasper, P.; Kégl, B.; Keilhauer, B.; Keivani, A.; Kelley, J. L.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapp, J.; Koang, D.-H.; Kotera, K.; Krohm, N.; Krömer, O.; Kruppke-Hansen, D.; Kuehn, F.; Kuempel, D.; Kulbartz, J. K.; Kunka, N.; La Rosa, G.; Lachaud, C.; Lautridou, P.; Leão, M. S. A. B.; Lebrun, D.; Lebrun, P.; Leigui de Oliveira, M. A.; Lemiere, A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; López, R.; Lopez Agüera, A.; Louedec, K.; Lozano Bahilo, J.; Lucero, A.; Ludwig, M.; Lyberis, H.; Maccarone, M. C.; Macolino, C.; Maldera, S.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Marin, V.; Maris, I. C.; Marquez Falcon, H. R.; Marsella, G.; Martello, D.; Martin, L.; Martínez Bravo, O.; Mathes, H. J.; Matthews, J.; Matthews, J. A. J.; Matthiae, G.; Maurizio, D.; Mazur, P. O.; Medina-Tanco, G.; Melissas, M.; Melo, D.; Menichetti, E.; Menshikov, A.; Meurer, C.; Mičanović, S.; Micheletti, M. I.; Miller, W.; Miramonti, L.; Mollerach, S.; Monasor, M.; Monnier Ragaigne, D.; Montanet, F.; Morales, B.; Morello, C.; Moreno, E.; Moreno, J. C.; Morris, C.; Mostafá, M.; Mueller, S.; Muller, M. A.; Müller, G.; Münchmeyer, M.; Mussa, R.; Navarra, G.; Navarro, J. L.; Navas, S.; Necesal, P.; Nellen, L.; Nhung, P. T.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Nožka, L.; Nyklicek, M.; Oehlschläger, J.; Olinto, A.; Oliva, P.; Olmos-Gilbaja, V. M.; Ortiz, M.; Pacheco, N.; Pakk Selmi-Dei, D.; Palatka, M.; Pallotta, J.; Palmieri, N.; Parente, G.; Parizot, E.; Parra, A.; Parrisius, J.; Parsons, R. D.; Pastor, S.; Paul, T.; Pavlidou c, V.; Payet, K.; Pech, M.; Pękala, J.; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petermann, E.; Petrera, S.; Petrinca, P.; Petrolini, A.; Petrov, Y.; Petrovic, J.; Pfendner, C.; Phan, N.; Piegaia, R.; Pierog, T.; Pieroni, P.; Pimenta, M.; Pirronello, V.; Platino, M.; Ponce, V. H.; Pontz, M.; Privitera, P.; Prouza, M.; Quel, E. J.; Rautenberg, J.; Ravel, O.; Ravignani, D.; Revenu, B.; Ridky, J.; Riggi, S.; Risse, M.; Ristori, P.; Rivera, H.; Rivière, C.; Rizi, V.; Robledo, C.; Rodriguez, G.; Rodriguez Martino, J.; Rodriguez Rojo, J.; Rodriguez-Cabo, I.; Rodríguez-Frías, M. D.; Ros, G.; Rosado, J.; Rossler, T.; Roth, M.; Rouillé-d'Orfeuil, B.; Roulet, E.; Rovero, A. C.; Salamida, F.; Salazar, H.; Salina, G.; Sánchez, F.; Santander, M.; Santo, C. E.; Santos, E.; Santos, E. M.; Sarazin, F.; Sarkar, S.; Sato, R.; Scharf, N.; Scherini, V.; Schieler, H.; Schiffer, P.; Schmidt, A.; Schmidt, F.; Schmidt, T.; Scholten, O.; Schoorlemmer, H.; Schovancova, J.; Schovánek, P.; Schroeder, F.; Schulte, S.; Schüssler, F.; Schuster, D.; Sciutto, S. J.; Scuderi, M.; Segreto, A.; Semikoz, D.; Settimo, M.; Shadkam, A.; Shellard, R. C.; Sidelnik, I.; Sigl, G.; Śmiałkowski, A.; Šmída, R.; Snow, G. R.; Sommers, P.; Sorokin, J.; Spinka, H.; Squartini, R.; Stapleton, J.; Stasielak, J.; Stephan, M.; Strazzeri, E.; Stutz, A.; Suarez, F.; Suomijärvi, T.; Supanitsky, A. D.; Šuša, T.; Sutherland, M. S.; Swain, J.; Szadkowski, Z.; Tamashiro, A.; Tapia, A.; Tarutina, T.; Taşcǎu, O.; Tcaciuc, R.; Tcherniakhovski, D.; Tegolo, D.; Thao, N. T.; Thomas, D.; Tiffenberg, J.; Timmermans, C.; Tiwari, D. K.; Tkaczyk, W.; Todero Peixoto, C. J.; Tomé, B.; Tonachini, A.; Travnicek, P.; Tridapalli, D. B.; Tristram, G.; Trovato, E.; Tueros, M.; Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño, I.; Valore, L.; van den Berg, A. M.; Vargas Cárdenas, B.; Vázquez, J. R.; Vázquez, R. A.; Veberič, D.; Venters, T.; Verzi, V.; Videla, M.; Villaseñor, L.; Wahlberg, H.; Wahrlich, P.; Wainberg, O.; Warner, D.; Watson, A. A.; Weber, M.; Weidenhaupt, K.; Weindl, A.; Westerhoff, S.; Whelan, B. J.; Wieczorek, G.; Wiencke, L.; Wilczyńska, B.; Wilczyński, H.; Will, M.; Williams, C.; Winchen, T.; Winders, L.; Winnick, M. G.; Wommer, M.; Wundheiler, B.; Yamamoto a, T.; Younk, P.; Yuan, G.; Yushkov, A.; Zamorano, B.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.; Zaw, I.; Zepeda, A.; Ziolkowski, M.

2011-01-01

Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation with neutron monitor data is found.

KSC-99pp0351

NASA Image and Video Library

1999-03-26

In the Vertical Processing Facility, TRW technicians look at the point of attachment on the Chandra X-ray Observatory, at left, for the solar panel array (behind them). They are getting ready to attach and deploy the solar panel. Formerly called the Advanced X-ray Astrophysics Facility, Chandra comprises three major elements: the spacecraft, the science instrument module (SIM), and the world's most powerful X-ray telescope. Chandra will allow scientists from around the world to see previously invisible black holes and high-temperature gas clouds, giving the observatory the potential to rewrite the books on the structure and evolution of our universe. Chandra is scheduled for launch July 9 aboard Space Shuttle Columbia, on mission STS-93

The Open Flux Problem

NASA Astrophysics Data System (ADS)

Linker, J. A.; Caplan, R. M.; Downs, C.; Riley, P.; Mikic, Z.; Lionello, R.; Henney, C. J.; Arge, C. N.; Liu, Y.; Derosa, M. L.; Yeates, A.; Owens, M. J.

2017-10-01

The heliospheric magnetic field is of pivotal importance in solar and space physics. The field is rooted in the Sun’s photosphere, where it has been observed for many years. Global maps of the solar magnetic field based on full-disk magnetograms are commonly used as boundary conditions for coronal and solar wind models. Two primary observational constraints on the models are (1) the open field regions in the model should approximately correspond to coronal holes (CHs) observed in emission and (2) the magnitude of the open magnetic flux in the model should match that inferred from in situ spacecraft measurements. In this study, we calculate both magnetohydrodynamic and potential field source surface solutions using 14 different magnetic maps produced from five different types of observatory magnetograms, for the time period surrounding 2010 July. We have found that for all of the model/map combinations, models that have CH areas close to observations underestimate the interplanetary magnetic flux, or, conversely, for models to match the interplanetary flux, the modeled open field regions are larger than CHs observed in EUV emission. In an alternative approach, we estimate the open magnetic flux entirely from solar observations by combining automatically detected CHs for Carrington rotation 2098 with observatory synoptic magnetic maps. This approach also underestimates the interplanetary magnetic flux. Our results imply that either typical observatory maps underestimate the Sun’s magnetic flux, or a significant portion of the open magnetic flux is not rooted in regions that are obviously dark in EUV and X-ray emission.

The Open Flux Problem

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

Linker, J. A.; Caplan, R. M.; Downs, C.

The heliospheric magnetic field is of pivotal importance in solar and space physics. The field is rooted in the Sun’s photosphere, where it has been observed for many years. Global maps of the solar magnetic field based on full-disk magnetograms are commonly used as boundary conditions for coronal and solar wind models. Two primary observational constraints on the models are (1) the open field regions in the model should approximately correspond to coronal holes (CHs) observed in emission and (2) the magnitude of the open magnetic flux in the model should match that inferred from in situ spacecraft measurements. Inmore » this study, we calculate both magnetohydrodynamic and potential field source surface solutions using 14 different magnetic maps produced from five different types of observatory magnetograms, for the time period surrounding 2010 July. We have found that for all of the model/map combinations, models that have CH areas close to observations underestimate the interplanetary magnetic flux, or, conversely, for models to match the interplanetary flux, the modeled open field regions are larger than CHs observed in EUV emission. In an alternative approach, we estimate the open magnetic flux entirely from solar observations by combining automatically detected CHs for Carrington rotation 2098 with observatory synoptic magnetic maps. This approach also underestimates the interplanetary magnetic flux. Our results imply that either typical observatory maps underestimate the Sun’s magnetic flux, or a significant portion of the open magnetic flux is not rooted in regions that are obviously dark in EUV and X-ray emission.« less

Observational Evidence for the Associated Formation of Blobs and Raining Inflows in the Solar Corona

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

Sanchez-Diaz, E.; Rouillard, A. P.; Lavraud, B.

The origin of the slow solar wind is still a topic of much debate. The continual emergence of small transient structures from helmet streamers is thought to constitute one of the main sources of the slow wind. Determining the height at which these transients are released is an important factor in determining the conditions under which the slow solar wind forms. To this end, we have carried out a multipoint analysis of small transient structures released from a north–south tilted helmet streamer into the slow solar wind over a broad range of position angles during Carrington Rotation 2137. Combining themore » remote-sensing observations taken by the Solar-TErrestrial RElations Observatory ( STEREO ) mission with coronagraphic observations from the SOlar and Heliospheric Observatory ( SOHO ) spacecraft, we show that the release of such small transient structures (often called blobs), which subsequently move away from the Sun, is associated with the concomitant formation of transient structures collapsing back toward the Sun; the latter have been referred to by previous authors as “raining inflows.” This is the first direct association between outflowing blobs and raining inflows, which locates the formation of blobs above the helmet streamers and gives strong support that the blobs are released by magnetic reconnection.« less

Viewing The Entire Sun With STEREO And SDO

NASA Astrophysics Data System (ADS)

Thompson, William T.; Gurman, J. B.; Kucera, T. A.; Howard, R. A.; Vourlidas, A.; Wuelser, J.; Pesnell, D.

2011-05-01

On 6 February 2011, the two Solar Terrestrial Relations Observatory (STEREO) spacecraft were at 180 degrees separation. This allowed the first-ever simultaneous view of the entire Sun. Combining the STEREO data with corresponding images from the Solar Dynamics Observatory (SDO) allows this full-Sun view to continue for the next eight years. We show how the data from the three viewpoints are combined into a single heliographic map. Processing of the STEREO beacon telemetry allows these full-Sun views to be created in near-real-time, allowing tracking of solar activity even on the far side of the Sun. This is a valuable space-weather tool, not only for anticipating activity before it rotates onto the Earth-view, but also for deep space missions in other parts of the solar system. Scientific use of the data includes the ability to continuously track the entire lifecycle of active regions, filaments, coronal holes, and other solar features. There is also a significant public outreach component to this activity. The STEREO Science Center produces products from the three viewpoints used in iPhone/iPad and Android applications, as well as time sequences for spherical projection systems used in museums, such as Science-on-a-Sphere and Magic Planet.

Objectives for the Space Infrared Telescope Facility

NASA Technical Reports Server (NTRS)

Spehalski, Richard J.; Werner, Michael W.

1991-01-01

The Space Infrared Telescope Facility (SIRFT) is a one-meter-class, liquid-helium-cooled, earth-orbiting astronomical observatory that will be the infrared component of NASA's family of Great Observatories. SIRTF will investigate numerous scientific areas including formation and evolution of galaxies, stars, and other solar systems; supernovae; phenomena in our own solar system; and, undoubtedly, topics that are outside today's scientific domain. SIRTF's three instruments will permit imaging at all infrared wavelengths from 1.8 to 1200 microns and spectroscopy from 2.5 to 200 microns. The observatory will operate at an altitude of 100,000 km where it will achieve a five-year lifetime and operate with better than 80 percent on-target efficiency. The scientific importance and technical and programmatic readiness of SIRTF has been recognized by the 1991 report of the National Research Council's Astronomy and Astrophysics Survey Committee which recently identified SIRTF as the highest priority major new initiative in all of astronomy for the coming decade.

Deep space target location with Hubble Space Telescope (HST) and Hipparcos data

NASA Technical Reports Server (NTRS)

Null, George W.

1988-01-01

Interplanetary spacecraft navigation requires accurate a priori knowledge of target positions. A concept is presented for attaining improved target ephemeris accuracy using two future Earth-orbiting optical observatories, the European Space Agency (ESA) Hipparcos observatory and the Nasa Hubble Space Telescope (HST). Assuming nominal observatory performance, the Hipparcos data reduction will provide an accurate global star catalog, and HST will provide a capability for accurate angular measurements of stars and solar system bodies. The target location concept employs HST to observe solar system bodies relative to Hipparcos catalog stars and to determine the orientation (frame tie) of these stars to compact extragalactic radio sources. The target location process is described, the major error sources discussed, the potential target ephemeris error predicted, and mission applications identified. Preliminary results indicate that ephemeris accuracy comparable to the errors in individual Hipparcos catalog stars may be possible with a more extensive HST observing program. Possible future ground and spacebased replacements for Hipparcos and HST astrometric capabilities are also discussed.

KSC-06pd2370

NASA Image and Video Library

2006-10-19

KENNEDY SPACE CENTER, FLA. - Inside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, workers prepare the twin observatories known as STEREO for encapsulation in the fairing. The fairing is a molded structure that fits flush with the outside surface of the Delta II upper stage booster and forms an aerodynamically smooth nose cone, protecting the spacecraft during launch and ascent. The STEREO (Solar Terrestrial Relations Observatory) mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. Designed and built by the Applied Physics Laboratory (APL) , the STEREO mission is being managed by NASA Goddard Space Flight Center. APL will maintain command and control of the observatories throughout the mission, while NASA tracks and receives the data, determines the orbit of the satellites, and coordinates the science results. STEREO is expected to lift off Oct. 25. Photo credit: NASA/George Shelton

KSC-06pd2372

NASA Image and Video Library

2006-10-19

KENNEDY SPACE CENTER, FLA. - Inside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, workers prepare the twin observatories known as STEREO for encapsulation in the fairing. The fairing is a molded structure that fits flush with the outside surface of the Delta II upper stage booster and forms an aerodynamically smooth nose cone, protecting the spacecraft during launch and ascent. The STEREO (Solar Terrestrial Relations Observatory) mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. Designed and built by the Applied Physics Laboratory (APL) , the STEREO mission is being managed by NASA Goddard Space Flight Center. APL will maintain command and control of the observatories throughout the mission, while NASA tracks and receives the data, determines the orbit of the satellites, and coordinates the science results. STEREO is expected to lift off Oct. 25. Photo credit: NASA/George Shelton

KSC-06pd2371

NASA Image and Video Library

2006-10-19

KENNEDY SPACE CENTER, FLA. - Inside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, workers prepare the twin observatories known as STEREO for encapsulation in the fairing. The fairing is a molded structure that fits flush with the outside surface of the Delta II upper stage booster and forms an aerodynamically smooth nose cone, protecting the spacecraft during launch and ascent. The STEREO (Solar Terrestrial Relations Observatory) mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. Designed and built by the Applied Physics Laboratory (APL) , the STEREO mission is being managed by NASA Goddard Space Flight Center. APL will maintain command and control of the observatories throughout the mission, while NASA tracks and receives the data, determines the orbit of the satellites, and coordinates the science results. STEREO is expected to lift off Oct. 25. Photo credit: NASA/George Shelton

Fault Detection and Correction for the Solar Dynamics Observatory Attitude Control System

NASA Technical Reports Server (NTRS)

Starin, Scott R.; Vess, Melissa F.; Kenney, Thomas M.; Maldonado, Manuel D.; Morgenstern, Wendy M.

2007-01-01

The Solar Dynamics Observatory is an Explorer-class mission that will launch in early 2009. The spacecraft will operate in a geosynchronous orbit, sending data 24 hours a day to a devoted ground station in White Sands, New Mexico. It will carry a suite of instruments designed to observe the Sun in multiple wavelengths at unprecedented resolution. The Atmospheric Imaging Assembly includes four telescopes with focal plane CCDs that can image the full solar disk in four different visible wavelengths. The Extreme-ultraviolet Variability Experiment will collect time-correlated data on the activity of the Sun's corona. The Helioseismic and Magnetic Imager will enable study of pressure waves moving through the body of the Sun. The attitude control system on Solar Dynamics Observatory is responsible for four main phases of activity. The physical safety of the spacecraft after separation must be guaranteed. Fine attitude determination and control must be sufficient for instrument calibration maneuvers. The mission science mode requires 2-arcsecond control according to error signals provided by guide telescopes on the Atmospheric Imaging Assembly, one of the three instruments to be carried. Lastly, accurate execution of linear and angular momentum changes to the spacecraft must be provided for momentum management and orbit maintenance. In thsp aper, single-fault tolerant fault detection and correction of the Solar Dynamics Observatory attitude control system is described. The attitude control hardware suite for the mission is catalogued, with special attention to redundancy at the hardware level. Four reaction wheels are used where any three are satisfactory. Four pairs of redundant thrusters are employed for orbit change maneuvers and momentum management. Three two-axis gyroscopes provide full redundancy for rate sensing. A digital Sun sensor and two autonomous star trackers provide two-out-of-three redundancy for fine attitude determination. The use of software to maximize chances of recovery from any hardware or software fault is detailed. A generic fault detection and correction software structure is used, allowing additions, deletions, and adjustments to fault detection and correction rules. This software structure is fed by in-line fault tests that are also able to take appropriate actions to avoid corruption of the data stream.

Magico-religious and social belief of tribals of district Udaipur, Rajasthan.

PubMed

Kushwah, Vandana Singh; Sisodia, Rashmi; Bhatnagar, Chhaya

2017-12-01

Religious beliefs and practices have long influenced human perceptions and uses of nature. Animals in particular play a prominent role in magico-religious practices and provide historical and cultural depth of these relationships. Understanding human-faunal relations is often fundamental to the cause of meaningful wildlife conservation. This study investigates the domestic and wild harvested species used for spiritual and religious purposes among the tribals of six tehsils of Udaipur district. The ethnozoological data were obtained by an emic approach, applying different tools such as semi-structured interviews, participatory rural appraisal, key informant interviews, and focus group discussions. The scientific name and species of animals were identified using relevant and standard literature. Present investigation is a part of major concept worked out for study on tribal people and their beliefs. Ethnozoological information was collected by interview of 150 tribals. The questionnaire was prepared in Hindi keeping all parameters in mind. A total of 55 respondents (35 males and 20 females) answered to the magico-religious parameter. The collected data were analyzed through informant fidelity level (FL). The present study was undertaken to have an insight of the ethnozoological uses of animals prevalent in Bhil, Meena, and Kathodi tribes inhabiting the Udaipur district of Rajasthan. A total of 25 animals used for magico-religious and social purposes were recorded from the study area. Out of the total number of animals, 60% (15) were mammals, 24% (6) were birds, 12% (3) were reptiles, and the rest 4% (1) were the mollusks. Of the total ethnozoological practices, 64% fall in the magico-religious category, 12% in socio-cultural category, 12% in the category of ethnomusical, and 12% in the category of taboos. The tribal people maintain strong ties with animals at both the material and spiritual level. Study reveals that traditional people depend on local therapies either magico-religious or natural ones in absence of awareness, modern medical facilities, expensive drugs, and poor transportation. However, the use of animal material in such practices is on a decline.

Optical observational programs at the Indian Institute of Astrophysics

NASA Astrophysics Data System (ADS)

Singh, Jagdev; Ravindra, B.

The Indian Institute of Astrophysics has been making optical observations of the sun for more than a century by taking images of the sun in continuum to study the photosphere, Ca-K line and H-alpha line in order to study the chromosphere by using the same instruments which are used to study the long term variations of the magnetic fields on the sun. The digitizers have been developed using uniform light sources, imaging optics without any vignetting in the required FOV and large format 4K×4K CCD cameras to digitize the data for scientific studies. At the Solar Tower Telescope we have performed very high resolution spectroscopic observations around Ca-K line to investigate the variations and delineate the contribution of various features to the solar cycle variations. Solar coronal studies have been done during the occurrence of total solar eclipses and with a coronagraph to study the coronal heating. Here we discuss the systematic temporal variations observed in the green and red emission profiles using high spectral and temporal observations during the 2006, 2009 and 2010 total solar eclipses. The TWIN telescope a new facility has been fabricated and installed at Kodaikanal observatory to continue the synoptic observations of the sun and a space-based coronagraph is also being designed and fabricated in collaboration with various laboratories of ISRO (LEOS, ISAC and SAC) and USO. In this article we present the summary of results of optical observational programs carried out at Kodaikanal Observatory and during the eclipse expeditions where authors have played a leading role. Furthermore, this review is not complete in all respects of all the observational programs carried out at the Kodaikanal observatory.

Chromospheric Variability: Analysis of 36 years of Time Series from the National Solar Observatory/Sacramento Peak Ca II K-line Monitoring Program

NASA Technical Reports Server (NTRS)

Scargle, Jeffrey D.; Keil, Stephen L.; Worden, Simon P.

2014-01-01

Analysis of more than 36 years of time series of seven parameters measured in the NSO/AFRL/Sac Peak K-line monitoring program elucidates five elucidates five components of the variation: (1) the solar cycle (period approx. 11 years), (2) quasi-periodic variations (periods approx 100 days), (3) a broad band stochastic process (wide range of periods), (4) rotational modulation, and (5) random observational errors. Correlation and power spectrum analyses elucidate periodic and aperiodic variation of the chromospheric parameters. Time-frequency analysis illuminates periodic and quasi periodic signals, details of frequency modulation due to differential rotation, and in particular elucidates the rather complex harmonic structure (1) and (2) at time scales in the range approx 0.1 - 10 years. These results using only full-disk data further suggest that similar analyses will be useful at detecting and characterizing differential rotation in stars from stellar light-curves such as those being produced by NASA's Kepler observatory. Component (3) consists of variations over a range of timescales, in the manner of a 1/f random noise process. A timedependent Wilson-Bappu effect appears to be present in the solar cycle variations (1), but not in the stochastic process (3). Component (4) characterizes differential rotation of the active regions, and (5) is of course not characteristic of solar variability, but the fact that the observational errors are quite small greatly facilitates the analysis of the other components. The recent data suggest that the current cycle is starting late and may be relatively weak. The data analyzed in this paper can be found at the National Solar Observatory web site http://nsosp.nso.edu/cak_mon/, or by file transfer protocol at ftp://ftp.nso.edu/idl/cak.parameters.

Reconnection Fluxes in Eruptive and Confined Flares and Implications for Superflares on the Sun

NASA Astrophysics Data System (ADS)

Tschernitz, Johannes; Veronig, Astrid M.; Thalmann, Julia K.; Hinterreiter, Jürgen; Pötzi, Werner

2018-01-01

We study the energy release process of a set of 51 flares (32 confined, 19 eruptive) ranging from GOES class B3 to X17. We use Hα filtergrams from Kanzelhöhe Observatory together with Solar Dynamics Observatory HMI and Solar and Heliospheric Observatory MDI magnetograms to derive magnetic reconnection fluxes and rates. The flare reconnection flux is strongly correlated with the peak of the GOES 1–8 Å soft X-ray flux (c = 0.92, in log–log space) for both confined and eruptive flares. Confined flares of a certain GOES class exhibit smaller ribbon areas but larger magnetic flux densities in the flare ribbons (by a factor of 2). In the largest events, up to ≈50% of the magnetic flux of the active region (AR) causing the flare is involved in the flare magnetic reconnection. These findings allow us to extrapolate toward the largest solar flares possible. A complex solar AR hosting a magnetic flux of 2 × 1023 Mx, which is in line with the largest AR fluxes directly measured, is capable of producing an X80 flare, which corresponds to a bolometric energy of about 7 × 1032 erg. Using a magnetic flux estimate of 6 × 1023 Mx for the largest solar AR observed, we find that flares of GOES class ≈X500 could be produced (E bol ≈ 3 × 1033 erg). These estimates suggest that the present day’s Sun is capable of producing flares and related space weather events that may be more than an order of magnitude stronger than have been observed to date.

Multi-point Shock and Flux Rope Analysis of Multiple Interplanetary Coronal Mass Ejections around 2010 August 1 in the Inner Heliosphere

NASA Astrophysics Data System (ADS)

Möstl, C.; Farrugia, C. J.; Kilpua, E. K. J.; Jian, L. K.; Liu, Y.; Eastwood, J. P.; Harrison, R. A.; Webb, D. F.; Temmer, M.; Odstrcil, D.; Davies, J. A.; Rollett, T.; Luhmann, J. G.; Nitta, N.; Mulligan, T.; Jensen, E. A.; Forsyth, R.; Lavraud, B.; de Koning, C. A.; Veronig, A. M.; Galvin, A. B.; Zhang, T. L.; Anderson, B. J.

2012-10-01

We present multi-point in situ observations of a complex sequence of coronal mass ejections (CMEs) which may serve as a benchmark event for numerical and empirical space weather prediction models. On 2010 August 1, instruments on various space missions, Solar Dynamics Observatory/Solar and Heliospheric Observatory/Solar-TErrestrial-RElations-Observatory (SDO/SOHO/STEREO), monitored several CMEs originating within tens of degrees from the solar disk center. We compare their imprints on four widely separated locations, spanning 120° in heliospheric longitude, with radial distances from the Sun ranging from MESSENGER (0.38 AU) to Venus Express (VEX, at 0.72 AU) to Wind, ACE, and ARTEMIS near Earth and STEREO-B close to 1 AU. Calculating shock and flux rope parameters at each location points to a non-spherical shape of the shock, and shows the global configuration of the interplanetary coronal mass ejections (ICMEs), which have interacted, but do not seem to have merged. VEX and STEREO-B observed similar magnetic flux ropes (MFRs), in contrast to structures at Wind. The geomagnetic storm was intense, reaching two minima in the Dst index (≈ - 100 nT), and was caused by the sheath region behind the shock and one of two observed MFRs. MESSENGER received a glancing blow of the ICMEs, and the events missed STEREO-A entirely. The observations demonstrate how sympathetic solar eruptions may immerse at least 1/3 of the heliosphere in the ecliptic with their distinct plasma and magnetic field signatures. We also emphasize the difficulties in linking the local views derived from single-spacecraft observations to a consistent global picture, pointing to possible alterations from the classical picture of ICMEs.

Prediction of transits of Solar system objects in Kepler/K2 images: an extension of the Virtual Observatory service SkyBoT

NASA Astrophysics Data System (ADS)

Berthier, J.; Carry, B.; Vachier, F.; Eggl, S.; Santerne, A.

2016-05-01

All the fields of the extended space mission Kepler/K2 are located within the ecliptic. Many Solar system objects thus cross the K2 stellar masks on a regular basis. We aim at providing to the entire community a simple tool to search and identify Solar system objects serendipitously observed by Kepler. The sky body tracker (SkyBoT) service hosted at Institut de mécanique céleste et de calcul des éphémérides provides a Virtual Observatory compliant cone search that lists all Solar system objects present within a field of view at a given epoch. To generate such a list in a timely manner, ephemerides are pre-computed, updated weekly, and stored in a relational data base to ensure a fast access. The SkyBoT web service can now be used with Kepler. Solar system objects within a small (few arcminutes) field of view are identified and listed in less than 10 s. Generating object data for the entire K2 field of view (14°) takes about a minute. This extension of the SkyBoT service opens new possibilities with respect to mining K2 data for Solar system science, as well as removing Solar system objects from stellar photometric time series.

The Solar Dynamics Observatory: Your On-Orbit Eye on the Sun

NASA Technical Reports Server (NTRS)

Pesnell, W. Dean

2011-01-01

The Solar Dynamics Observatory (SDO) was launched on February 11, 2010 into the partly cloudy skies above Cape Canaveral, Florida. Over the next month SDO moved into a 28 degree inclined geosynchronous orbit at the longitude of the ground station in New Mexico. SDO is the first Space Weather Mission in NASA's Living With a Star Program. SDO's main goal is to understand and predict those solar variations that influence life on Earth and our technological systems. The SDO science investigations will determine how the Sun's magnetic field is generated and structured, how this stored magnetic energy is released into the heliosphere as the solar wind, energetic particles, and variations in the solar irradiance. The SDO mission consists of three scientific investigations (AIA, EVE, and HMI), a spacecraft bus, and a dedicated Ka-band ground station to handle the 150 Mbps data flow. SDO continues a long tradition of NASA missions providing calibrated solar spectral irradiance data, in this case using multiple measurements of the irradiance and rocket underflights of the spacecraft. The other instruments on SDO will be used to explain and develop predictive models of the solar spectral irradiance in the extreme ultraviolet. Science teams at LMSAL, LASP, and Stanford are responsible for processing, analyzing, distributing, and archiving the science data. We will talk about the launch of SDO and describe the data and science it is providing to NASA.

Eruptions from the Sun

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2015-11-01

The Sun often exhibits outbursts, launching material from its surface in powerful releases of energy. Recent analysis of such an outburst captured on video by several Sun-monitoring spacecraft may help us understand the mechanisms that launch these eruptions.Many OutburstsSolar jets are elongated, transient structures that are thought to regularly release magnetic energy from the Sun, contributing to coronal heating and solar wind acceleration. Coronal mass ejections (CMEs), on the other hand, are enormous blob-like explosions, violently ejecting energy and mass from the Sun at incredible speeds.But could these two types of events actually be related? According to a team of scientists at the University of Science and Technology of China, they may well be. The team, led by Jiajia Liu, has analyzed observations of a coronal jet that they believe prompted the launch of a powerful CME.Observing an ExplosionGif of a movie of the CME, taken by the Solar Dynamics Observatorys Atmospheric Imaging Assembly at a wavelength of 304. The original movie can be found in the article. [Liu et al.]An army of spacecraft was on hand to witness the event on 15 Jan 2013 including the Solar Dynamics Observatory (SDO), the Solar and Heliospheric Observatory (SOHO), and the Solar Terrestrial Relations Observatory (STEREO). The instruments on board these observatories captured the drama on the northern limb of the Sun as, at 19:32 UT, a coronal jet formed. Just eight minutes later, a powerful CME was released from the same active region.The fact that the jet and CME occurred in the same place at roughly the same time suggests theyre related. But did the initial motions of the CME blob trigger the jet? Or did the jet trigger the CME?Tying It All TogetherIn a recently published study, Liu and collaborators analyzed the multi-wavelength observations of this event to find the heights and positions of the jet and CME. From this analysis, they determined that the coronal jet triggered the release of material to form the CME, which then erupted into space with the jet at its core at speeds of over 1000 km/s.Based on observed clues of the magnetic field configurations, the team has put together a theory for how this event unfolded. They believe that sudden magnetic reconnection in an active region accelerated plasma to form a large-scale coronal jet. This burst of energy also provided a push on a blob of gas, threaded with magnetic field lines, that lay above the jet. The blob then rose, and when the field lines broke, it was released as a CME with the jet at its core.CitationJiajia Liu et al 2015 ApJ 813 115. doi:10.1088/0004-637X/813/2/115

Elves, Forbush Decreases and Solar Activity Studies at the Pierre Auger Observatory

NASA Astrophysics Data System (ADS)

Colalillo, Roberta

The Pierre Auger Observatory, designed to observe cosmic rays at the highest energies, can also be a valid ground based instrument for the observation of transient luminous events and for studying the modulation of galactic cosmic rays due to solar activity. The Fluorescence Detector can observe elves, transient luminous emissions from altitudes between 80 and 95 km above sea level, with timescales of tens of microseconds, which are triggered by lightning activity. A dedicated trigger and an extended readout scheme were introduced to enhance detection efficiency of these events and to improve the knowledge of some peculiar characteristics. The low energy mode of the Surface Detector, on the other hand, records variations in the flux of low energy secondary particles with extreme detail. With the Scaler mode, it is possible to register the rate of signals for deposited energies between 15-100 MeV; the Histogram mode, using the calibration peak and charge histograms of the individual pulses detected by each water-Cherenkov station, covers different deposited energy ranges up to 1 GeV. The variations in the flux of galactic cosmic rays have been studied on short and intermediate time scales (Forbush decreases), but also a long-term analysis, which shows the sensitivity of the Observatory to the solar cycle variation, is in progress.

On-line Eclipse Resources from the U.S. Naval Observatory: Planning Ahead for April 2024

NASA Astrophysics Data System (ADS)

Fredericks, Amy C.; Bartlett, J. L.; Bell, S.; Stapleton, J. C.

2014-01-01

On 8 April 2024, “…night from mid-day…” (Archilochus, 648 BCE) will appear to fortunate observers along a narrow band, approximately 115 mi (185 km) wide, that crosses fifteen states from Texas to Maine. In response to growing interest in the two total solar eclipses that will sweep the continental United States in the next 11 years, the U.S. Naval Observatory has developed an on-line resource center with direct links to 2024-specific services: the 2024 April 8 Total Solar Eclipse page (http://aa.usno.navy.mil/data/docs/Eclipse2024.php). The Solar Eclipse Computer (http://aa.usno.navy.mil/data/docs/SolarEclipses.php) calculates tables of local circumstances for events visible throughout the world. A similar service is available for lunar eclipses, Lunar Eclipse Computer (http://aa.usno.navy.mil/data/docs/LunarEclipse.php). The USNO Eclipse Portal (http://astro.ukho.gov.uk/eclbin/query_usno.cgi) provides diagrams and animations showing the global circumstances for events visible throughout the world and local circumstances for events visible at selected locations. The Web site, which includes both solar and lunar eclipses, is a joint effort with Her Majesty’s Nautical Almanac Office. The Eclipses of the Sun and Moon page (http://aa.usno.navy.mil/data/docs/UpcomingEclipses.php) links to electronic copies of the visibility maps from The Astronomical Almanac. The Eclipse Reference List (http://aa.usno.navy.mil/faq/docs/eclipse_ref.php) is a representative survey of the available literature for those interested in delving into these phenomena, either technically or historically. As exciting as the 2024 total solar eclipse, another spectacular event will precede it; a total solar eclipse will cross a different swath of the continent on August 21, 2017. The U.S. Naval Observatory has a resource center for that event as well (http://aa.usno.navy.mil/data/docs/Eclipse2017.php) . If your plans for 2024 are not yet made, visit the 2024 April 8 Total Solar Eclipse page to prepare for up to 4 minutes 31 seconds of “unexampled beauty, grandeur, and impressiveness” (Newcomb 1890) and of darkness.

Responses of Solar Irradiance and the Ionosphere to an Intense Activity Region

NASA Astrophysics Data System (ADS)

Chen, Yiding; Liu, Libo; Le, Huijun; Wan, Weixing

2018-03-01

Solar rotation (SR) variation dominates solar extremely ultraviolet (EUV) changes on the timescale of days. The F10.7 index is usually used as an indicator for solar EUV. The SR variation of F10.7 significantly enhanced during the 2008th-2009th Carrington rotations (CRs) owing to an intense active region; F10.7 increased about 180 units during that SR period. That was the most prominent SR variation of F10.7 during solar cycle 23. In this paper, global electron content (GEC) is used to investigate ionospheric response to that strong variation of solar irradiance indicated by F10.7. The variation of GEC with F10.7 was anomalous (GEC-F10.7 slope significantly decreased) during the 2008th-2009th CRs; however, GEC versus EUV variation during that period was consistent with that during adjacent time intervals when using Solar Heliospheric Observatory/Solar EUV Monitor 26-34 nm EUV measurements. The reason is that F10.7 response to that intense active region was much stronger than EUV response; thus, the EUV-F10.7 slope decreased. We confirmed decreased EUV-F10.7 slope during the 2008th-2009th CRs for different wavelengths within 27-120 nm using Thermosphere, Ionosphere, Mesosphere Energetics and Dynamics/Solar EUV Experiment high spectral resolution EUV measurements. And on the basis of Solar Heliospheric Observatory/Solar EUV Monitor EUV measurements during solar cycle 23, we further presented that EUV-F10.7 slope statistically tends to decrease when the SR variation of F10.7 significantly enhances. Moreover, we found that ionospheric time lag effect to EUV is exaggerated when using F10.7, owing to the time lag effect of EUV to F10.7.

Dominion Radio Astrophysical Observatory

NASA Astrophysics Data System (ADS)

Murdin, P.

2000-11-01

The Dominion Radio Astrophysical Observatory began operating in 1959, and joined the NATIONAL RESEARCH COUNCIL in 1970. It became part of the Herzberg Institute of Astrophysics in 1975. The site near Penticton, BC has a 26 m radio telescope, a seven-antenna synthesis telescope on a 600 m baseline and two telescopes dedicated to monitoring the solar radio flux at 10.7 cm. This part of the Institu...

Community Science and Data Center (CSDC) | ast.noao.edu

Science.gov Websites

ground-based nighttime astronomy in the United States and is operated by the Association of Universities for Research in Astronomy (AURA). under cooperative agreement with the National Science Foundation. If you would like information about solar astronomy, visit the National Solar Observatory. If you would

Solar energy system installed at Mount Rushmore National Visitor Center in Keystone, South Dakota

NASA Technical Reports Server (NTRS)

1979-01-01

The design and installation of the solar energy system installed at the Mount Rushmore Visitor Center is described. The system was designed to furnish about 45 percent of the heating for the total facility and about 53 percent partial cooling for the 2000 square foot observatory.

From Static to Dynamic: Choosing and Implementing a Web-Based CMS

ERIC Educational Resources Information Center

Kneale, Ruth

2008-01-01

Working as systems librarian for the Advanced Technology Solar Telescope (ATST), a project for the National Solar Observatory (NSO) based in Tucson, Arizona, a large part of the author's responsibilities involve running the web site. She began looking into content management systems (CMSs), specifically ones for website control. A CMS is generally…

NASA Marshall Space Flight Center solar observatory report, January - June 1993

NASA Technical Reports Server (NTRS)

Smith, J. E.

1993-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during January-June 1993. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code.

NASA Marshall Space Flight Center Solar Observatory report, July - October 1993

NASA Technical Reports Server (NTRS)

Smith, J. E.

1994-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during June-October 1993. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code.

NASA Marshall Space Flight Center Solar Observatory report, March - May 1994

NASA Technical Reports Server (NTRS)

Smith, J. E.

1994-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during March-May 1994. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code.

Economic Evaluation of Observatory Solar-Energy System

NASA Technical Reports Server (NTRS)

1982-01-01

Long-term economic performance of a commercial solar-energy system was analyzed and used to predict economic performance at four additional sites. Analysis described in report was done to demonstrate viability of design over a broad range of environmental/economic conditions. Topics covered are system description, study approach, economic analysis and system optimization.

Solar Dynamics Observatory Lessons Learned

NASA Technical Reports Server (NTRS)

Rivera, Rachel; Uhl, Andrew; Secunda, Mark

2010-01-01

Mission is to study how solar activity is created and how space weather results from that activity. Atmospheric Imaging Assembly (AIA): High Resolution Images of 10 wavelengths every 10 seconds. Extreme Ultraviolet Variability Experiment (EVE): Measure Sun's brightness in EUV. Helioseismic and Magnetic Imager (HMI): Measures Doppler shift to study waves of the Sun. Launched February 11, 2010.

The Compound and Homologous Eruptions from the SAR 11429

NASA Astrophysics Data System (ADS)

Dhakal, Suman Kumar; Zhang, Jie

2016-05-01

Super Active Regions (SARs) are ARs which shows extremely high rate of solar eruptions. NOAA AR 11429 was a SAR which produced 47 C-Class, 15 M-Class and 3 X-Class flares and 8 CMEs during its passage from the front disk of the Sun. This SAR had anti-Hale and delta-spot magnetic configuration and many sub-regions of magnetic flux emergence. With the aid of multi-wavelength observations of the Solar Dynamics Observatory (SDO), the Solar Terrestrial Relations Observatory (STEREO) and nonlinear force-free model for the magnetic field in the solar corona, we found the existence of many magnetic flux structures (flux bundles) in the corona of the AR. The energy released by these co-existing flux bundles within short time, resulted in compound erutpions from the AR on March 9 and 10, 2012. In the period of 38 hours, after the CME eruption on March 9, the continuous shearing and cancellation and new magnetic flux emergence resulted in another CME on March 10. Both of the events showed the compound nature and the similarity of the foot-points and EUV dimming made these eruptions homologous.

Time-Distance Helioseismology Data-Analysis Pipeline for Helioseismic and Magnetic Imager Onboard Solar Dynamics Observatory (SDO-HMI) and Its Initial Results

NASA Technical Reports Server (NTRS)

Zhao, J.; Couvidat, S.; Bogart, R. S.; Parchevsky, K. V.; Birch, A. C.; Duvall, Thomas L., Jr.; Beck, J. G.; Kosovichev, A. G.; Scherrer, P. H.

2011-01-01

The Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory (SDO/HMI) provides continuous full-disk observations of solar oscillations. We develop a data-analysis pipeline based on the time-distance helioseismology method to measure acoustic travel times using HMI Doppler-shift observations, and infer solar interior properties by inverting these measurements. The pipeline is used for routine production of near-real-time full-disk maps of subsurface wave-speed perturbations and horizontal flow velocities for depths ranging from 0 to 20 Mm, every eight hours. In addition, Carrington synoptic maps for the subsurface properties are made from these full-disk maps. The pipeline can also be used for selected target areas and time periods. We explain details of the pipeline organization and procedures, including processing of the HMI Doppler observations, measurements of the travel times, inversions, and constructions of the full-disk and synoptic maps. Some initial results from the pipeline, including full-disk flow maps, sunspot subsurface flow fields, and the interior rotation and meridional flow speeds, are presented.

Max '91: Flare research at the next solar maximum

NASA Technical Reports Server (NTRS)

Dennis, Brian; Canfield, Richard; Bruner, Marilyn; Emslie, Gordon; Hildner, Ernest; Hudson, Hugh; Hurford, Gordon; Lin, Robert; Novick, Robert; Tarbell, Ted

1988-01-01

To address the central scientific questions surrounding solar flares, coordinated observations of electromagnetic radiation and energetic particles must be made from spacecraft, balloons, rockets, and ground-based observatories. A program to enhance capabilities in these areas in preparation for the next solar maximum in 1991 is recommended. The major scientific issues are described, and required observations and coordination of observations and analyses are detailed. A program plan and conceptual budgets are provided.

Solar physics in Potsdam. (German Title: Sonnenphysik in Potsdam)

NASA Astrophysics Data System (ADS)

Staude, Jürgen

Solar research initiated the establishment of the Astrophysical Observatory Potsdam (AOP) in 1874. The present contribution outlines the development of solar physics in Potsdam from the early history of the AOP to this day. The main topics are the work of Karl Schwarzschild, the investigations related to the general theory of relativity, the foundation of the Einstein tower, Walter Grotrian's founding of modern coronal physics, and the investigations of sunspot magnetic fields.

The Compton Observatory Science Workshop

NASA Technical Reports Server (NTRS)

Shrader, Chris R. (Editor); Gehrels, Neil (Editor); Dennis, Brian (Editor)

1992-01-01

The Compton Observatory Science Workshop was held in Annapolis, Maryland on September 23-25, 1991. The primary purpose of the workshop was to provide a forum for the exchange of ideas and information among scientists with interests in various areas of high energy astrophysics, with emphasis on the scientific capabilities of the Compton Observatory. Early scientific results, as well as reports on in-flight instrument performance and calibrations are presented. Guest investigator data products, analysis techniques, and associated software were discussed. Scientific topics covered included active galaxies, cosmic gamma ray bursts, solar physics, pulsars, novae, supernovae, galactic binary sources, and diffuse galactic and extragalactic emission.

Signature of open magnetic field lines in the extended solar corona and of solar wind acceleration

NASA Technical Reports Server (NTRS)

Antonucci, E.; Giordano, S.; Benna, C.; Kohl, J. L.; Noci, G.; Michels, J.; Fineschi, S.

1997-01-01

The observations carried out with the ultraviolet coronagraph spectrometer onboard the Solar and Heliospheric Observatory (SOHO) are discussed. The purpose of the observations was to determine the line of sight and radial velocity fields in coronal regions with different magnetic topology. The results showed that the regions where the high speed solar wind flows along open field lines are characterized by O VI 1032 and HI Lyman alpha 1216 lines. The global coronal maps of the line of sight velocity were reconstructed. The corona height, where the solar wind reaches 100 km/s, was determined.

Mauna Kea Observatory infrared observations

NASA Technical Reports Server (NTRS)

Jefferies, J. T.

1974-01-01

Galactic and solar system infrared observations are reported using a broad variety of radiometric and spectroscopic instrumentation. Infrared programs and papers published during this period are listed.

The Pierre Auger Observatory scaler mode for the study of solar activity modulation of galactic cosmic rays

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

Abreu, P.; /Lisbon, LIFEP /Lisbon, IST; Aglietta, M.

2011-01-01

Since data-taking began in January 2004, the Pierre Auger Observatory has been recording the count rates of low energy secondary cosmic ray particles for the self-calibration of the ground detectors of its surface detector array. After correcting for atmospheric effects, modulations of galactic cosmic rays due to solar activity and transient events are observed. Temporal variations related with the activity of the heliosphere can be determined with high accuracy due to the high total count rates. In this study, the available data are presented together with an analysis focused on the observation of Forbush decreases, where a strong correlation withmore » neutron monitor data is found.« less

HELIO: The Heliophysics Integrated Observatory

NASA Technical Reports Server (NTRS)

Bentley, R. D.; Csillaghy, A.; Aboudarham, J.; Jacquey, C.; Hapgood, M. A.; Bocchialini, K.; Messerotti, M.; Brooke, J.; Gallagher, P.; Fox, P.;

WMAP Observatory Thermal Design and On-Orbit Thermal Performance

NASA Technical Reports Server (NTRS)

Glazer, Stuart D.; Brown, Kimberly D.; Michalek, Theodore J.; Ancarrow, Walter C.

2003-01-01

The Wilkinson Microwave Anisotropy Probe (WMAP) observatory, launched June 30, 2001, is designed to measure the cosmic microwave background radiation with unprecedented precision and accuracy while orbiting the second Lagrange point (L2). The instrument cold stage must be cooled passively to <95K, and systematic thermal variations in selected instrument components controlled to less than 0.5 mK (rms) per spin period. This paper describes the thermal design and testing of the WMAP spacecraft and instrument. Flight thermal data for key spacecraft and instrument components are presented from launch through the first year of mission operations. Effects of solar flux variation due to the Earth's elliptical orbit about the sun, surface thermo-optical property degradations, and solar flares on instrument thermal stability are discussed.

Bus Vent Design Evolution for the Solar Dynamics Observatory

NASA Technical Reports Server (NTRS)

Woronowicz, Michael

2010-01-01

As a spacecraft undergoes ascent in a launch vehicle, its pressure environment transitions from one atmosphere to high vacuum in a matter of minutes. Venting of internal cavities is necessary to prevent the buildup of pressure differentials across cavity walls. Opposing the need to vent these volumes freely into space are thermal, optical, and electrostatic requirements for limiting or prohibiting the intrusion of unwanted energy into the same cavities. Bus vent design evolution is discussed for the Solar Dynamics Observatory. Design changes were influenced by a number of factors and concerns, such as contamination control, electrostatic discharge, changes in bus material, and driving fairing ascent pressure for a launch vehicle that was just entering service as this satellite project had gotten underway.

AstroGrid: the UK's Virtual Observatory Initiative

NASA Astrophysics Data System (ADS)

Mann, Robert G.; Astrogrid Consortium; Lawrence, Andy; Davenhall, Clive; Mann, Bob; McMahon, Richard; Irwin, Mike; Walton, Nic; Rixon, Guy; Watson, Mike; Osborne, Julian; Page, Clive; Allan, Peter; Giaretta, David; Perry, Chris; Pike, Dave; Sherman, John; Murtagh, Fionn; Harra, Louise; Bentley, Bob; Mason, Keith; Garrington, Simon

AstroGrid is the UK's Virtual Observatory (VO) initiative. It brings together the principal astronomical data centres in the UK, and has been funded to the tune of ˜pounds 5M over the next three years, via PPARC, as part of the UK e--science programme. Its twin goals are the provision of the infrastructure and tools for the federation and exploitation of large astronomical (X-ray to radio), solar and space plasma physics datasets, and the delivery of federations of current datasets for its user communities to exploit using those tools. Whilst AstroGrid's work will be centred on existing and future (e.g. VISTA) UK datasets, it will seek solutions to generic VO problems and will contribute to the developing international virtual observatory framework: AstroGrid is a member of the EU-funded Astrophysical Virtual Observatory project, has close links to a second EU Grid initiative, the European Grid of Solar Observations (EGSO), and will seek an active role in the development of the common standards on which the international virtual observatory will rely. In this paper we shall primarily describe the concrete plans for AstroGrid's one-year Phase A study, which will centre on: (i) the definition of detailed science requirements through community consultation; (ii) the undertaking of a ``functionality market survey" to test the utility of existing technologies for the VO; and (iii) a pilot programme of database federations, each addressing different aspects of the general database federation problem. Further information on AstroGrid can be found at AstroGrid .

Blue Hill Observatory Sunshine - Assessment of Climate Signals in the Longest Continuous Meteorological Record in North America

NASA Astrophysics Data System (ADS)

Magee, N. B.; Finocchio, P.; Melaas, E. K.; Iacono, M. J.

2014-12-01

The Blue Hill Meteorological Observatory occupies a unique place in the history of the American Meteorological Society and the development of atmospheric science. Through its 129-year history, the Observatory has been operated by founder Abbott Lawrence Rotch (1861-1912), Harvard University, and the National Weather Service, and it is presently run by the non-profit Blue Hill Observatory Science Center. While daily temperature and precipitation records are available through the National Climatic Data Center, they do not include the full record of sunshine duration data that were measured using a Campbell-Stokes sunshine recorder. We have recently digitized the Observatory's original daily sunshine archives, and now present the first full collection and analysis of sunshine records extending from 1889 to the present. This data set is unique and salient to modern climate research because the collection represents the earliest and longest continuous measurements of insolation outside of Western Europe. Together the record provides an unprecedented glimpse into regional climate features, as well as important links between global phenomena and regional climate. Analysis reveals long-term fluctuations of cloud-cover and solar radiation, including signals of regional industrialization, global-dimming, volcanic eruptions, the 11-Year Solar Cycle, and the El Niño Southern Oscillation. Shorter period fluctuations include evidence of an intricate annual pattern of sunshine duration and correlations with the Arctic Oscillation, North Atlantic Oscillation, and galactic cosmic rays.

Large-Scale periodic solar velocities: An observational study

NASA Technical Reports Server (NTRS)

Dittmer, P. H.

1977-01-01

Observations of large-scale solar velocities were made using the mean field telescope and Babcock magnetograph of the Stanford Solar Observatory. Observations were made in the magnetically insensitive ion line at 5124 A, with light from the center (limb) of the disk right (left) circularly polarized, so that the magnetograph measures the difference in wavelength between center and limb. Computer calculations are made of the wavelength difference produced by global pulsations for spherical harmonics up to second order and of the signal produced by displacing the solar image relative to polarizing optics or diffraction grating.

SOHO EIT Carrington maps from synoptic full-disk data

NASA Technical Reports Server (NTRS)

Thompson, B. J.; Newmark, J. S.; Gurman, J. B.; Delaboudiniere, J. P.; Clette, F.; Gibson, S. E.

1997-01-01

The solar synoptic maps, obtained from observations carried out since May 1996 by the extreme-ultraviolet imaging telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO), are presented. The maps were constructed for each Carrington rotation with the calibrated data. The off-limb maps at 1.05 and 1.10 solar radii were generated for three coronal lines using the standard applied to coronagraph synoptic maps. The maps reveal several aspects of the solar structure over the entire rotation and are used in the whole sun month modeling campaign. @txt extreme-ultraviolet imaging telescope

Infant oral health: Knowledge, attitude and practices of parents in Udaipur, India

PubMed Central

Nagarajappa, Ramesh; Kakatkar, Gauri; Sharda, Archana J; Asawa, Kailash; Ramesh, Gayathri; Sandesh, Nagarajappa

2013-01-01

Background: The aim of this study was to assess the infant oral health (IOH) related knowledge, attitudes and practices (KAP) of parents in Udaipur, India. Materials and Methods: A cross-sectional descriptive study was conducted among 470 parents visiting the Department of Pediatrics, Rabindranath Tagore Medical College and Hospital. A 32-item questionnaire covering socio-demographic characteristics and questions pertaining to KAP regarding IOH care was used to collect the data. Descriptive statistics, Student's t-test, one-way analysis of variance, and Scheffe's test were used for the statistical analysis (P ≤ 0.05). Results: Majority of the parents had good knowledge regarding tooth eruption, but had a poor knowledge of cleaning (58.7%) and development of caries (48.5%). Parents in the age group of 25-30 years showed significantly higher mean knowledge (25.90 ± 3.93), attitude (15.71 ± 2.23), and practice (20.09 ± 2.50) scores. Female parents showed a significantly higher mean knowledge (21.45 ± 4.27) and attitude scores (14.97 ± 2.15) than the male parents. Conclusion: Parent's knowledge on IOH care was inadequate. Health professionals, who are the first to come into contact with expectant and new mothers, need to disseminate appropriate and accurate information about oral health-care for infants. PMID:24348626

Infant oral health: Knowledge, attitude and practices of parents in Udaipur, India.

PubMed

Nagarajappa, Ramesh; Kakatkar, Gauri; Sharda, Archana J; Asawa, Kailash; Ramesh, Gayathri; Sandesh, Nagarajappa

2013-09-01

The aim of this study was to assess the infant oral health (IOH) related knowledge, attitudes and practices (KAP) of parents in Udaipur, India. A cross-sectional descriptive study was conducted among 470 parents visiting the Department of Pediatrics, Rabindranath Tagore Medical College and Hospital. A 32-item questionnaire covering socio-demographic characteristics and questions pertaining to KAP regarding IOH care was used to collect the data. Descriptive statistics, Student's t-test, one-way analysis of variance, and Scheffe's test were used for the statistical analysis (P ≤ 0.05). Majority of the parents had good knowledge regarding tooth eruption, but had a poor knowledge of cleaning (58.7%) and development of caries (48.5%). Parents in the age group of 25-30 years showed significantly higher mean knowledge (25.90 ± 3.93), attitude (15.71 ± 2.23), and practice (20.09 ± 2.50) scores. Female parents showed a significantly higher mean knowledge (21.45 ± 4.27) and attitude scores (14.97 ± 2.15) than the male parents. Parent's knowledge on IOH care was inadequate. Health professionals, who are the first to come into contact with expectant and new mothers, need to disseminate appropriate and accurate information about oral health-care for infants.

Association of sugary foods and drinks consumption with behavioral risk and oral health status of 12- and 15-year-old Indian school children.

PubMed

Asawa, Kailash; Sen, Nandini; Bhat, Nagesh; Tak, Mridula; Sultane, Pratibha; Patil, Vishal

2018-01-01

This study aims to assess the association of sugary foods and drinks consumption with behavioral risk and oral health status of 12- and 15-year-old government school children in Udaipur. A descriptive cross-sectional study was conducted among of 12- and 15-year-old government schoolchildren of Udaipur. A survey pro forma designed based on HBSC (Health behaviour in School-aged Children) study protocol and WHO Oral Health Assessment Form for Children (2013) was used. Chi-Square test, Independent Sample t -test, and Multinomial Logistic Regression analysis were used with 95% confidence interval and 5% significance level. Out of 710 participants, 455 (64.1%) were males and 255 females (35.9%). Majority of 15 years age (57.3%) consumed more soft drinks than 12-year-old. Males showed a comparatively greater tendency to have sugar sweetened products than females. The decayed, missing, and filled teeth (dmft) and DMFT scores were relatively higher for subjects who consumed sugary substances more than once/day than who had less than once/day. Gingivitis was associated with high sugar diet. Sugary foods and drinks consumption is significantly associated with behavioral habits of children and is a clear behavioral risk for oral health.

Simultaneous control of multiple instruments at the Advanced Technology Solar Telescope

NASA Astrophysics Data System (ADS)

Johansson, Erik M.; Goodrich, Bret

2012-09-01

The Advanced Technology Solar Telescope (ATST) is a 4-meter solar observatory under construction at Haleakala, Hawaii. The simultaneous use of multiple instruments is one of the unique capabilities that makes the ATST a premier ground based solar observatory. Control of the instrument suite is accomplished by the Instrument Control System (ICS), a layer of software between the Observatory Control System (OCS) and the instruments. The ICS presents a single narrow interface to the OCS and provides a standard interface for the instruments to be controlled. It is built upon the ATST Common Services Framework (CSF), an infrastructure for the implementation of a distributed control system. The ICS responds to OCS commands and events, coordinating and distributing them to the various instruments while monitoring their progress and reporting the status back to the OCS. The ICS requires no specific knowledge about the instruments. All information about the instruments used in an experiment is passed by the OCS to the ICS, which extracts and forwards the parameters to the appropriate instrument controllers. The instruments participating in an experiment define the active instrument set. A subset of those instruments must complete their observing activities in order for the experiment to be considered complete and are referred to as the must-complete instrument set. In addition, instruments may participate in eavesdrop mode, outside of the control of the ICS. All instrument controllers use the same standard narrow interface, which allows new instruments to be added without having to modify the interface or any existing instrument controllers.

ON A CORONAL BLOWOUT JET: THE FIRST OBSERVATION OF A SIMULTANEOUSLY PRODUCED BUBBLE-LIKE CME AND A JET-LIKE CME IN A SOLAR EVENT

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

Shen Yuandeng; Liu Yu; Su Jiangtao

2012-02-01

The coronal blowout jet is a peculiar category among various jet phenomena, in which the sheared base arch, often carrying a small filament, experiences a miniature version of blowout eruption that produces large-scale coronal mass ejection (CME). In this paper, we report such a coronal blowout jet with high-resolution multi-wavelength and multi-angle observations taken from Solar Dynamics Observatory, Solar Terrestrial Relations Observatory, and Big Bear Solar Observatory. For the first time, we find that simultaneous bubble-like and jet-like CMEs were dynamically related to the blowout jet that showed cool and hot components next to each other. Our observational results indicatemore » that (1) the cool component resulted from the eruption of the filament contained within the jet's base arch, and it further caused the bubble-like CME; (2) the jet-like CME was associated with the hot component, which was the outward moving heated plasma generated by the reconnection of the base arch and its ambient open field lines. On the other hand, bifurcation of the jet's cool component was also observed, which resulted from the uncoupling of the erupting filament's two legs that were highly twisted at the very beginning. Based on these results, we propose a model to interpret the coronal blowout jet, in which the external reconnection not only produces the jet-like CME, but also leads to the rising of the filament. Subsequently, internal reconnection starts underneath the rising filament and thereby causes the bubble-like CME.« less

Relating Alfvén Wave Heating Model to Observations of a Solar Active Region

NASA Astrophysics Data System (ADS)

Yoritomo, J. Y.; Van Ballegooijen, A. A.

2012-12-01

We compared images from the Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA) with simulations of propagating and dissipating Alfvén waves from a three-dimensional magnetohydrodynamic (MHD) model (van Ballegooijen et. al 2011; Asgari-Targhi & van Ballegooijen 2012). The goal was to search for observational evidence of Alfvén waves in the solar corona and understand their role in coronal heating. We looked at one particular active region on the 5th of May 2012. Certain distinct loops in the SDO/AIA observations were selected and expanded. Movies were created from these selections in an attempt to discover transverse motions that may be Alfvén waves. Using a magnetogram of that day and the corresponding synoptic map, a potential field model was created for the active region. Three-dimensional MHD models for several loops in different locations in the active region were created. Each model specifies the temperature, pressure, magnetic field strength, average heating rate, and other parameters along the loop. We find that the heating is intermittent in the loops and reflection occurs at the transition region. For loops at larger and larger height, a point is reached where thermal non-equilibrium occurs. In the center this critical height is much higher than in the periphery of the active region. Lastly, we find that the average heating rate and coronal pressure decrease with increasing height in the corona. This research was supported by an NSF grant for the Smithsonian Astrophysical Observatory (SAO) Solar REU program and a SDO/AIA grant for the Smithsonian Astrophysical Observatory.

NASA Marshall Space Flight Center Solar Observatory Report, July to December 1992

NASA Technical Reports Server (NTRS)

Smith, J. E.

1993-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during July-December 1992. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code.

NASA Marshall Space Flight Center Solar Observatory report, January - June 1992

NASA Technical Reports Server (NTRS)

Smith, James E.

1992-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during Jan. to Jun. 1992. The systems that make up the facility are a magnetograph telescope, and H-alpha telescope, a Questar telescope, and a computer code.

A Representative Survey of U.S. Space Systems and Methods for Estimating Their Costs

DTIC Science & Technology

1992-11-01

68 TETR.I Radose: U.S. Air Force satellites carrying radiation dosimeters Radose 06/15/63 07/30/63 Radose-5E1 09/28/63 SN39 Radose-5EIA 12105/63... OSL Orbiting Solar Laboratory OSO Orbiting Solar Observatory OSSA Office of Space Science and Applications OSSE Oriented Scintillation Spectrometer

Research at the Stanford Center for Radar Astronomy

NASA Technical Reports Server (NTRS)

1972-01-01

The research is reported in the applications of radar and radio techniques to the study of the solar system, and to space programs. Experiments reported include: bistatic-radar on Apollo missions, development of an unmanned geophysical observatory in the Antartic, Bragg scattering probes of sea states, characteristics of dense solar wind disturbances, and satellite communications for Alaska.

The solar cycle; Proceedings of the National Solar Observatory/Sacramento Peak 12th Summer Workshop, Sunspot, NM, Oct. 15-18, 1991

NASA Technical Reports Server (NTRS)

Harvey, Karen L. (Editor)

1992-01-01

Attention is given to a flux-transport model, the effect of fractal distribution on the evolution of solar surface magnetic fields, active nests on the sun, magnetic flux transport in solar active regions, recent advances in stellar cycle research, magnetic intermittency on the sun, a search for existence of large-scale motions on the sun, and new solar cycle data from the NASA/NSO spectromagnetograph. Attention is also given to the solar cycle variation of coronal temperature during cycle 22, the distribution of the north-south asymmetry for the various activity cycles, solar luminosity variation, a two-parameter model of total solar irradiance variation over the solar cycle, the origin of the solar cycle, nonlinear feedbacks in the solar dynamo, and long-term dynamics of the solar cycle.

Extra Solar Planetary Imaging Coronagraph and Science Requirements for the James Webb Telescope Observatory

NASA Technical Reports Server (NTRS)

Clampin, Mark

2004-01-01

1) Extra solar planetary imaging coronagraph. Direct detection and characterization of Jovian planets, and other gas giants, in orbit around nearby stars is a necessary precursor to Terrestrial Planet Finder 0 in order to estimate the probability of Terrestrial planets in our stellar neighborhood. Ground based indirect methods are biased towards large close in Jovian planets in solar systems unlikely io harbor Earthlike planets. Thus to estimate the relative abundances of terrestrial planets and to determine optimal observing strategies for TPF a pathfinder mission would be desired. The Extra-Solar Planetary Imaging Coronagraph (EPIC) is such a pathfinder mission. Upto 83 stellar systems are accessible with a 1.5 meter unobscured telescope and coronagraph combination located at the Earth-Sun L2 point. Incorporating radiometric and angular resolution considerations show that Jovians could be directly detected (5 sigma) in the 0.5 - 1.0 micron band outside of an inner working distance of 5/D with integration times of -10 - 100 hours per observation. The primary considerations for a planet imager are optical wavefront quality due to manufacturing, alignment, structural and thermal considerations. pointing stability and control, and manufacturability of coronagraphic masks and stops to increase the planetary-to- stellar contrast and mitigate against straylight. Previously proposed coronagraphic concepts are driven to extreme tolerances. however. we have developed and studied a mission, telescope and coronagraphic detection concept, which is achievable in the time frame of a Discovery class NASA mission. 2) Science requirements for the James Webb Space Telescope observatory. The James Webb Space Observatory (JWST) is an infrared observatory, which will be launched in 201 1 to an orbit at L2. JWST is a segmented, 18 mirror segment telescope with a diameter of 6.5 meters, and a clear aperture of 25 mA2. The telescope is designed to conduct imaging and spectroscopic observations from 0.6-27 microns. The primary mirror find and understand predicted first light objects, observe galaxies back to their earliest precursors so that we can understand their growth and evolution, unravel the birth and early evolution of stars and planetary systems, and study planetary systems and the origins of life. In this paper we discuss the science goals for JWST in the context of the performance requirements they levy on the observatory.

The Chandra X-Ray Observatory and its Role for the Study of Ionized Plasmas

NASA Technical Reports Server (NTRS)

Weisskopf, Martin C.

2010-01-01

NASA's Chandra X-Ray Observatory was launched in July of 1999. Featuring a 1000cm2-class X-ray telescope with sub-arcsecond angular resolution, the Observatory has observed targets from the solar system including the earth s moon, comets, and planets to the most distant galaxy clusters and active galactic nuclei. Capable of performing moderate energy resolution image-resolved spectroscopy using its CCD detectors, and high-resolution grating spectroscopy, the Observatory has produced, and continues to produce, valuable data and insights into the emission mechanisms of the ionized plasmas in which the X-rays originate. We present a brief overview of the Observatory to provide insight as to how to use it for your investigations. We also present an, admittedly brief and biased, overview of some of the results of investigations performed with Chandra that may be of interest to this audience.

Solar Radio Observation using Callisto Spectrometer at Sumedang West Java Indonesia: Current Status and Future Development Plan in Indonesia

NASA Astrophysics Data System (ADS)

Manik, T.; Sitompul, P.; Batubara, M.; Harjana, T.; Yatini, C. Y.; Monstein, C.

2016-04-01

Sumedang Observatory (6.91°S, 107,84°E) was established in 1975 and is one of the solar observation facilities of the Space Science Center of Indonesian National Institute of Aeronautics and Space (LAPAN), located around 40 km, east part of Bandung City, West Java, Indonesia. Several instrumentations for solar and space observation such as optical telescopes, radio solar spectrograph, flux gate magnetometer, etc. are operated there, together with an ionosphere sounding system (ionosonde) that was set up later. In July 2014, a standard Callisto (Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy and Transportable Observatory) spectrometer was installed at Sumedang Observatory for solar radio activity monitoring. Callisto has been developed in the framework of IHY2007 and ISWI, supported by UN and NASA. Callisto spectrometer has observation capability in the frequency range of 45-870 MHz. The Callisto spectrometer receives signal by using a set of 21 elements log-periodic antenna, model CLP5130-1N, pointed to the Sun and equipped with a low noise pre-amplifier. With respect to the Radio Frequency Interferences (RFI) measurements, the Callisto spectrometer is operated individually in frequency ranges of 45-80 MHz and 180-450 MHz. Observation status and data flow are monitored in on-line from center office located in Bandung. The data was transferred to central database at FHNW (Fachhochschule Nordwestschweiz) server every 15 minutes to appear on e-Callisto network subsequently. A real time data transfer and data processing based on Python software also has been developed successfully to be used as an input for Space Weather Information and Forecasting Services (SWIFtS) provided by LAPAN. On 5th November 2014, Callisto spectrometer at Sumedang observed the first clear solar radio event, a solar radio burst type II corresponding to a coronal mass ejection (CME), indicated by a strong X-ray event of M7.9 that was informed on by Space Weather Prediction Center (SWPC) NOAA. Thereafter, Callisto spectrometer at Sumedang also observed several solar radio bursts in various types. This paper describes the system configuration of Callisto spectrometer installed at Sumedang, RFI measurement and chosen observation strategy, real time data transfer and processing, as well as several samples of present results of solar radio burst monitoring at Sumedang, and future development plan of Callisto spectrometer in Indonesia which will be able to cover 14 hours of day solar observation. Keywords: Callisto spectrometer, solar radio observation, SWIFtS.

Automated Identification of Coronal Holes from Synoptic EUV Maps

NASA Astrophysics Data System (ADS)

Hamada, Amr; Asikainen, Timo; Virtanen, Ilpo; Mursula, Kalevi

2018-04-01

Coronal holes (CHs) are regions of open magnetic field lines in the solar corona and the source of the fast solar wind. Understanding the evolution of coronal holes is critical for solar magnetism as well as for accurate space weather forecasts. We study the extreme ultraviolet (EUV) synoptic maps at three wavelengths (195 Å/193 Å, 171 Å and 304 Å) measured by the Solar and Heliospheric Observatory/Extreme Ultraviolet Imaging Telescope (SOHO/EIT) and the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) instruments. The two datasets are first homogenized by scaling the SDO/AIA data to the SOHO/EIT level by means of histogram equalization. We then develop a novel automated method to identify CHs from these homogenized maps by determining the intensity threshold of CH regions separately for each synoptic map. This is done by identifying the best location and size of an image segment, which optimally contains portions of coronal holes and the surrounding quiet Sun allowing us to detect the momentary intensity threshold. Our method is thus able to adjust itself to the changing scale size of coronal holes and to temporally varying intensities. To make full use of the information in the three wavelengths we construct a composite CH distribution, which is more robust than distributions based on one wavelength. Using the composite CH dataset we discuss the temporal evolution of CHs during the Solar Cycles 23 and 24.

Mingantu, 18th-Century Mongol Astronomer and Radioheliograph Namesake

NASA Astrophysics Data System (ADS)

Pasachoff, Jay M.

2013-01-01

The 18th-century Mongol astronomer Mingantu (1692-1765) has been honored with a city named after him and a nearby solar telescope array. During the IAU/Beijing, my wife and I went to the new Chinese solar radioheliograph, the Mingantu Observing Station, in Inner Mongolia, ~400 km northwest of Beijing, a project of the National Astronomical Observatories, Chinese Academy of Sciences. It currently contains 40 dishes each 4.5 m across, with a correlator from Beijing. Within a year, 60 2-m dishes will be added. We passed by the 12-century ruins of Xanadu (about 20 km north of Zhangbei) about halfway. The radioheliograph is in a plane about 1 km across, forming a three-armed spiral for interferometric solar mapping, something colleagues and I had carried out with the Jansky Very Large Array, taking advantage of the lunar occultation before annularity at the 20 May 2012 solar eclipse. In the central square of Mingantu city, a statue ~10-m high of the Mongol astronomer Mingantu appears. Its base bears a plaque ~1-m high of IAU Minor Planet Circular MPC 45750 announcing the naming in 2002 of asteroid 28242 Mingantu, discovered at a Chinese observatory in 1999. Mingantu carried out orbital calculations, mapping, mathematical work on infinite series, and other scientific research. He is honored by a modern museum behind the statue. The museum's first 40% describes Mingantu and his work, and is followed by some artifacts of the region from thousands of years ago. The final, large room contains a two-meter-square scale model of the radioheliograph, flat-screen televisions running Solar Dynamics Observatory and other contemporary visualizations, orreries and other objects, and large transparencies of NASA and other astronomical imagery. See my post at http://www.skyandtelescope.com/community/skyblog/newsblog/ specfically Astro-Sightseeing_in_Inner_Mongolia-167712965.html. We thank Yihua Yan for arranging the visit and Wang Wei (both NAOC) for accompanying us. My solar research is supported by grant 1047726 from the Solar Research Program/Atmospheric and Geospace Sciences Division/NSF. I am also grateful for a NSF travel grant through AAS.

The LCOGT Network for Solar System Science

NASA Astrophysics Data System (ADS)

Lister, Tim

2012-10-01

Las Cumbres Observatory Global Telescope (LCOGT) network is a planned homogeneous network of over 35 telescopes at 6 locations in the northern and southern hemispheres. This network is versatile and designed to respond rapidly to target of opportunity events and also to do long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make LCOGT ideal for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and ultimately for the discovery of new objects. Currently LCOGT is operating the two 2m Faulkes Telescopes at Haleakala, Maui and Siding Spring Observatory, Australia and in March 2012 completed the install of the first member of the new 1m telescope network at McDonald Observatory, Texas. Further deployments of six to eight 1m telescopes to CTIO in Chile, SAAO in South Africa and Siding Spring Observatory are expected in late 2012-early 2013. I am using the growing LCOGT network to confirm newly detected NEO candidates produced by PanSTARRS (PS1) and other sky surveys and to obtain follow-up astrometry and photometry for radar-targeted objects. I have developed an automated system to retrieve new PS1 NEOs, compute orbits, plan observations and automatically schedule them for follow-up on the robotic telescopes of the LCOGT Network. In the future, LCOGT has proposed to develop a Minor Planet Investigation Project (MPIP) that will address the existing lack of resources for minor planet follow-up, takes advantage of ever-increasing new datasets, and develops a platform for broad public participation in relevant scientific exploration. We plan to produce a cloud-based Solar System investigation environment, a citizen science project (AgentNEO), and a cyberlearning environment, all under the umbrella of MPIP.

Geomagnetic activity during 10 - 11 solar cycles that has been observed by old Russian observatories.

NASA Astrophysics Data System (ADS)

Seredyn, Tomasz; Wysokinski, Arkadiusz; Kobylinski, Zbigniew; Bialy, Jerzy

2016-07-01

A good knowledge of solar-terrestrial relations during past solar activity cycles could give the appropriate tools for a correct space weather forecast. The paper focuses on the analysis of the historical collections of the ground based magnetic observations and their operational indices from the period of two sunspot solar cycles 10 - 11, period 1856 - 1878 (Bartels rotations 324 - 635). We use hourly observations of H and D geomagnetic field components registered at Russian stations: St. Petersburg - Pavlovsk, Barnaul, Ekaterinburg, Nertshinsk, Sitka, and compare them to the data obtained from the Helsinki observatory. We compare directly these records and also calculated from the data of the every above mentioned station IHV indices introduced by Svalgaard (2003), which have been used for further comparisons in epochs of assumed different polarity of the heliospheric magnetic field. We used also local index C9 derived by Zosimovich (1981) from St. Petersburg - Pavlovsk data. Solar activity is represented by sunspot numbers. The correlative and continuous wavelet analyses are applied for estimation of the correctness of records from different magnetic stations. We have specially regard to magnetic storms in the investigated period and the special Carrington event of 1-2 Sep 1859. Generally studied magnetic time series correctly show variability of the geomagnetic activity. Geomagnetic activity presents some delay in relation to solar one as it is seen especially during descending and minimum phase of the even 11-year cycle. This pattern looks similarly in the case of 16 - 17 solar cycles.

Neutrino Observations from the Sudbury Neutrino Observatory

DOE R&D Accomplishments Database

Q. R. Ahmad, R. C. Allen, T. C. Andersen, J. D. Anglin, G. B?hler, J. C. Barton, E. W. Beier, M. Bercovitch, J. Bigu, S. Biller, R. A. Black, I. Blevis, R. J. Boardman, J. Boger, E. Bonvin, M. G. Boulay, M. G. Bowler, T. J. Bowles, S. J. Brice, M. C. Browne, T. V. Bullard, T. H. Burritt, K. Cameron, J. Cameron, Y. D. Chan, M. Chen, H. H. Chen, X. Chen, M. C. Chon, B. T. Cleveland, E. T. H. Clifford, J. H. M. Cowan, D. F. Cowen, G. A. Cox, Y. Dai, X. Dai, F. Dalnoki-Veress, W. F. Davidson, P. J. Doe, G. Doucas, M. R. Dragowsky, C. A. Duba, F. A. Duncan, J. Dunmore, E. D. Earle, S. R. Elliott, H. C. Evans, G. T. Ewan, J. Farine, H. Fergani, A. P. Ferraris, R. J. Ford, M. M. Fowler, K. Frame, E. D. Frank, W. Frati, J. V. Germani, S. Gil, A. Goldschmidt, D. R. Grant, R. L. Hahn, A. L. Hallin, E. D. Hallman, A. Hamer, A. A. Hamian, R. U. Haq, C. K. Hargrove, P. J. Harvey, R. Hazama, R. Heaton, K. M. Heeger, W. J. Heintzelman, J. Heise, R. L. Helmer, J. D. Hepburn, H. Heron, J. Hewett, A. Hime, M. Howe, J. G. Hykawy, M. C. P. Isaac, P. Jagam, N. A. Jelley, C. Jillings, G. Jonkmans, J. Karn, P. T. Keener, K. Kirch, J. R. Klein, A. B. Knox, R. J. Komar, R. Kouzes, T. Kutter, C. C. M. Kyba, J. Law, I. T. Lawson, M. Lay, H. W. Lee, K. T. Lesko, J. R. Leslie, I. Levine, W. Locke, M. M. Lowry, S. Luoma, J. Lyon, S. Majerus, H. B. Mak, A. D. Marino, N. McCauley, A. B. McDonald, D. S. McDonald, K. McFarlane, G. McGregor, W. McLatchie, R. Meijer Drees, H. Mes, C. Mifflin, G. G. Miller, G. Milton, B. A. Moffat, M. Moorhead, C. W. Nally, M. S. Neubauer, F. M. Newcomer, H. S. Ng, A. J. Noble, E. B. Norman, V. M. Novikov, M. O'Neill, C. E. Okada, R. W. Ollerhead, M. Omori, J. L. Orrell, S. M. Oser, A. W. P. Poon, T. J. Radcliffe, A. Roberge, B. C. Robertson, R. G. H. Robertson, J. K. Rowley, V. L. Rusu, E. Saettler, K. K. Schaffer, A. Schuelke, M. H. Schwendener, H. Seifert, M. Shatkay, J. J. Simpson, D. Sinclair, P. Skensved, A. R. Smith, M. W. E. Smith, N. Starinsky, T. D. Steiger, R. G. Stokstad, R. S. Storey, B. Sur, R. Tafirout, N. Tagg, N. W. Tanner, R. K. Taplin, M. Thorman, P. Thornewell, P. T. Trent, Y. I. Tserkovnyak, R. Van Berg, R. G. Van de Water, C. J. Virtue, C. E. Waltham, J.-X. Wang, D. L. Wark, N. West, J. B. Wilhelmy, J. F. Wilkerson, J. Wilson, P. Wittich, J. M. Wouters, and M. Yeh

2001-09-24

The Sudbury Neutrino Observatory (SNO) is a water imaging Cherenkov detector. Its usage of 1000 metric tons of D{sub 2}O as target allows the SNO detector to make a solar-model independent test of the neutrino oscillation hypothesis by simultaneously measuring the solar {nu}{sub e} flux and the total flux of all active neutrino species. Solar neutrinos from the decay of {sup 8}B have been detected at SNO by the charged-current (CC) interaction on the deuteron and by the elastic scattering (ES) of electrons. While the CC reaction is sensitive exclusively to {nu}{sub e}, the ES reaction also has a small sensitivity to {nu}{sub {mu}} and {nu}{sub {tau}}. In this paper, recent solar neutrino results from the SNO experiment are presented. It is demonstrated that the solar flux from {sup 8}B decay as measured from the ES reaction rate under the no-oscillation assumption is consistent with the high precision ES measurement by the Super-Kamiokande experiment. The {nu}{sub e} flux deduced from the CC reaction rate in SNO differs from the Super-Kamiokande ES results by 3.3{sigma}. This is evidence for an active neutrino component, in additional to {nu}{sub e}, in the solar neutrino flux. These results also allow the first experimental determination of the total active {sup 8}B neutrino flux from the Sun, and is found to be in good agreement with solar model predictions.

"Route of astronomical observatories'' project: classical observatories from the Renaissance to the rise of astrophysics

NASA Astrophysics Data System (ADS)

Wolfschmidt, Gudrun

2015-08-01

Observatories offer a good possibility for serial transnational applications. A well-known example for a thematic programme is the Struve arc, already recognized as World Heritage.I will discuss what has been achieved and show examples, like the route of astronomical observatories or the transition from classical astronomy to modern astrophysics (La Plata, Hamburg, Nice, etc.), visible in the architecture, the choice of instruments, and the arrangement of the observatory buildings in an astronomy park. This corresponds to the main categories according to which the ``outstanding universal value'' (UNESCO criteria ii, iv and vi) of the observatories have been evaluated: historic, scientific, and aesthetic. This proposal is based on the criteria of a comparability of the observatories in terms of the urbanistic complex and the architecture, the scientific orientation, equipment of instruments, authenticity and integrity of the preserved state, as well as in terms of historic scientific relations and scientific contributions.Apart from these serial transnational applications one can also choose other groups like baroque or neo-classical observatories, solar physics observatories or a group of observatories equipped with the same kind of instruments and made by the same famous firm. I will also discuss why the implementation of the Astronomy and World Heritage Initiative is difficult and why there are problems to nominate observatories for election in the national Tentative Lists

Calibration development strategies for the Daniel K. Inouye Solar Telescope (DKIST) data center

NASA Astrophysics Data System (ADS)

Watson, Fraser T.; Berukoff, Steven J.; Hays, Tony; Reardon, Kevin; Speiss, Daniel J.; Wiant, Scott

2016-07-01

The Daniel K. Inouye Solar Telescope (DKIST), currently under construction on Haleakalā, in Maui, Hawai'i will be the largest solar telescope in the world and will use adaptive optics to provide the highest resolution view of the Sun to date. It is expected that DKIST data will enable significant and transformative discoveries that will dramatically increase our understanding of the Sun and its effects on the Sun-Earth environment. As a result of this, it is a priority of the DKIST Data Center team at the National Solar Observatory (NSO) to be able to deliver timely and accurately calibrated data to the astronomical community for further analysis. This will require a process which allows the Data Center to develop calibration pipelines for all of the facility instruments, taking advantage of similarities between them, as well as similarities to current generation instruments. There will also be a challenges which are addressed in this article, such as the large volume of data expected, and the importance of supporting both manual and automated calibrations. This paper will detail the current calibration development strategies being used by the Data Center team at the National Solar Observatory to manage this calibration effort, so as to ensure delivery of high quality scientific data routinely to users.

Sun Emits an X2.2 Flare on March 11, 2015

NASA Image and Video Library

2015-03-11

The sun emitted a significant solar flare, peaking at 12:22 p.m. EDT on March 11, 2015. NASA’s Solar Dynamics Observatory, which watches the sun constantly, captured an image of the event. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however -- when intense enough -- they can disturb the atmosphere in the layer where GPS and communications signals travel. This flare is classified as an X2.2-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. This image was captured by NASA's Solar Dynamics Observatory and shows a blend of light from the 171 and 131 Ångström wavelengths. The Earth is shown to scale. Credit: NASA/Goddard/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Design and Ground Calibration of the Helioseismic and Magnetic Imager (HMI) Instrument on the Solar Dynamics Observatory (SDO)

NASA Technical Reports Server (NTRS)

Schou, J.; Scherrer, P. H.; Bush, R. I.; Wachter, R.; Couvidat, S.; Rabello-Soares, M. C.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.; Duvall, T. L., Jr.;

“Dandelion” Filament Eruption and Coronal Waves Associated with a Solar Flare on 2011 February 16

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

Cabezas, Denis P.; Ishitsuka, Mutsumi; Ishitsuka, José K.

Coronal disturbances associated with solar flares, such as H α Moreton waves, X-ray waves, and extreme ultraviolet (EUV) coronal waves, are discussed herein in relation to magnetohydrodynamic fast-mode waves or shocks in the corona. To understand the mechanism of coronal disturbances, full-disk solar observations with high spatial and temporal resolution over multiple wavelengths are of crucial importance. We observed a filament eruption, whose shape is like a “dandelion,” associated with the M1.6 flare that occurred on 2011 February 16 in H α images taken by the Flare Monitoring Telescope at Ica University, Peru. We derive the three-dimensional velocity field ofmore » the erupting filament. We also identify winking filaments that are located far from the flare site in the H α images, whereas no Moreton wave is observed. By comparing the temporal evolution of the winking filaments with those of the coronal wave seen in the EUV images data taken by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory and by the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory-Ahead , we confirm that the winking filaments were activated by the EUV coronal wave.« less

The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection

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

Yan, X. L.; Xue, Z. K.; Wang, J. C.

Solar flares and coronal mass ejections are the most powerful explosions in the Sun. They are major sources of potentially destructive space weather conditions. However, the possible causes of their initiation remain controversial. Using high-resolution data observed by the New Solar Telescope of Big Bear Solar Observatory, supplemented by Solar Dynamics Observatory observations, we present unusual observations of a small-scale emerging flux rope near a large sunspot, whose eruption produced an M-class flare and a coronal mass ejection. The presence of the small-scale flux rope was indicated by static nonlinear force-free field extrapolation as well as data-driven magnetohydrodynamics modeling ofmore » the dynamic evolution of the coronal three-dimensional magnetic field. During the emergence of the flux rope, rotation of satellite sunspots at the footpoints of the flux rope was observed. Meanwhile, the Lorentz force, magnetic energy, vertical current, and transverse fields were increasing during this phase. The free energy from the magnetic flux emergence and twisting magnetic fields is sufficient to power the M-class flare. These observations present, for the first time, the complete process, from the emergence of the small-scale flux rope, to the production of solar eruptions.« less

The Kanzelhöhe Observatory

NASA Astrophysics Data System (ADS)

Pötzi, Werner; Temmer, Manuela; Veronig, Astrid; Hirtenfellner-Polanec, Wolfgang; Baumgartner, Dietmar

2013-04-01

Kanzelhöhe Observatory (KSO; kso.ac.at) located in the South of Austria is part of the Institute of Physics of the University of Graz. Since the early 1940s, the Sun has been observed in various layers and wavelengths. Currently, KSO provides high-cadence full-disk observations of the solar disk in three wavelengths: H-alpha line, Ca II K line, white light. Real-time images are published online. For scientific use, the data is processed, and immediately available to the scientific community after each observing day via the Kanzelhöhe Online Data Archive archive (KODA; kanzelhohe.uni-graz.at). KSO is part of the Global H-Alpha Network and is also one of the contributing stations for the international sunspot number. In the frame of ESA's Space Situational Awareness program, methods are currently under development for near-real image recognition with respect to solar flares and filaments. These data products will give valuable complementary information for the solar sources of space weather.

Integrating a Data Center and Resident Archive into the Emerging Virtual Observatiry System: Practical experience and perspectives

NASA Astrophysics Data System (ADS)

Davis, A. J.; Kanekal, S. G.; Looper, M. D.; Mason, G. M.; Mewaldt, R. A.

2006-12-01

The SAMPEX Resident Archive is currently under construction, and will be co-hosted at Caltech with the ACE Science Center. With SAMPEX in low earth orbit, and ACE at L1, and a suite of instruments on each spacecraft, the combined data cover a very broad range in species, energy, location, and time. The data include solar wind, solar energetic particle, and galactic cosmic ray intensity and composition data, as well as solar wind and magnetic field parameters on a variety of time scales. We describe our recent efforts to provide enhanced access to these data via the emerging virtual observatory system, including work with the Space Physics Archive Search and Extract (SPASE) Consortium to ensure that the ACE and SAMPEX data can be adequately described using the SPASE data model, development of a SOAP web services interface between the ACE Science Center and the virtual observatories, and ideas for combining the ACE and SAMPEx data in useful ways.

Calibration of the Reflected Solar Instrument for the Climate Absolute Radiance and Refractivity Observatory

NASA Technical Reports Server (NTRS)

Thome, Kurtis; Barnes, Robert; Baize, Rosemary; O'Connell, Joseph; Hair, Jason

2010-01-01

The Climate Absolute Radiance and Refractivity Observatory (CLARREO) plans to observe climate change trends over decadal time scales to determine the accuracy of climate projections. The project relies on spaceborne earth observations of SI-traceable variables sensitive to key decadal change parameters. The mission includes a reflected solar instrument retrieving at-sensor reflectance over the 320 to 2300 nm spectral range with 500-m spatial resolution and 100-km swath. Reflectance is obtained from the ratio of measurements of the earth s surface to those while viewing the sun relying on a calibration approach that retrieves reflectance with uncertainties less than 0.3%. The calibration is predicated on heritage hardware, reduction of sensor complexity, adherence to detector-based calibration standards, and an ability to simulate in the laboratory on-orbit sources in both size and brightness to provide the basis of a transfer to orbit of the laboratory calibration including a link to absolute solar irradiance measurements.

Jitter Test Program and On-Orbit Mitigation Strategies for Solar Dynamic Observatory

NASA Technical Reports Server (NTRS)

Liu, Kuo-Chia; Kenney, Thomas; Maghami, Peiman; Mule, Pete; Blaurock, Carl; Haile, William B.

2007-01-01

The Solar Dynamic Observatory (SDO) aims to study the Sun's influence on the Earth, the source, storage, and release of the solar energy, and the interior structure of the Sun. During science observations, the jitter stability at the instrument focal plane must be maintained to less than a fraction of an arcsecond for two of the SDO instruments. To meet these stringent requirements, a significant amount of analysis and test effort has been devoted to predicting the jitter induced from various disturbance sources. This paper presents an overview of the SDO jitter analysis approach and test effort performed to date. It emphasizes the disturbance modeling, verification, calibration, and validation of the high gain antenna stepping mechanism and the reaction wheels, which are the two largest jitter contributors. This paper also describes on-orbit mitigation strategies to protect the system from analysis model uncertainties. Lessons learned from the SDO jitter analyses and test programs are included in the paper to share the knowledge gained with the community.

Observing Solar Radio Bursts from the Lunar Surface

NASA Technical Reports Server (NTRS)

MacDowall, R. J.; Gopalswamy, N.; Kaiser, M. L.; Lazio, T. J.; Jones, D. L.; Bale, S. D.; Burns, J.; Kasper, J. C.; Weiler, K. W.

2011-01-01

Locating low frequency radio observatories on the lunar surface has a number of advantages, including fixes locations for the antennas and no terrestrial interference on the far side of the moon. Here, we describe the Radio Observatory for Lunar Sortie Science (ROLSS), a concept for a low frequency, radio imaging interferometric array designed to study particle acceleration in the corona and inner heliosphere. ROLSS would be deployed during an early lunar sortie or by a robotic rover as part of an unmanned landing. The prime science mission is to image type II and type III solar radio bursts with the aim of determining the sites at and mechanisms by which the radiating particles are accelerated. Secondary science goals include constraining the density of the lunar ionosphere by searching for a low radio frequency cutoff of the solar radio emissions and constraining the low energy electron population in astrophysical sources. Furthermore, ROLSS serves a pathfinder function for larger lunar radio arrays designed for faint sources.

Solar-Heliospheric-Interstellar Cosmic Ray Tour with the NASA Virtual Energetic Particle Observatory and the Space Physics Data Facility

NASA Astrophysics Data System (ADS)

Cooper, John F.; Papitashvili, Natalia E.; Johnson, Rita C.; Lal, Nand; McGuire, Robert E.

2015-04-01

NASA now has a large collection of solar, heliospheric, and local interstellar (Voyager 1) cosmic ray particle data sets that can be accessed through the data system services of the NASA Virtual Energetic Particle Observatory (VEPO) in collaboration with the NASA Space Physics Data Facility SPDF), respectively led by the first and last authors. The VEPO services were developed to enhance the long-existing OMNIWeb solar wind and energetic particle services of SPDF for on-line browse, correlative, and statistical analysis of NASA and ESA mission fields, plasma, and energetic particle data. In this presentation we take of tour through VEPO and SPDF of SEP reservoir events, the outer heliosphere earlier surveyed by the Pioneer, Voyager, and Ulysses spacecraft and now being probed by New Horizons, and the heliosheath-heliopause-interstellar regions now being explored by the Voyagers and IBEX. Implications of the latter measurements are also considered for the flux spectra of low to high energy cosmic rays in interstellar space.

Tight Loops Close-Up [video

NASA Image and Video Library

2014-05-19

NASA's Solar Dynamics Observatory (SDO) zoomed in almost to its maximum level to watch tight, bright loops and much longer, softer loops shift and sway above an active region on the sun, while a darker blob of plasma in their midst was pulled about every which way (May 13-14, 2014). The video clip covers just over a day beginning at 14:19 UT on May 13. The frames were taken in the 171-angstroms wavelength of extreme ultraviolet light, but colorized red, instead of its usual bronze tone. This type of dynamic activity continues almost non-stop on the sun as opposing magnetic forces tangle with each other. Credit: NASA/Solar Dynamics Observatory NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Obituary: Helen Dodson Prince, 1905-2002

NASA Astrophysics Data System (ADS)

Lindner, Rudi Paul

2009-01-01

Helen Dodson Prince, a pioneer in the observation of solar flares, a pioneer in women's rise in the profession of astronomy, and a respected and revered educator of future astronomers, died on 4 February 2002 in Arlington, Virginia. Helen Dodson was born in Baltimore, Maryland, on 31 December 1905. Her parents were Helen Walter and Henry Clay Dodson. Helen went to Goucher College in nearby Towson with a full scholarship in mathematics. She turned to astronomy under the influence of a legendary teacher, Professor Florence P. Lewis, and she graduated in 1927. Funded by grants and private charity, she earned the Ph.D. in astronomy at the University of Michigan under the direction of Heber Doust Curtis in 1933. Dodson taught at Wellesley College from 1933 until 1943, when she went on leave to spend the last three years of World War II at the MIT Radiation Laboratory. She returned to Goucher after the war as professor of astronomy and mathematics, and in 1947 she came back to Michigan both as professor of astronomy and staff member of the McMath-Hulbert Observatory, of which she became associate director. In 1976 she retired from Michigan and spent her later years in Alexandria, Virginia. In 1932 Dodson held the Dean Van Meter fellowship from Goucher; in 1954 she received the Annie Jump Cannon Prize from the AAS; and in 1974 The University of Michigan honored her with its Faculty Distinguished Achievement Award. She published over 130 articles, mostly on her research specialty, solar flares. Dodson's interest in the Sun began at Michigan, although her dissertation was, like so many Michigan dissertations of the era, on stellar spectroscopy, "A Study of the Spectrum of 25 Orionis." She came to Michigan during the establishment and growth of the solar observatory at Lake Angelus, the creation of three gifted and industrious amateurs. Heber Curtis fostered the growth of the McMath-Hulbert enterprise and brought it into the University. Dodson's solar activity grew as a result of a number of summers spent, during her Wellesley years, at the solar observatory at Meudon, near Paris. When she returned to Michigan, Dodson became involved in the study of solar flares, based upon the long series of daily observations made with the tower telescopes at Lake Angelus and the improved spectroscopic equipment developed by Robert McMath, Orren Mohler, Leo Goldberg, Keith Pierce, and others. Her colleague during most of these years was Emma Ruth Hedeman, who co-authored many articles with her. Among her great accomplishments was the Comprehensive Flare Index, a widely used measure of flare activity. A "real live wire" and "a marvelous woman," in the words of students and colleagues, Dodson was also a kind and effective teacher, not at all vain about her accomplishments: She held that solar behavior has a way of making people humble. Dodoson was married to Edmund L. Prince and lived across Lake Angelus from the McMath-Hulbert Observatory; often she sailed to work, a joy denied to almost all other astronomers. During her years at McMath-Hulbert, The University of Michigan was the sole major American research university to have two women holding professorial positions in astronomy: Helen Dodson Prince and Hazel Marie Losh. One of the founding members of the Solar Physics Division, Professor Prince was a major factor in the rise and success of the McMath-Hulbert Observatory, even when, after the 1950s, urban growth and upper Midwestern weather conditions conspired to cripple the advantages the observatory's technologies had once conferred. Her colleagues and students recall her with great respect and affection.

The three-dimensional angular widths of CMEs and their relations to the source regions

NASA Astrophysics Data System (ADS)

Zhao, X.; Feng, X. S.

2017-12-01

The angular width of a coronal mass ejection (CME) is an important factor to determine whether the corresponding interplanetary CME (ICME) and its preceding shock will reach our Earth. However, very few studies are involved to study the decisive factors of the CME's angular width. In this study, we use the three-dimensional (3D) angular width of CMEs obtained from the Graduated Cylindrical Shell (GCS) model based on observations of Solar Terrestrial Relations Observatory (STEREO) to study the relations between the CME's 3D width and characteristics of the CME's source region. We find that for the CMEs produced by active regions (ARs), the CME width has some correlations with the AR's area and flux, but these correlations are not strong. The magnetic flux contained in the CME seems to come from only part of the AR's total flux. For the CMEs produced by flare regions, the correlations between the CME angular width and the flare region's area and flux are strong. The magnetic flux within those CMEs seems to totally (even not enough) come from the flare region. Our findings prefer to support that the CME's 3D angular width can be generally estimated based on observations of Solar Dynamics Observatory (SDO) for its source region instead of the observations from coronagraphs onboard Solar and Heliospheric Observatory (SOHO) and STEREO.

Mid-level Solar Flare

NASA Image and Video Library

2014-10-02

NASA's Solar Dynamics Observatory captured these images of a solar flare on Oct. 2, 2014. The solar flare is the bright flash of light on the right limb of the sun. A burst of solar material erupting out into space can be seen just below it. Read more: 1.usa.gov/1mW8rel Credit: NASA/Goddard/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

ATLAS-SOHO: Satellite Arrival and Uncrating, Uncrating of the Propulsion Unit and Electric Module

NASA Technical Reports Server (NTRS)

1995-01-01

The SOHO satellite, part of the International Solar-Terrestrial Physics Program (ISTP), is a solar observatory designed to study the structure, chemical composition, and dynamics of the solar interior. It will also observe the structure (density, temperature and velocity fields), dynamics and composition of the outer solar atmosphere, and the solar wind and its relation to the solar atmosphere. The spacecraft was launched on December 2, 1995. This video shows the unloading of the satellite from the transport plane at the Kennedy Space Station and the lowering to an awaiting flatbed truck. The video also shows the uncrating of the satellite, the propulsion unit and the electric module in a clean room.

Space Motions of Low-Mass Stars. III.

NASA Astrophysics Data System (ADS)

Upgren, A. R.; Sperauskas, J.; Boyle, R. P.

Radial velocity observations are presented for 149 stars taken from the McCormick lists of dwarf K and M stars in a continuing program of radial velocities of faint nearby stars. The data will serve to derive a total stellar density of these kinds of stars in the solar neighborhood. These data were obtained with the spectrometer of the Vilnius University Observatory mounted on the 1.6 m Kuiper Telescope of the Steward Observatory.

Space science

NASA Technical Reports Server (NTRS)

1975-01-01

A fact sheet on the NASA space science program is presented. Some of the subjects considered include the following: (1) the Orbiting Astronomical Observatory, (2) the Orbiting Solar Observatory, (3) the Small Astronomy Satellite, (4) lunar programs, (5) planetary programs using the Mariner, Pioneer 10, and Viking space probes, and (6) the Scout, Thor-Delta, and Atlas-Centaur launch vehicles. For each program there is a description of the effort, the schedule, management, program officials, and funding aspects in outline form.

Cyclic and Long-Term Variation of Sunspot Magnetic Fields

DTIC Science & Technology

2014-10-15

observations from the Royal Greenwich Observatory (RGO) to establish a relationship between the sunspot areas and the sunspot field strengths for...cycles 15 – 19. This relationship was used to create a proxy of the peak magnetic field strength based on sunspot areas from the RGO and the USAF/NOAA...Next, we used the sunspot observations from the Royal Greenwich Observatory (RGO) to establish a relationship between the sunspot ar- Solar Origins of

Istoriko-Astronomicheskie Issledovaniya %t Studies in the History of Astronomy

NASA Astrophysics Data System (ADS)

Idlis, G. M.

This collection contains papers covering a wide scope of problems in the history of astronomy, both domestic and worldwide. It includes the following basic subdivisions: Astronomy, cosmology and cosmogony of the 20th century; researches and findings; ancient and medieval astronomy; history of observatories and others. Among the most interesting problems considered in the present issue: the origin of the Earth and the geospheres: a bit of history and the current state of the problem; the Near-Earth Astronomy as an independent astronomical discipline; the problem of visual registration of observations in optical astronomy in the 17th - 18th centuries; evidence of lunar and solar calendars in Russian chronicles; the history of the first observatory of the Moscow University; the history of Pulkovo observatory for the last 50 years; the life and activity of the outstanding Russian astronomer A. A. Belopolsky (for his 150th anniversary); a reconstruction of Philolaus' solar system model; and many others. The book is addressed to professional scientists, astronomy amateurs, pedagogues, and everybody interested in the history of science.

Solar Dynamics Observatory On-Orbit Jitter Testing, Analysis, and Mitigation Plans

NASA Technical Reports Server (NTRS)

Liu, Kuo-Chia; Blaurock, Carl A.; Bourkland, Kristin L.; Morgenstern, Wendy M.; Maghami, Peiman G.

2011-01-01

The recently launched Solar Dynamics Observatory (SDO) has two science instruments onboard that required sub-arcsecond pointing stability. Significant effort has been spent pre-launch to characterize the disturbances sources and validating jitter level at the component, sub-assembly, and spacecraft levels. However, an end-to-end jitter test emulating the flight condition was not performed on the ground due to cost and risk concerns. As a result, the true jitter level experienced on orbit remained uncertain prior to launch. Based on the pre-launch analysis, several operational constraints were placed on the observatory aimed to minimize the instrument jitter levels. If the actual jitter is below the analysis predictions, these operational constraints can be relaxed to reduce the burden of the flight operations team. The SDO team designed a three-day jitter test, utilizing the instrument sensors to measure pointing jitter up to 256 Hz. The test results were compared to pre-launch analysis predictions, used to determine which operational constraints can be relaxed, and analyzed for setting the jitter mitigation strategies for future SDO operations.

Extreme Ultraviolet Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO): Overview of Science Objectives, Instrument Design, Data Products, and Model Developments

NASA Technical Reports Server (NTRS)

Woods, T. N.; Eparvier, F. G.; Hock, R.; Jones, A. R.; Woodraska, D.; Judge, D.; Didkovsky, L.; Lean, J.; Mariska, J.; Warren, H.;

The Ultimate Private Observatory

NASA Astrophysics Data System (ADS)

Aymond, J.

2009-03-01

An amateur astronomer from Washington Parish, Southeast Louisiana, USA has designed and built an amazing observatory. It is not only an astronomical observatory, but a home theater, and tornado shelter designed to take a direct hit from an F5 tornado. The facility is fully equipped and automated, with a hydraulically driven roof that weighs 20,571 lbs., which lifts up, then rolls away to the end of the tracks. This leaves the user sitting inside of four 14-foot high walls open to the night sky. It has two premium quality telescopes for viewing deep space and objects inside the solar system. The chair that the observer sits on is also hydraulically driven.

Spacecraft Conceptual Design for the 8-Meter Advanced Technology Large Aperture Space Telescope (ATLAST)

NASA Technical Reports Server (NTRS)

Hopkins, Randall C.; Capizzo, Peter; Fincher, Sharon; Hornsby, Linda S.; Jones, David

2010-01-01

The Advanced Concepts Office at Marshall Space Flight Center completed a brief spacecraft design study for the 8-meter monolithic Advanced Technology Large Aperture Space Telescope (ATLAST-8m). This spacecraft concept provides all power, communication, telemetry, avionics, guidance and control, and thermal control for the observatory, and inserts the observatory into a halo orbit about the second Sun-Earth Lagrange point. The multidisciplinary design team created a simple spacecraft design that enables component and science instrument servicing, employs articulating solar panels for help with momentum management, and provides precise pointing control while at the same time fast slewing for the observatory.

Minerva: A Dedicated Observatory for the Detection of Small Planets in the Solar Neighborhood

NASA Astrophysics Data System (ADS)

Hogstrom, Kristina; Johnson, J. A.; Wright, J.; McCrady, N.; Swift, J.; Muirhead, P.; Bottom, M.; Plavchan, P.; Zhao, M.; Riddle, R. L.

2013-01-01

Minerva is an array of 0.7m aperture robotic telescopes to be built atop Palomar Mountain outfitted for both photometry and high-resolution spectroscopy. It will be the first U.S. observatory dedicated to exoplanetary science capable of both precise radial velocimetry and transit studies. The multi-telescope concept will be implemented to either observe separate targets or a single target with a larger effective aperture. The flexibility of the observatory will maximize scientific potential and also provide ample opportunities for education and public outreach. The design and implementation of Minerva will be carried out by postdoctoral and student researchers at Caltech.

An Experimentalist's Overview of Solar Neutrinos

NASA Astrophysics Data System (ADS)

Oser, Scott M.

2012-02-01

Four decades of solar neutrino research have demonstrated that solar models do a remarkable job of predicting the neutrino fluxes from the Sun, to the extent that solar neutrinos can now serve as a calibrated neutrino source for experiments to understand neutrino oscillations and mixing. In this review article I will highlight the most significant experimental results, with emphasis on the latest model-independent measurements from the Sudbury Neutrino Observatory. The solar neutrino fluxes are seen to be generally well-determined experimentally, with no indications of time variability, while future experiments will elucidate the lower energy part of the neutrino spectrum, especially pep and CNO neutrinos.

Depth and latitude dependence of the solar internal angular velocity

NASA Technical Reports Server (NTRS)

Rhodes, Edward J., Jr.; Cacciani, Alessandro; Korzennik, Sylvain; Tomczyk, Steven; Ulrich, Roger K.; Woodard, Martin F.

1990-01-01

One of the design goals for the dedicated helioseismology observing state located at Mount Wilson Observatory was the measurement of the internal solar rotation using solar p-mode oscillations. In this paper, the first p-mode splittings obtained from Mount Wilson are reported and compared with those from several previously published studies. It is demonstrated that the present splittings agree quite well with composite frequency splittings obtained from the comparisons. The splittings suggest that the angular velocity in the solar equatorial plane is a function of depth below the photosphere. The latitudinal differential rotation pattern visible at the surface appears to persist at least throughout the solar convection zone.

Mid-level Solar Flare

NASA Image and Video Library

2017-12-08

SDO View of M7.3 Class Solar Flare on Oct. 2, 2014 NASA's Solar Dynamics Observatory captured this image of an M7.3 class solar flare on Oct. 2, 2014. The solar flare is the bright flash of light on the right limb of the sun. A burst of solar material erupting out into space can be seen just below it. Credit: NASA/Goddard/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

An Empirical Model of the Variation of the Solar Lyman-α Spectral Irradiance

NASA Astrophysics Data System (ADS)

Kretzschmar, Matthieu; Snow, Martin; Curdt, Werner

2018-03-01

We propose a simple model that computes the spectral profile of the solar irradiance in the hydrogen Lyman alpha line, H Ly-α (121.567 nm), from 1947 to present. Such a model is relevant for the study of many astronomical environments, from planetary atmospheres to interplanetary medium. This empirical model is based on the SOlar Heliospheric Observatory/Solar Ultraviolet Measurement of Emitted Radiation observations of the Ly-α irradiance over solar cycle 23 and the Ly-α disk-integrated irradiance composite. The model reproduces the temporal variability of the spectral profile and matches the independent SOlar Radiation and Climate Experiment/SOLar-STellar Irradiance Comparison Experiment spectral observations from 2003 to 2007 with an accuracy better than 10%.

Sun Emits a Mid-Level Flare on Dec. 4, 2014

NASA Image and Video Library

2017-12-08

The sun emitted a solar flare on Dec. 4, 2014, seen as the flash of light in this image from NASA's Solar Dynamics Observatory. The image blends two wavelengths of extreme ultraviolet light – 131 and 171 Angstroms – which are typically colored in teal and gold, respectively. Read more: 1.usa.gov/121n7PP Image Credit: NASA/SDO

NASA Marshall Space Flight Center Solar Observatory report, January - June 1990

NASA Technical Reports Server (NTRS)

Smith, James E.

1990-01-01

A description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility is presented and a summary of its observations and data reduction is given. The systems that make up the facility are a magnetograph telescope, an H alpha telescope, a Questar telescope, and a computer code. The data are represented by longitudinal contours with azimuth plots.

NASA Marshall Space Flight Center solar observatory

NASA Technical Reports Server (NTRS)

Smith, James E.

1988-01-01

A description is provided of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and a summary is given of its observations and data reduction during Jan. to Mar. 1988. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer center. The data are represented by longitudinal contours with azimuth plots.

Evolution and advection of solar mesogranulation

NASA Technical Reports Server (NTRS)

Muller, Richard; Auffret, Herve; Roudier, Thierry; Vigneau, Jean; Simon, George W.; Frank, Zoe; Shine, Richard A.; Title, Alan M.

1992-01-01

A three-hour sequence of observations at the Pic du Midi observatory has been obtained which shows the evolution of solar mesogranules from appearance to disappearance with unprecedented clarity. It is seen that the supergranules, which are known to advect the granules with their convective motion, also advect the mesogranules to their boundaries. This process controls the evolution and disappearance of mesogranules.

The Virtual Earth-Solar Observatory of the SCiESMEX

NASA Astrophysics Data System (ADS)

De la Luz, V.; Gonzalez-Esparza, A.; Cifuentes-Nava, G.

2015-12-01

The Mexican Space Weather Service (SCiESMEX, http://www.sciesmex.unam.mx) started operations in October 2014. The project includes the Virtual Earth-Solar Observatory (VESO, http://www.veso.unam.mx). The VESO is a improved project wich objetive is integrate the space weather instrumentation network from the National Autonomous University of Mexico (UNAM). The network includes the Mexican Array Radiotelescope (MEXART), the Callisto receptor (MEXART), a Neutron Telescope, a Cosmic Ray Telescope. the Schumann Antenna, the National Magnetic Service, and the mexican GPS network (TlalocNet). The VESO facility is located at the Geophysics Institute campus Michoacan (UNAM). We offer the service of data store, real-time data, and quasi real-time data. The hardware of VESO includes a High Performance Computer (HPC) dedicated specially to big data storage.

Development of a CCD based solar speckle imaging system

NASA Astrophysics Data System (ADS)

Nisenson, Peter; Stachnik, Robert V.; Noyes, Robert W.

1986-02-01

A program to develop software and hardware for the purpose of obtaining high angular resolution images of the solar surface is described. The program included the procurement of a Charge Coupled Devices imaging system; an extensive laboratory and remote site testing of the camera system; the development of a software package for speckle image reconstruction which was eventually installed and tested at the Sacramento Peak Observatory; and experiments of the CCD system (coupled to an image intensifier) for low light level, narrow spectral band solar imaging.

An equatorial coronal hole at solar minimum

NASA Technical Reports Server (NTRS)

Bromage, B. J. I.; DelZanna, G.; DeForest, C.; Thompson, B.; Clegg, J. R.

1997-01-01

The large transequatorial coronal hole that was observed in the solar corona at the end of August 1996 is presented. It consists of a north polar coronal hole called the 'elephant's trunk or tusk'. The observations of this coronal hole were carried out with the coronal diagnostic spectrometer onboard the Solar and Heliospheric Observatory (SOHO). The magnetic field associated with the equatorial coronal hole is strongly connected to that of the active region at its base, resulting in the two features rotating at almost the same rate.

Earth Science

NASA Image and Video Library

1995-12-02

The Solar Heliospheric Observatory (SOHO) is launched atop an ATLAS-IIAS expendable launch vehicle. Liftoff from launch complex 36B at Cape Canaveral Air Station marked the 10th Atlas launch from the Eastern range for 1995. SOHO is a cooperative effort involving NASA and the European Space Agency (ESA) within the framework of the International Solar-Terrestrial Physics Program. During its 2-year mission, the SOHO spacecraft gathered data on the internal structure of the Sun, its extensive outer atmosphere and the origin of the solar wind.

GPM Solar Array Gravity Negated Deployment Testing

NASA Technical Reports Server (NTRS)

Penn, Jonathan; Johnson, Chris; Lewis, Jesse; Dear, Trevin; Stewart, Alphonso

2014-01-01

NASA Goddard Space Flight Center (GSFC) successfully developed a g-negation support system for use on the solar arrays of the Global Precipitation Measurement (GPM) Satellite. This system provides full deployment capability at the subsystem and observatory levels. In addition, the system provides capability for deployed configuration first mode frequency verification testing. The system consists of air pads, a support structure, an air supply, and support tables. The g-negation support system was used to support all deployment activities for flight solar array deployment testing.

THE RECURRENT INTENSITY VARIATIONS OF PRIMARY COSMIC RADIATION IN PERIODS OF MAXIMUM SOLAR ACTIVITY (in French)

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

Freon, A.; Berry, J.; Coste, J.-P.

1959-02-01

Some recordings of the variations of intensity of cosmic neutrons, made since October 1956 at the observatory of the Pic du Midi and since July 1957 on the Kerguelen Islands, have shown the existence, since the beginning of the observations and during at least 20 solar rotations, of a cyclic variation with a stable period equal to 27.35 plus or minus 0.1 solar days and a maximum amplitude of 2.2% attained in October 1957. (tr-auth)

Churning Prominence

NASA Image and Video Library

2017-01-30

On Jan. 23-24, 2017, NASA Solar Dynamics Observatory watched as a solar prominence rose up along the edge of the sun and twisted and churned for about two days before falling apart. The dynamic action was generated by competing magnetic forces. The images were taken in a wavelength extreme ultraviolet light that observes activity close to the solar surface, perfect for capturing prominences, which are notoriously unstable clouds of plasma suspended above the sun. Movies are available at http://photojournal.jpl.nasa.gov/catalog/PIA11237

How MAG4 Improves Space Weather Forecasting

NASA Technical Reports Server (NTRS)

Falconer, David; Khazanov, Igor; Barghouty, Nasser

2013-01-01

Dangerous space weather is driven by solar flares and Coronal Mass Ejection (CMEs). Forecasting flares and CMEs is the first step to forecasting either dangerous space weather or All Clear. MAG4 (Magnetogram Forecast), developed originally for NASA/SRAG (Space Radiation Analysis Group), is an automated program that analyzes magnetograms from the HMI (Helioseismic and Magnetic Imager) instrument on NASA SDO (Solar Dynamics Observatory), and automatically converts the rate (or probability) of major flares (M- and X-class), Coronal Mass Ejections (CMEs), and Solar Energetic Particle Events.

The solar gamma ray and neutron capabilities of COMPTEL on the Gamma Ray Observatory

NASA Technical Reports Server (NTRS)

Ryan, James M.; Lockwood, John A.

1989-01-01

The imaging Compton telescope COMPTEL on the Gamma Ray Observatory (GRO) has unusual spectroscopic capabilities for measuring solar gamma-ray and neutron emission. The launch of the GRO is scheduled for June 1990 near the peak of the sunspot cycle. With a 30 to 40 percent probability for the Sun being in the COMPTEL field-of-view during the sunlit part of an orbit, a large number of flares will be observed above the 800 keV gamma-ray threshold of the telescope. The telescope energy range extends to 30 MeV with high time resolution burst spectra available from 0.1 to 10 MeV. Strong Compton tail suppression of instrumental gamma-ray interactions will facilitate improved spectral analysis of solar flare emissions. In addition, the high signal to noise ratio for neutron detection and measurement will provide new neutron spectroscopic capabilities. Specifically, a flare similar to that of 3 June 1982 will provide spectroscopic data on greater than 1500 individual neutrons, enough to construct an unambiguous spectrum in the energy range of 20 to 200 MeV. Details of the instrument and its response to solar gamma-rays and neutrons will be presented.

Solar Activity Seen at Sunspot Site Tracked by Mars Rover

NASA Image and Video Library

2015-07-10

An eruption from the surface of the sun is conspicuous in the lower left portion of this July 6, 2015, image from NASA's Earth-orbiting Solar Dynamics Observatory (SDO). It originates from a location on the surface where NASA's Curiosity Mars rover had been tracking a sunspot in late June and early July. This image was taken by the Atmosphere Imaging Assembly on SDO using the instrument's 131-Angstrom wavelength channel, which is sensitive to hot solar flares. The sun completes a rotation about once a month -- faster near its equator than near its poles. This summer, Mars has a view of the opposite side of the sun from what's facing Earth. Images from Curiosity tracking a southern-hemisphere sunspot until it rotated out of view during the July 4 weekend are in an animation at PIA19801. This location on the sun rotated into position to be seen from Earth a few days later. The eruption visible in this image was linked to a coronal mass ejection observed by SDO and NASA's Solar and Heliospheric Observatory. The coronal mass ejection affected interplanetary space weather, as shown at http://go.nasa.gov/1JSXLF3. http://photojournal.jpl.nasa.gov/catalog/PIA19680

Comet ISON Seen Coming and Going

NASA Image and Video Library

2013-11-30

"Timelapse" series of images of comet ISON as viewed by ESA/NASA's Solar and Heliospheric Observatory, or SOHO. This image is a composite, with the sun imaged by NASA's Solar Dynamics Observatory in the center, and SOHO's two coronagraphs showing the solar atmosphere, the corona. The most recent image in this is from 5:30 p.m. EST on Nov. 29, 2013. Continuing a history of surprising behavior, material from Comet ISON appeared on the other side of the sun on the evening on Nov. 28, 2013, despite not having been seen in observations during its closest approach to the sun. The question remains whether it is merely debris from the comet, or if some portion of the comet's nucleus survived, but late-night analysis from scientists with NASA's Comet ISON Observing Campaign suggest that there is at least a small nucleus intact. Image Credit:ESA&NASA/SOHO/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

International Heliophysical Year and Astronomy and Space Science Activities in Arab States: Concentration on United Arab Emirates and Iraq

NASA Astrophysics Data System (ADS)

Al-Naimiy, Hamid M. K.; Al-Douri, Ala A. J.

2008-12-01

This paper summarizes International Heliophysical Year (IHY), astronomy and space sciences (ASS) activities in many Arab countries with the concentration on Iraq and UAE. The level and type of these activities differ in each country. -The paper shows also the current activities on topics related to IHY in different countries, following are suggested future Astronomy and Space Science (ASS) plans in some of these countries: -UAE Research Centre for Solar Physics, Astronomy and Space Sciences: A proposal under consideration for building a Solar Physics and Space Research Centre that may contain: Solar, radio and optical observatories, and Very Low Frequency (VLF) Receiver for remote sensing the Ionosphere on UAE region. The proposed research project will facilitate the establishment and conduct of VLF observations in the United Arab Emirate (UAE) as a part of Asia sector, thus providing a basis for comparison to facilitate global extrapolations and conclusions. -Iraqi National Astronomical Observatory (INAO): The Kurdistan Government/Universities planning to rebuilt INAO which has been destroyed during the two wars. Proposed suggestion is to build a 5-6 meters optical telescope and small solar telescope on the tope of Korek Mountain, which has excellent observing conditions.

Heliophysics: The New Science of the Sun-Solar System Connection. Recommended Roadmap for Science and Technology 2005-2035

NASA Technical Reports Server (NTRS)

2005-01-01

This is a Roadmap to understanding the environment of our Earth, from its life-sustaining Sun out past the frontiers of the solar system. A collection of spacecraft now patrols this space, revealing not a placid star and isolated planets, but an immense, dynamic, interconnected system within which our home planet is embedded and through which space explorers must journey. These spacecraft already form a great observatory with which the Heliophysics program can study the Sun, the heliosphere, the Earth, and other planetary environments as elements of a system--one that contains dynamic space weather and evolves in response to solar, planetary, and interstellar variability. NASA continually evolves the Heliophysics Great Observatory by adding new missions and instruments in order to answer the challenging questions confronting us now and in the future as humans explore the solar system. The three heliophysics science objectives: opening the frontier to space environment prediction; understanding the nature of our home in space, and safeguarding the journey of exploration, require sustained research programs that depend on combining new data, theory, analysis, simulation, and modeling. Our program pursues a deeper understanding of the fundamental physical processes that underlie the exotic phenomena of space.

The EUV-observatory TESIS on board Coronas-Photon: scientific goals and initial plan of observations

NASA Astrophysics Data System (ADS)

Bogachev, Sergey

The TESIS a EUV-observatory for solar research from space will be launched in 2008 September on board the satellite Coronas-Photon from cosmodrome Plesetsk. TESIS is a project of Lebedev Physical Institute of Russian Academy of Science with contribution from Space Research Center of Polish Academy of Science (the spectrometer SphinX). The experiment will focus on quasi-monochromatic imaging of the Sun and XUV spectroscopy of solar plasma. The scientific payload of TESIS contains five instruments: (1) Bragg crystal spectroheliometer for Sun monochromatic imaging in the line MgXII 8.42 A, (2) the normal-incidence Herschelian EUV telescopes with a resolution of 1.7 arc sec operated in lines FeXXII 133 A, FeIX 171 A and HeII 304 A, (3) the EUV imaging spectrometer, (4) the wide-field Ritchey-Chretien coronograph and (5) the X-ray spectrometer SphinX. The TESIS will focus on coordinated study of solar activity from the transition region to the outer corona up to 4 solar radii in wide temperature range from 5*104 to 2*107 K. We describe the scientific goals of the TESIS and its initial plan of observations.

Sweeping Arches and Loops [video

NASA Image and Video Library

2014-07-10

Two active regions with their intense magnetic fields produced towering arches and spiraling coils of solar loops above them (June 29 - July 1, 2014) as they rotated into view. When viewed in extreme ultraviolet light, magnetic field lines are revealed by charged particles that travel along them. These active regions appear as dark sunspots when viewed in filtered light. Note the small blast in the upper of the two major active regions, followed by more coils of loops as the region reorganizes itself. The still was taken on June 30 at 10:33 UT. Credit: NASA/Solar Dynamics Observatory Two active regions with their intense magnetic fields produced towering arches and spiraling coils of solar loops above them (June 29 - July 1, 2014) as they rotated into view. When viewed in extreme ultraviolet light, magnetic field lines are revealed by charged particles that travel along them. These active regions appear as dark sunspots when viewed in filtered light. Note the small blast in the upper of the two major active regions, followed by more coils of loops as the region reorganizes itself. The still was taken on June 30 at 10:33 UT. Credit: Solar Dynamics Observatory/NASA.

Solar Irradiance from 165 to 400 nm in 2008 and UV Variations in Three Spectral Bands During Solar Cycle 24

NASA Astrophysics Data System (ADS)

Meftah, M.; Bolsée, D.; Damé, L.; Hauchecorne, A.; Pereira, N.; Irbah, A.; Bekki, S.; Cessateur, G.; Foujols, T.; Thiéblemont, R.

2016-12-01

Accurate measurements of the solar spectral irradiance (SSI) and its temporal variations are of primary interest to better understand solar mechanisms, and the links between solar variability and Earth's atmosphere and climate. The SOLar SPECtrum (SOLSPEC) instrument of the Solar Monitoring Observatory (SOLAR) payload onboard the International Space Station (ISS) has been built to carry out SSI measurements from 165 to 3088 nm. We focus here on the ultraviolet (UV) part of the measured solar spectrum (wavelengths less than 400 nm) because the UV part is potentially important for understanding the solar forcing of Earth's atmosphere and climate. We present here SOLAR/SOLSPEC UV data obtained since 2008, and their variations in three spectral bands during Solar Cycle 24. They are compared with previously reported UV measurements and model reconstructions, and differences are discussed.

SUMER observations detecting downward propagating waves in the solar transition region

NASA Technical Reports Server (NTRS)

Wikstol, O.; Judge, P. G.; Hansteen, V.; Wilhelm, K.; Schuehle, U.; Moran, T.

1997-01-01

The O IV density sensitive emission lines around 1400 A, using the solar ultraviolet measurement of emitted radiation (SUMER) instrument onboard the Solar and Heliospheric Observatory (SOHO), are reported on. The data for the quiet sun, obtained close to the disk center and the solar limb were acquired. A systematic correlation between a density sensitive emission line ratio and Doppler shift across the same emission profiles was obtained. The correlation is such that the density is higher in the downflowing than in the upflowing plasma. The results are in good agreement with the simulations of downward propagating waves.

Calibration of the Multi-Spectral Solar Telescope Array multilayer mirrors and XUV filters

NASA Technical Reports Server (NTRS)

Allen, Maxwell J.; Willis, Thomas D.; Kankelborg, Charles C.; O'Neal, Ray H.; Martinez-Galarce, Dennis S.; Deforest, Craig E.; Jackson, Lisa; Lindblom, Joakim; Walker, Arthur B. C., Jr.; Barbee, Troy W., Jr.

1993-01-01

The Multi-Spectral Solar Telescope Array (MSSTA), a rocket-borne solar observatory, was successfully flown in May, 1991, obtaining solar images in eight XUV and FUV bands with 12 compact multilayer telescopes. Extensive measurements have recently been carried out on the multilayer telescopes and thin film filters at the Stanford Synchrotron Radiation Laboratory. These measurements are the first high spectral resolution calibrations of the MSSTA instruments. Previous measurements and/or calculations of telescope throughputs have been confirmed with greater accuracy. Results are presented on Mo/Si multilayer bandpass changes with time and experimental potassium bromide and tellurium filters.

Astronomy in Denver: Centenary of the 1918 total solar eclipse across Denver

NASA Astrophysics Data System (ADS)

Stencel, Robert E.

2018-06-01

Totality during the 2017 August 21 solar eclipse (Saros 145) traveled along a path across the United States similar to that which occurred for the eclipse on 1918 June 8 (Saros 126), but with a less west-northerly track. This placed Denver and its then new Chamberlin Observatory in the path of totality. Denver University astronomy Professor Herbert Howe offered use of the Chamberlin Observatory 20-inch f/15 refractor, with its Clark doublet lens and Saegmueller mounting, in service of eclipse-related research. In preparation for the eclipse, Professor Howe and assistants had spent the last three months of 1917, refurbishing mechanical aspects of the telescope. Edwin Frost, then Director of Yerkes Observatory expressed interest and made a reconnaissance visit to the area in September 1917, reporting results in the Feb. 1918 issue of Popular Astronomy ( http://adsabs.harvard.edu/abs/1918PA.....26R.103F ). Frank Schlesinger, then director of Allegheny Observatory, asked if he might attach a special camera for star photography to the telescope at the eclipse, to test displacement of stars, in order to test a prediction of relativity theory. Among the additional visiting astronomical luminaries present on that June day in 1918 were Annie J. Cannon (Harvard), John Duncan (Wellesley), Herbert R. Morgan (U.S. Naval Observatory) and Robert Trumpler (Berkeley). To learn the results of all this eclipse preparedness, you will need to attend my talk in order to get “the rest of the story” or visit our twitter feed at: https://twitter.com/Chamberlin_Obs .

Ground System for Solar Dynamics Observatory (SDO) Mission

NASA Technical Reports Server (NTRS)

Tann, Hun K.; Silva, Christopher J.; Pages, Raymond J.

2005-01-01

NASA s Goddard Space Flight Center (GSFC) has recently completed its Critical Design Review (CDR) of a new dual Ka and S-band ground system for the Solar Dynamics Observatory (SDO) Mission. SDO, the flagship mission under the new Living with a Star Program Office, is one of GSFC s most recent large-scale in-house missions. The observatory is scheduled for launch in August 2008 from the Kennedy Space Center aboard an Atlas-5 expendable launch vehicle. Unique to this mission is an extremely challenging science data capture requirement. The mission is required to capture 99.99% of available science over 95% of all observation opportunities. Due to the continuous, high volume (150 Mbps) science data rate, no on-board storage of science data will be implemented on this mission. With the observatory placed in a geo-synchronous orbit at 36,000 kilometers within view of dedicated ground stations, the ground system will in effect implement a "real-time" science data pipeline with appropriate data accounting, data storage, data distribution, data recovery, and automated system failure detection and correction to keep the science data flowing continuously to three separate Science Operations Centers (SOCs). Data storage rates of approx. 45 Tera-bytes per month are expected. The Mission Operations Center (MOC) will be based at GSFC and is designed to be highly automated. Three SOCs will share in the observatory operations, each operating their own instrument. Remote operations of a multi-antenna ground station in White Sands, New Mexico from the MOC is part of the design baseline.

McDonald Observatory Planetary Search - A high precision stellar radial velocity survey for other planetary systems

NASA Technical Reports Server (NTRS)

Cochran, William D.; Hatzes, Artie P.

1993-01-01

The McDonald Observatory Planetary Search program surveyed a sample of 33 nearby F, G, and K stars since September 1987 to search for substellar companion objects. Measurements of stellar radial velocity variations to a precision of better than 10 m/s were performed as routine observations to detect Jovian planets in orbit around solar type stars. Results confirm the detection of a companion object to HD114762.

Shuttle and Transfer Orbit Thermal Analysis and Testing of the Chandra X-Ray Observatory Charge-Couple Device Imaging Spectrometer Radiator Shades

NASA Technical Reports Server (NTRS)

Sharp, John R.

1999-01-01

Thermal analyses of the Shuttle and Transfer Orbit of the Advanced X-Ray Astrophysics Facility Charge-Coupled Device (CCD) Imaging Spectrometer (ACIS), one of two science instruments on the Chandra X-Ray Observatory, revealed a low-earth orbit (LEO) overheating problem on the goldized Kapton faces of two radiator shades. The shades were coated with the goldized Kapton to provide a low hemispherical emittance to minimize direct and backloaded heating from the sun and the observatory and high specularity to optimize the coupling to space on two passive radiators which cool the focal plane to -120 C +/- 1 C during on-orbit operations. Since the observatory has a highly elliptical final orbit of 10,000 kilometers by 140,000 kilometers and the ACIS radiators and shades are oriented anti-sun, the high solar absorptance to emittance ratio of the goldized Kapton was not an issue. However, during Shuttle bay-to-earth operations, the short duration solar heating occurring near the eclipse entry and exit resulted in shade temperatures in excess of the cure temperature of the adhesive used to bond the goldized Kapton and honeycomb face-sheets. The detailed thermal analysis demonstrating the LEO overheating as well as the redesign options and thermal testing of a redesigned development unit shade are presented.

The Greenwich Photo-heliographic Results (1874 - 1976): Initial Corrections to the Printed Publications

NASA Astrophysics Data System (ADS)

Erwin, E. H.; Coffey, H. E.; Denig, W. F.; Willis, D. M.; Henwood, R.; Wild, M. N.

2013-11-01

A new sunspot and faculae digital dataset for the interval 1874 - 1955 has been prepared under the auspices of the NOAA National Geophysical Data Center (NGDC). This digital dataset contains measurements of the positions and areas of both sunspots and faculae published initially by the Royal Observatory, Greenwich, and subsequently by the Royal Greenwich Observatory (RGO), under the title Greenwich Photo-heliographic Results ( GPR) , 1874 - 1976. Quality control (QC) procedures based on logical consistency have been used to identify the more obvious errors in the RGO publications. Typical examples of identifiable errors are North versus South errors in specifying heliographic latitude, errors in specifying heliographic (Carrington) longitude, errors in the dates and times, errors in sunspot group numbers, arithmetic errors in the summation process, and the occasional omission of solar ephemerides. Although the number of errors in the RGO publications is remarkably small, an initial table of necessary corrections is provided for the interval 1874 - 1917. Moreover, as noted in the preceding companion papers, the existence of two independently prepared digital datasets, which both contain information on sunspot positions and areas, makes it possible to outline a preliminary strategy for the development of an even more accurate digital dataset. Further work is in progress to generate an extremely reliable sunspot digital dataset, based on the long programme of solar observations supported first by the Royal Observatory, Greenwich, and then by the Royal Greenwich Observatory.

Use of Statistical Estimators as Virtual Observatory Search ParametersEnabling Access to Solar and Planetary Resources through the Virtual Observatory

NASA Astrophysics Data System (ADS)

Merka, J.; Dolan, C. F.

2015-12-01

Finding and retrieving space physics data is often a complicated taskeven for publicly available data sets: Thousands of relativelysmall and many large data sets are stored in various formats and, inthe better case, accompanied by at least some documentation. VirtualHeliospheric and Magnetospheric Observatories (VHO and VMO) help researches by creating a single point of uniformdiscovery, access, and use of heliospheric (VHO) and magnetospheric(VMO) data.The VMO and VHO functionality relies on metadata expressed using theSPASE data model. This data model is developed by the SPASE WorkingGroup which is currently the only international group supporting globaldata management for Solar and Space Physics. The two Virtual Observatories(VxOs) have initiated and lead a development of a SPASE-related standardnamed SPASE Query Language for provided a standard way of submittingqueries and receiving results.The VMO and VHO use SPASE and SPASEQL for searches based on various criteria such as, for example, spatial location, time of observation, measurement type, parameter values, etc. The parameter values are represented by their statisticalestimators calculated typically over 10-minute intervals: mean, median, standard deviation, minimum, and maximum. The use of statistical estimatorsenables science driven data queries that simplify and shorten the effort tofind where and/or how often the sought phenomenon is observed, as we will present.

The French Jesuit Mission to Thailand in the 1680s and the Establishment of a Major Astronomical Observatory

NASA Astrophysics Data System (ADS)

Soonthornthum, Boonrucksar; Orchiston, Wayne; Komonjinda, Siramas

2012-09-01

The first great Thai ruler to encourage the adoption of Western culture and technology was King Narai, and his enlightened attitude led to the rapid development of Thailand. King Narai also had a passion for astronomy, and he pursued this interest by allowing French Jesuit missionaries to set up a large modern well-equipped astronomical observatory in Lopburi Province between AD 1685 and 1687. This was known as the Wat San Paolo Observatory, and King Narai and the missionaries observed a total lunar eclipse on 10 December 1685 and a partial solar eclipse on 30 April 1688. These observations and others made at Wat San Paolo Observatory during the 1680s marked the start of modern scientific astronomy in Thailand. In this paper we discuss King Narai's scientific and other interests, the founding of the Wat San Paolo Observatory, the missionaries who conducted the astronomical programs, their instruments and their observations. We also describe the surviving ruins of the Observatory and their interpretation as a site of national scientific importance in Thailand.

The High Energy Astronomy Observatory X-ray Telescope

NASA Technical Reports Server (NTRS)

Miller, R.; Austin, G.; Koch, D.; Jagoda, N.; Kirchner, T.; Dias, R.

1978-01-01

The High Energy Astronomy Observatory-Mission B (HEAO-B) is a satellite observatory for the purpose of performing a detailed X-ray survey of the celestial sphere. Measurements will be made of stellar radiation in the range 0.2 through 20 keV. The primary viewing requirement is to provide final aspect solution and internal alignment information to correlate an observed X-ray image with the celestial sphere to within one-and-one-half arc seconds. The Observatory consists of the HEAO Spacecraft together with the X-ray Telescope. The Spacecraft provides the required attitude control and determination system, data telemetry system, space solar power system, and interface with the launch vehicle. The X-ray Telescope includes a high resolution mirror assembly, optical bench metering structure, X-ray detectors, detector positioning system, detector electronics and aspect sensing system.

The detection of upwardly propagating waves channeling energy from the chromosphere to the low corona

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

Freij, N.; Nelson, C. J.; Mumford, S.

There have been ubiquitous observations of wave-like motions in the solar atmosphere for decades. Recent improvements to space- and ground-based observatories have allowed the focus to shift to smaller magnetic structures on the solar surface. In this paper, high-resolution ground-based data taken using the Swedish 1 m Solar Telescope is combined with co-spatial and co-temporal data from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) satellite to analyze running penumbral waves (RPWs). RPWs have always been thought to be radial wave propagation that occurs within sunspots. Recent research has suggested that they are in fact upwardlymore » propagating field-aligned waves (UPWs). Here, RPWs within a solar pore are observed for the first time and are interpreted as UPWs due to the lack of a penumbra that is required to support RPWs. These UPWs are also observed co-spatially and co-temporally within several SDO/AIA elemental lines that sample the transition region and low corona. The observed UPWs are traveling at a horizontal velocity of around 17 ± 0.5 km s{sup –1} and a minimum vertical velocity of 42 ± 21 km s{sup –1}. The estimated energy of the waves is around 150 W m{sup –2}, which is on the lower bound required to heat the quiet-Sun corona. This is a new, yet unconsidered source of wave energy within the solar chromosphere and low corona.« less

Demonstrating the Error Budget for the Climate Absolute Radiance and Refractivity Observatory Through Solar Irradiance Measurements

NASA Technical Reports Server (NTRS)

Thome, Kurtis; McCorkel, Joel; McAndrew, Brendan

2016-01-01

The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission addresses the need to observe highaccuracy, long-term climate change trends and to use decadal change observations as a method to determine the accuracy of climate change. A CLARREO objective is to improve the accuracy of SI-traceable, absolute calibration at infrared and reflected solar wavelengths to reach on-orbit accuracies required to allow climate change observations to survive data gaps and observe climate change at the limit of natural variability. Such an effort will also demonstrate National Institute of Standards and Technology (NIST) approaches for use in future spaceborne instruments. The current work describes the results of laboratory and field measurements with the Solar, Lunar for Absolute Reflectance Imaging Spectroradiometer (SOLARIS) which is the calibration demonstration system (CDS) for the reflected solar portion of CLARREO. SOLARIS allows testing and evaluation of calibration approaches, alternate design and/or implementation approaches and components for the CLARREO mission. SOLARIS also provides a test-bed for detector technologies, non-linearity determination and uncertainties, and application of future technology developments and suggested spacecraft instrument design modifications. Results of laboratory calibration measurements are provided to demonstrate key assumptions about instrument behavior that are needed to achieve CLARREO's climate measurement requirements. Absolute radiometric response is determined using laser-based calibration sources and applied to direct solar views for comparison with accepted solar irradiance models to demonstrate accuracy values giving confidence in the error budget for the CLARREO reflectance retrieval.

A global SOLIS vector spectromagnetograph (VSM) network

NASA Astrophysics Data System (ADS)

Streander, K. V.; Giampapa, M. S.; Harvey, J. W.; Henney, C. J.; Norton, A. A.

2008-07-01

Understanding the Sun's magnetic field related activity is far from complete as reflected in the limited ability to make accurate predictions of solar variability. To advance our understanding of solar magnetism, the National Solar Observatory (NSO) constructed the Synoptic Optical Long-term Investigations of the Sun (SOLIS) suite of instruments to conduct high precision optical measurements of processes on the Sun whose study requires sustained observations over long time periods. The Vector Spectromagnetograph (VSM), the principal SOLIS instrument, has been in operation since 2003 and obtains photospheric vector data, as well as photospheric and chromospheric longitudinal magnetic field measurements. Instrument performance is being enhanced by employing new, high-speed cameras that virtually freeze seeing, thus improving sensitivity to measure the solar magnetic field configuration. A major operational goal is to provide real-time and near-real-time data for forecasting space weather and increase scientific yield from shorter duration solar space missions and ground-based research projects. The National Solar Observatory proposes to build two near-duplicates of the VSM instrument and place them at international sites to form a three-site global VSM network. Current electronic industry practice of short lifetime cycles leads to improved performance and reduced acquisition costs but also to redesign costs and engineering impacts that must be minimized. The current VSM instrument status and experience gained from working on the original instrument is presented herein and used to demonstrate that one can dramatically reduce the estimated cost and fabrication time required to duplicate and commission two additional instruments.

Observation of the Kelvin–Helmholtz Instability in a Solar Prominence

NASA Astrophysics Data System (ADS)

Yang, Heesu; Xu, Zhi; Lim, Eun-Kyung; Kim, Sujin; Cho, Kyung-Suk; Kim, Yeon-Han; Chae, Jongchul; Cho, Kyuhyoun; Ji, Kaifan

2018-04-01

Many solar prominences end their lives in eruptions or abrupt disappearances that are associated with dynamical or thermal instabilities. Such instabilities are important because they may be responsible for energy transport and conversion. We present a clear observation of a streaming kink-mode Kelvin–Helmholtz Instability (KHI) taking place in a solar prominence using the Hα Lyot filter installed at the New Vacuum Solar Telescope, Fuxian-lake Solar Observatory in Yunnan, China. On one side of the prominence, a series of plasma blobs floated up from the chromosphere and streamed parallel to the limb. The plasma stream was accelerated to about 20–60 km s‑1 and then undulated. We found that 2″- and 5″-size vortices formed, floated along the stream, and then broke up. After the 5″-size vortex, a plasma ejection out of the stream was detected in the Solar Dynamics Observatory/Atmospheric Imaging Assembly images. Just before the formation of the 5″-size vortex, the stream displayed an oscillatory transverse motion with a period of 255 s with the amplitude growing at the rate of 0.001 s‑1. We attribute this oscillation of the stream and the subsequent formation of the vortex to the KHI triggered by velocity shear between the stream, guided by the magnetic field and the surrounding media. The plasma ejection suggests the transport of prominence material into the upper layer by the KHI in its nonlinear stage.

X-class Solar Flare on March 29, 2014

NASA Image and Video Library

2014-03-31

Extreme ultraviolet light streams out of an X-class solar flare as seen in this image captured on March 29, 2014, by NASA's Solar Dynamics Observatory. This image blends two wavelengths of light: 304 and 171 Angstroms, which help scientists observe the lower levels of the sun's atmosphere. More info: The sun emitted a significant solar flare, peaking at 1:48 p.m. EDT March 29, 2014, and NASA's Solar Dynamics Observatory captured images of the event. Solar flares are powerful bursts of radiation. Harmful radiation from a flare cannot pass through Earth's atmosphere to physically affect humans on the ground, however -- when intense enough -- they can disturb the atmosphere in the layer where GPS and communications signals travel. To see how this event impacted Earth, please visit NOAA's Space Weather Prediction Center at spaceweather.gov, the U.S. government's official source for space weather forecasts, alerts, watches and warnings. This flare is classified as an X.1-class flare. X-class denotes the most intense flares, while the number provides more information about its strength. An X2 is twice as intense as an X1, an X3 is three times as intense, etc. Credit: NASA/SDO NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Flux Cancelation: The Key to Solar Eruptions

NASA Technical Reports Server (NTRS)

Panesar, Navdeep K.; Sterling, Alphonse; Moore, Ronald; Chakrapani, Prithi; Innes, Davina; Schmit, Don; Tiwari, Sanjiv

2017-01-01

Solar coronal jets are magnetically channeled eruptions that occur in all types of solar environments (e.g. active regions, quiet-Sun regions and coronal holes). Recent studies show that coronal jets are driven by the eruption of small-scare filaments (minifilaments). Once the eruption is underway magnetic reconnection evidently makes the jet spire and the bright emission in the jet base. However, the triggering mechanism of these eruptions and the formation mechanism of the pre-jet minifilaments are still open questions. In this talk, mainly using SDO/AIA (Solar Dynamics Observatory / Atmospheric Imaging Assembly) and SDO/HIM (Solar Dynamics Observatory / Helioseismic and Magnetic Imager) data, first I will address the question: what triggers the jet-driving minifilament eruptions in different solar environments (coronal holes, quiet regions, active regions)? Then I will talk about the magnetic field evolution that produces the pre-jet minifilaments. By examining pre-jet evolutionary changes in line-of-sight HMI magnetograms while examining concurrent EUV (Extreme Ultra-Violet) images of coronal and transition-region emission, we find clear evidence that flux cancelation is the main process that builds pre-jet minifilaments, and is also the main process that triggers the eruptions. I will also present results from our ongoing work indicating that jet-driving minifilament eruptions are analogous to larger-scare filament eruptions that make flares and CMEs (Coronal Mass Ejections). We find that persistent flux cancellation at the neutral line of large-scale filaments often triggers their eruptions. From our observations we infer that flux cancelation is the fundamental process from the buildup and triggering of solar eruptions of all sizes.

Measurement of Solar Neutrons on 05 March 2012, Using a Fiber-Type Neutron Monitor Onboard the Attached Payload to the ISS

NASA Astrophysics Data System (ADS)

Koga, K.; Muraki, Y.; Masuda, S.; Shibata, S.; Matsumoto, H.; Kawano, H.

2017-08-01

The solar neutron detector Space Environment Data Acquisition Equipment - Attached Payload (SEDA-FIB) onboard the International Space Station (ISS) detected several events from the solar direction associated with three large solar flares observed on 05 (X1.1), 07 (X5.4), and 09 (M6.3) March 2012. In this study, we focus on the interesting event of 05 March, present the temporal profiles of the neutrons, and discuss the physics that may be related to a possible acceleration scenario for ions above the solar surface. We compare our data with images of the flares obtained by the ultraviolet telescope Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO).

Millimeter and hard x ray/gamma ray observations of solar flares during the June 1991 GRO campaign

NASA Technical Reports Server (NTRS)

Kundu, M. R.; White, S. M.; Gopalswamy, N.; Lim, J.

1992-01-01

We have carried out high-spatial-resolution millimeter observations of solar flares using the Berkeley-Illinois-Maryland Array (BIMA). At the present time, BIMA consists of only three elements, which is not adequate for mapping highly variable solar phenomena, but is excellent for studies of the temporal structure of flares at millimeter wavelengths at several different spatial scales. We present BIMA observations made during the Gamma Ray Observatories (GRO)/Solar Max 1991 campaign in Jun. 1991 when solar activity was unusually high. Our observations covered the period 8-9 Jun. 1991; this period overlapped the period 4-15 Jun. when the Compton Telescope made the Sun a target of opportunity because of the high level of solar activity.

Modeling solar wind with boundary conditions from interplanetary scintillations

DOE PAGES

Manoharan, P.; Kim, T.; Pogorelov, N. V.; ...

2015-09-30

Interplanetary scintillations make it possible to create three-dimensional, time- dependent distributions of the solar wind velocity. Combined with the magnetic field observations in the solar photosphere, they help perform solar wind simulations in a genuinely time-dependent way. Interplanetary scintillation measurements from the Ooty Radio Astronomical Observatory in India provide directions to multiple stars and may assure better resolution of transient processes in the solar wind. In this paper, we present velocity distributions derived from Ooty observations and compare them with those obtained with the Wang-Sheeley-Arge (WSA) model. We also present our simulations of the solar wind flow from 0.1 AUmore » to 1 AU with the boundary conditions based on both Ooty and WSA data.« less

Correlation of total, diffuse, and direct solar radiation

NASA Technical Reports Server (NTRS)

Buyco, E. H.; Namkoong, D.

1977-01-01

Present requirements for realistic solar energy system evaluations necessitate a comprehensive body of solar-radition data. The data should include both diffuse and direct solar radiation as well as their total on an hourly (or shorter) basis. In general, however, only the total solar radiation values were recorded. This report presents a correlation that relates the diffuse component of an hourly total solar radiation value to the total radiation ratio of the maximum value attainable. The data used were taken at the Blue Hill Observatory in Milton, Massachusetts, for the period 1952. The relation - in the form of the data plots - can be used in situations in which only the hourly total radiation data are available but the diffuse component is desired.

Elongated Coronal Hole

NASA Image and Video Library

2016-03-24

NASA Solar Dynamics Observatory shows a long coronal hole has rotated so that was temporarily facing right towards Earth Mar. 23-25, 2016. Coronal holes appear dark when viewed in some wavelengths of extreme ultraviolet light.

Tenth Planet Discovered

NASA Image and Video Library

2005-08-03

These time-lapse images of a newfound dwarf planet in our solar system, formerly known as 2003 UB313 or Xena, and now called Eris, were taken using the Samuel Oschin Telescope at the Palomar Observatory.

STEREO Press Briefing

NASA Image and Video Library

2011-08-17

David Webb, a research physicist from the Institute for Scientific Research at Boston College speaks during a press briefing, Thursday, Aug. 18, 2011, at NASA Headquarters in Washington. The briefing was held to discuss new details about the structure of solar storms and the impact they have on Earth. The new information comes from NASA's Solar Terrestrial Relations Observatory, or STEREO, spacecraft and other NASA probes. Photo Credit: (NASA/GSFC/Rebecca Roth)

Multi-Satellite Attitude Prediction program/Orbiting Solar Observatory-8 (MSAP/OSO-8) operating guide

NASA Technical Reports Server (NTRS)

Tate, V. H.; Wyckoff, D. C.; Decicco, J. M.

1976-01-01

The sun's lower corona and chromosphere and their interaction in the X-ray and ultraviolet (UV) spectral regions were investigated to better understand the transport of energy from the photosphere to the corona. The interaction between the solar electromagnetic and particle radiation and the earth's environment was studied and the background component of cosmic X-rays was discussed.

NASA Marshall Space Flight Center Solar Observatory report, October - December 1990

NASA Technical Reports Server (NTRS)

Smith, James E.

1991-01-01

A description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility is provided, and a summary of its observations and data reduction during Oct. - Dec. 1990 is presented. The systems that make up the facility are a magnetograph telescope, and H-alpha telescope, a Questar telescope, and a computer code. The data are represented by longitudinal contours with azimuth plots.

NASA Marshall Space Flight Center solar observatory report, January - December 1987

NASA Technical Reports Server (NTRS)

Smith, James E.

1989-01-01

This report provides a description of the NASA Marshall Space Flight Center's Solar Vector Magnetograph Facility and gives a summary of its observations and data reduction during January to December 1987. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code. The data are represented by longitudinal contours with azimuth plots.

NASA Marshall Space Flight Center Solar Observatory report, July - September 1990

NASA Technical Reports Server (NTRS)

Smith, James E.

1991-01-01

A description of the NASA Marshall Space Flight C nter's Solar Vector Magnetograph Facility is provided and gives a summary of its observations and data reduction during Jul. - Sep. 1990. The systems that make up the facility are a magnetograph telescope, an H-alpha telescope, a Questar telescope, and a computer code. The data are represented by longitudinal contours with azimuth plots.

NASA Marshall Space Flight Center solar observatory report, January to December 1989

NASA Technical Reports Server (NTRS)

Smith, James E.

1990-01-01

A description is provided of the NASA-Marshall's Solar Vector Magnetograph Facility and a summary of its observations and data reduction during January to December 1989 is given. The systems that make up the facility are a magnetograph telescope, and H-alpha telescope, a Questar telescope, and a computer code. The data are represented by longitudinal contours with azimuth plots.

Radar Studies in the Solar System

NASA Technical Reports Server (NTRS)

Shapiro, Irwin I.

1996-01-01

We aid in a study of the solar system by means of ground-based radar. We have concentrated on (1) developing the ephemerides needed to acquire radar data at Arecibo Observatory and (2) analyzing the resultant data to: test fundamental laws of gravitation; determine the size, shape, topography, and spin vectors of the targets; and study the surface properties of these objects, through their scattering law and polarization characteristics.

Multi-Spectral Solar Telescope Array. II - Soft X-ray/EUV reflectivity of the multilayer mirrors

NASA Technical Reports Server (NTRS)

Barbee, Troy W., Jr.; Weed, J. W.; Hoover, Richard B.; Allen, Maxwell J.; Lindblom, Joakim F.; O'Neal, Ray H.; Kankelborg, Charles C.; Deforest, Craig E.; Paris, Elizabeth S.; Walker, Arthur B. C., Jr.

1991-01-01

The Multispectral Solar Telescope Array is a rocket-borne observatory which encompasses seven compact soft X-ray/EUV, multilayer-coated, and two compact far-UV, interference film-coated, Cassegrain and Ritchey-Chretien telescopes. Extensive measurements are presented on the efficiency and spectral bandpass of the X-ray/EUV telescopes. Attention is given to systematic errors and measurement errors.

The Multi-Spectral Solar Telescope Array. II - Soft X-ray/EUV reflectivity of the multilayer mirrors

NASA Technical Reports Server (NTRS)

Barbee, Troy W., Jr.; Weed, J. W.; Hoover, Richard B. C., Jr.; Allen, Max J.; Lindblom, Joakim F.; O'Neal, Ray H.; Kankelborg, Charles C.; Deforest, Craig E.; Paris, Elizabeth S.; Walker, Arthur B. C.

1992-01-01

We have developed seven compact soft X-ray/EUV (XUV) multilayer coated and two compact FUV interference film coated Cassegrain and Ritchey-Chretien telescopes for a rocket borne observatory, the Multi-Spectral Solar Telescope Array. We report here on extensive measurements of the efficiency and spectral bandpass of the XUV telescopes carried out at the Stanford Synchrotron Radiation Laboratory.

STEREO Press Briefing

NASA Image and Video Library

2011-08-17

Craig DeForest, a staff scientist at the Southwest Research Institute in Boulder, Colo., speaks during a press briefing, Thursday, Aug. 18, 2011, at NASA Headquarters in Washington. The briefing was held to discusses new details about the structure of solar storms and the impact they have on Earth. The new information comes from NASA's Solar Terrestrial Relations Observatory, or STEREO, spacecraft and other NASA probes. Photo Credit: (NASA/GSFC/Rebecca Roth)

The Solar Connections Observatory for Planetary Environments (SCOPE):

NASA Astrophysics Data System (ADS)

Oliversen, R.; Harris, W.; Ballester, G.; Bougher, S.; Broadfoot, L.; Combi, M.; Cravens, T.; Gombosi, T.; Herbert, F.; Joseph, C.; Kozyra, J.; Limaye, S.; Morgenthaler, J.; Paxton, L.; Roesler, F.; Sandel, W.; Ben Jaffel, L.

2001-12-01

The NASA Sun-Earth Connection theme roadmap calls for comparative study of how the planets and local interstellar medium (LISM) interact with and respond to changes in the solar wind and UV radiation field. Each planet interaction is unique and defined by solar input and local conditions of magnetic field strength and orientation, rotation rate, heliocentric distance, internal plasma, and ionospheric conductivity and circulation. Because the different elements of the environment respond to external and internal influences that are variable on many temporal and spatial scales, the study of a planetary system requires simultaneous understanding of the solar wind and diagnostics of the sun-planet interaction including auroral intensity and variation, upper atmospheric circulation and composition, and the distribution of neutrals and plasmas near the planet. The Solar Connections Observatory for Planetary Environments (SCOPE) is a mission to study Solar interactions from the level of planetary upper atmospheres to the heliopause. SCOPE consists of a binocular EUV/FUV telescope that provides high spatial resolution imaging, broadband spectro-imaging, and high-resolution H Ly-alpha line spectroscopy between 55-290 nm. SCOPE will study planetary environments as examples of the solar connection and map the distribution of interplanetary H and the interaction of LISM plasma with the solar wind at the heliopause. A key to the SCOPE approach is to include Earth in its research objectives. SCOPE will monitor terrestrial auroral energy deposition and leverage local measurements of the solar wind and propagation models to derive the expected conditions at Superior planets that will be observed in annual opposition campaigns. This will permit direct comparison of planetary and terrestrial responses to the same solar wind stream. Using a combination of observations and MHD models, SCOPE will isolate the different controlling parameters in each planet system and gain insight into the underlying physical processes that define the solar connection.

Global Magnetohydrodynamic Modeling of the Solar Corona

NASA Technical Reports Server (NTRS)

Linker, Jon A.

1998-01-01

The coronal magnetic field defines the structure of the solar corona, the position of the heliospheric current sheet, the regions of fast and slow solar wind, and the most likely sites of coronal mass ejections. There are few measurements of the magnetic fields in the corona, but the line-of-sight component of the global magnetic fields in the photosphere have been routinely measured for many years (for example, at Stanford's Wilcox Solar Observatory, and at the National Solar Observatory at Kitt Peak). The SOI/MDI instrument is now providing high-resolution full-disk magnetograms several times a day. Understanding the large-scale structure of the solar corona and inner heliosphere requires accurately mapping the measured photospheric magnetic field into the corona and outward. Ideally, a model should not only extrapolate the magnetic field, but should self-consistently reconstruct both the plasma and magnetic fields in the corona and solar wind. Support from our NASA SR&T contract has allowed us to develop three-dimensional magnetohydrodynamic (MHD) computations of the solar corona that incorporate observed photospheric magnetic fields into the boundary conditions. These calculations not only describe the magnetic field in the corona and interplanetary spice, but also predict the plasma properties as well. Our computations thus far have been successful in reproducing many aspects of both coronal and interplanetary data, including the structure of the streamer belt, the location of coronal hole boundaries, and the position and shape of the heliospheric current sheet. The most widely used technique for extrapolating the photospheric magnetic field into the corona and heliosphere are potential field models, such as the potential field source-surface model (PFSS),and the potential field current-sheet (PFCS) model

Tracking Waves from Sunspots Gives New Solar Insight

NASA Image and Video Library

2017-12-08

While it often seems unvarying from our viewpoint on Earth, the sun is constantly changing. Material courses through not only the star itself, but throughout its expansive atmosphere. Understanding the dance of this charged gas is a key part of better understanding our sun – how it heats up its atmosphere, how it creates a steady flow of solar wind streaming outward in all directions, and how magnetic fields twist and turn to create regions that can explode in giant eruptions. Now, for the first time, researchers have tracked a particular kind of solar wave as it swept upward from the sun's surface through its atmosphere, adding to our understanding of how solar material travels throughout the sun. Scientists analyzed sunspot images from a trio of observatories -- including the Big Bear Solar Observatory, which captured this footage -- to make the first-ever observations of a solar wave traveling up into the sun’s atmosphere from a sunspot. Tracking solar waves like this provides a novel tool for scientists to study the atmosphere of the sun. The imagery of the journey also confirms existing ideas, helping to nail down the existence of a mechanism that moves energy – and therefore heat – into the sun’s mysteriously-hot upper atmosphere, called the corona. A study on these results was published Oct. 11, 2016, in The Astrophysical Journal Letters. Image credit: Zhao et al/NASA/SDO/IRIS/BBSO Read more: go.nasa.gov/2dRv80g NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

Solar Terrestrial Relations Observatory (STEREO)

NASA Technical Reports Server (NTRS)

Davila, Joseph M.; SaintCyr, O. C.

2003-01-01

The solar magnetic field is constantly generated beneath the surface of the Sun by the solar dynamo. To balance this flux generation, there is constant dissipation of magnetic flux at and above the solar surface. The largest phenomenon associated with this dissipation is the Coronal Mass Ejection (CME). The Solar and Heliospheric Observatory (SOHO) has provided remarkable views of the corona and CMEs, and served to highlight how these large interplanetary disturbances can have terrestrial consequences. STEREO is the next logical step to study the physics of CME origin, propagation, and terrestrial effects. Two spacecraft with identical instrument complements will be launched on a single launch vehicle in November 2007. One spacecraft will drift ahead and the second behind the Earth at a separation rate of 22 degrees per year. Observation from these two vantage points will for the first time allow the observation of the three-dimensional structure of CMEs and the coronal structures where they originate. Each STEREO spacecraft carries a complement of 10 instruments, which include (for the first time) an extensive set of both remote sensing and in-situ instruments. The remote sensing suite is capable of imaging CMEs from the solar surface out to beyond Earth's orbit (1 AU), and in-situ instruments are able to measure distribution functions for electrons, protons, and ions over a broad energy range, from the normal thermal solar wind plasma to the most energetic solar particles. It is anticipated that these studies will ultimately lead to an increased understanding of the CME process and provide unique observations of the flow of energy from the corona to the near-Earth environment. An international research program, the International Heliophysical Year (IHY) will provide a framework for interpreting STEREO data in the context of global processes in the Sun-Earth system.

Early Science Results from SOFIA, the Worlds Largest Airborne Observatory

NASA Astrophysics Data System (ADS)

De Buizer, J.

2012-09-01

The Stratospheric Observatory for Infrared Astronomy, or SOFIA, is the largest flying observatory ever built, consisting of a 2.7-meter diameter telescope embedded in a modified Boeing 747-SP aircraft. SOFIA is a joint project between NASA and the German Aerospace Center Deutsches Zentrum fur Luft und-Raumfahrt. By flying at altitudes up to 45000 feet, the observatory gets above 99.9% of the infrared-absorbing water vapor in the Earth's atmosphere. This opens up an almost uninterrupted wavelength range from 0.3-1600 microns that is in large part obscured from ground based observatories. Since its 'Initial Science Flight' in December 2010, SOFIA has flown several dozen science flights, and has observed a wide array of objects from Solar System bodies, to stellar nurseries, to distant galaxies. This talk will review some of the exciting new science results from these first flights which were made by three instruments: the mid-infrared camera FORCAST, the far-infrared heterodyne spectrometer GREAT, and the optical occultation photometer HIPO.

A search for hep solar neutrinos at the Sudbury Neutrino Observatory

NASA Astrophysics Data System (ADS)

Winchester, Timothy J.

Solar neutrinos from the fusion hep reaction, (helium-3 fusing with a proton to become helium-4, releasing a positron and neutrino), have previously remained undetected due to their flux being about one one-thousandth that of boron-8 neutrinos. These neutrinos are interesting theoretically because they are less dependent on solar composition than other solar neutrinos, and therefore provide a somewhat independent test of the Standard Solar Model. In this analysis, we develop a new event fitter for existing data from the Sudbury Neutrino Observatory. We also use the fitter to remove backgrounds that previously limited the fiducial volume, which we increase by 30%. We use a modified Wald-Wolfowitz test to increase the amount of live time by 200 days (18%) and show that this data is consistent with the previously-used data. Finally, we develop a Bayesian analysis technique to make full use of the posterior distributions of energy returned by the event fitter. In the first significant detection of hep neutrinos, we find that the most-probable rate of hep events is 3.5 x 10. 4 /cm. 2/s, which is significantly higher than the theoretical prediction. We find that the 95% credible region extends from 1.0 to 7.2 x 10. 4 /cm. 2/s, and that we can therefore exclude a rate of 0 hep events at greater than 95% probability.

Solar Cycle Fine Structure and Surface Rotation from Ca II K-Line Time Series Data

NASA Astrophysics Data System (ADS)

Scargle, Jeff; Keil, Steve; Worden, Pete

2011-10-01

Analysis of three and a half decades of data from the NSO/AFRL/Sac Peak K-line monitoring program yields evidence for four components to the variation: (a) the solar cycle, with considerable fine structure and a quasi-periodicity of 122.4 days; (b) a stochastic process, faster than (a) and largely independent of it, (c) a quasi-periodic signal due to rotational modulation, and of course (d) observational errors (shown to be quite small). Correlation and power spectrum analyses elucidate periodic and aperiodic variation of these chromospheric parameters. Time-frequency analysis is especially useful for extracting information about differential rotation, and in particular elucidates the connection between its behavior and fine structure of the solar cycle on approximately one-year time scales. These results further suggest that similar analyses will be useful at detecting and characterizing differential rotation in stars from stellar light-curves such as those being produced by NASA's Kepler observatory. Component (b) consists of variations over a range of timescales, in the manner of a "1/f" random process. A time-dependent Wilson-Bappu effect appears to be present in the solar cycle variations (a), but not in the stochastic process (b). The data can be found at the National Solar Observatory web site http://nsosp.nso.edu/data/cak_mon.html, or by file transfer protocol at ftp://ftp.nso.edu/idl/cak.parameters.

Astronomia solare e ottica con il foro stenopeico

NASA Astrophysics Data System (ADS)

Sigismondi, Costantino

The observation of the Sun with pinholes was started in Florence's Cathedral in 1475, and in Ulugh Beg observatory in Samarcand in 1424-29, well before the invention of the telescope, for measuring the solar position and the variation of the obliquity of the Earth's axis. Later, with Kepler, pinholes' telescopes were used to follow the solar spots when the telescopes made by Galileo were not available. The use of pinholes in positional solar astrometry continued successfully up to 1800 in some great Italian and French Churches. Nowadays by using pinholes it is possible to show the principles of positional astronomy and imaging to students with instruments very easy to be built at almost no cost. The concepts of focal length, best focus, angular resolution, atmospheric seeing and atmospheric transmittance can be verified with such simple devices. Such pinhole telescopes have been built by primary-school students at the Astronomical Observatory dedicated to the Pope astronomer Sylvester II, located in Bukowiec, Poland, which is at its third year of activity. The largest solar spots have been observed clearly with these instruments, demonstrating the principles discussed in this presentation. The light cast by one of this devices with 70 m of focal length and 1 cm of diameter has permitted to repeat the experiences on the diffraction of the light, made in 1648 by the Jesuits Riccioli and Grimaldi.

The Solar Dynamics Observatory

NASA Technical Reports Server (NTRS)

Pesnell, William D.

2008-01-01

The Solar Dynamics Observatory (SDO) is the first Space Weather Mission in NASA's Living With a Star Program. SDO's main goal is to understand, driving towards a predictive capability, those solar variations that influence life on Earth and humanity's technological systems. The past decade has seen an increasing emphasis on understanding the entire Sun, from the nuclear reactions at the core to the development and loss of magnetic loops in the corona. SDO's three science investigations (HMI, AIA, and EVE) will determine how the Sun's magnetic field is generated and structured, how this stored magnetic energy is released into the heliosphere and geospace as the solar wind, energetic particles, and variations in the solar irradiance. SDO will return full-disk Dopplergrams, full-disk vector magnetograms, full-disk images at nine EIUV wavelengths, and EUV spectral irradiances, all taken at a rapid cadence. This means you can 'observe the database' to study events, but we can also move forward in producing quantitative models of what the Sun is doing today. SDO is scheduled to launch in 2008 on an Atlas V rocket from the Kennedy Space Center, Cape Canaveral, Florida. The satellite will fly in a 28 degree inclined geosynchronous orbit about the longitude of New Mexico, where a dedicated Ka-band ground station will receive the 150 Mbps data flow. How SDO data will transform the study of the Sun and its affect on Space Weather studies will be discussed.

Building a new space weather facility at the National Observatory of Athens

NASA Astrophysics Data System (ADS)

Kontogiannis, Ioannis; Belehaki, Anna; Tsiropoula, Georgia; Tsagouri, Ioanna; Anastasiadis, Anastasios; Papaioannou, Athanasios

2016-01-01

The PROTEAS project has been initiated at the Institute of Astronomy, Astrophysics, Space Applications and Remote Sensing (IAASARS) of the National Observatory of Athens (NOA). One of its main objectives is to provide observations, processed data and space weather nowcasting and forecasting products, designed to support the space weather research community and operators of commercial and industrial systems. The space weather products to be released by this facility, will be the result of the exploitation of ground-based, as well as space-borne observations and of model results and tools already available or under development by IAASARS researchers. The objective will be achieved through: (a) the operation of a small full-disk solar telescope to conduct regular observations of the Sun in the H-alpha line; (b) the construction of a database with near real-time solar observations which will be available to the community through a web-based facility (HELIOSERVER); (c) the development of a tool for forecasting Solar Energetic Particle (SEP) events in relation to observed solar eruptive events; (d) the upgrade of the Athens Digisonde with digital transceivers and the capability of operating in bi-static link mode and (e) the sustainable operation of the European Digital Upper Atmosphere Server (DIAS) upgraded with additional data sets integrated in an interface with the HELIOSERVER and with improved models for the real-time quantification of the effects of solar eruptive events in the ionosphere.

CAN A NANOFLARE MODEL OF EXTREME-ULTRAVIOLET IRRADIANCES DESCRIBE THE HEATING OF THE SOLAR CORONA?

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

Tajfirouze, E.; Safari, H.

2012-01-10

Nanoflares, the basic units of impulsive energy release, may produce much of the solar background emission. Extrapolation of the energy frequency distribution of observed microflares, which follows a power law to lower energies, can give an estimation of the importance of nanoflares for heating the solar corona. If the power-law index is greater than 2, then the nanoflare contribution is dominant. We model a time series of extreme-ultraviolet emission radiance as random flares with a power-law exponent of the flare event distribution. The model is based on three key parameters: the flare rate, the flare duration, and the power-law exponentmore » of the flare intensity frequency distribution. We use this model to simulate emission line radiance detected in 171 A, observed by Solar Terrestrial Relation Observatory/Extreme-Ultraviolet Imager and Solar Dynamics Observatory/Atmospheric Imaging Assembly. The observed light curves are matched with simulated light curves using an Artificial Neural Network, and the parameter values are determined across the active region, quiet Sun, and coronal hole. The damping rate of nanoflares is compared with the radiative losses cooling time. The effect of background emission, data cadence, and network sensitivity on the key parameters of the model is studied. Most of the observed light curves have a power-law exponent, {alpha}, greater than the critical value 2. At these sites, nanoflare heating could be significant.« less

Evidence for the Magnetic Breakout Model in an Equatorial Coronal-Hole Jet

NASA Technical Reports Server (NTRS)

Kumar, Pankaj; Karpen, Judith T.; Antiochos, Spiro K.; Wyper, Peter F.; Devore, C. Richard; DeForest, Craig E.

2018-01-01

Small, impulsive jets commonly occur throughout the solar corona, but are especially visible in coronal holes. Evidence is mounting that jets are part of a continuum of eruptions that extends to much larger coronal mass ejections and eruptive flares. Because coronal-hole jets originate in relatively simple magnetic structures, they offer an ideal testbed for theories of energy buildup and release in the full range of solar eruptions. We analyzed an equatorial coronal-hole jet observed by the Solar Dynamics Observatory (SDO)/AIA (Atmospheric Imaging Assembly)) on 2014 January 9 in which the magnetic-field structure was consistent with the embedded-bipole topology that we identified and modeled previously as an origin of coronal jets. In addition, this event contained a mini-filament, which led to important insights into the energy storage and release mechanisms. SDO/HMI (Solar Dynamics Observatory/Helioseismic and Magnetic Imager) magnetograms revealed footpoint motions in the primary minority-polarity region at the eruption site, but show negligible flux emergence or cancellation for at least 16 hours before the eruption. Therefore, the free energy powering this jet probably came from magnetic shear concentrated at the polarity inversion line within the embedded bipole. We find that the observed activity sequence and its interpretation closely match the predictions of the breakout jet model, strongly supporting the hypothesis that the breakout model can explain solar eruptions on a wide range of scales.

On-orbit degradation of recent space-based solar instruments and understanding of the degradation processes

NASA Astrophysics Data System (ADS)

Meftah, M.; Dominique, M.; BenMoussa, A.; Dammasch, I. E.; Bolsée, D.; Pereira, N.; Damé, L.; Bekki, S.; Hauchecorne, A.

2017-05-01

The space environment is considered hazardous to spacecraft, resulting in materials degradation. Understanding the degradation of space-based instruments is crucial in order to achieve the scientific objectives, which are derived from these instruments. This paper discusses the on-orbit performance degradation of recent spacebased solar instruments. We will focus on the instruments of three space-based missions such as the Project for On-Board Autonomy 2 (PROBA2) spacecraft, the Solar Monitoring Observatory (SOLAR) payload onboard the Columbus science Laboratory of the International Space Station (ISS) and the PICARD spacecraft. Finally, this paper intends to understand the degradation processes of these space-based solar instruments.

Multi-thermal observations of flares and eruptions with the Atmospheric Imaging Assembly on the Solar Dynamics Observatory. (Invited)

NASA Astrophysics Data System (ADS)

Schrijver, C. J.; Aia Science Team

2010-12-01

The revolutionary advance in observational capabilities offered by SDO's AIA offers new views of solar flares and eruptions. The high cadence and spatial resolution, the full-Sun coverage, and the variety of thermal responses of the AIA channels from thousands to millions of degrees enable the study the source regions of solar explosions, as well as the responses of the solar corona from their immediate vicinity to regions over a solar radius away. These observations emphasize the importance of magnetic connectivity and topology, the frequent occurrence of fast wave-like perturbations, and the contrasts between impulsive compact X-ray-bright flares and long-duration EUV-bright phenomena.

Wanderings of the 'Simply Perfect' Burnham Telescope

NASA Astrophysics Data System (ADS)

Lattis, James

2017-08-01

S.W. Burnham's 6-inch Clark refractor, in service from 1870, quickly became famous as a potent double star catcher. It was the instrument he used for the site survey of Lick Observatory in 1879. Sold to Washburn Observatory, it travelled to Caroline Island with Edward Holden to search for Vulcan during the total solar eclipse of May 1883. Back in Madison, it was used by George Comstock for his measurements of refraction and aberration. In the late 1950s it was used at the Knuijt Observatory in Appleton, Wisconsin. Travels and transformations of this famous telescope have spread its parts widely as astronomical relics, and it even remains in active service today.

Contamination control requirements implementation for the James Webb Space Telescope (JWST), part 2: spacecraft, sunshield, observatory, and launch

NASA Astrophysics Data System (ADS)

Wooldridge, Eve M.; Schweiss, Andrea; Henderson-Nelson, Kelly; Woronowicz, Michael; Patel, Jignasha; Macias, Matthew; McGregor, R. Daniel; Farmer, Greg; Schmeitzky, Olivier; Jensen, Peter; Rumler, Peter; Romero, Beatriz; Breton, Jacques

2014-09-01

This paper will continue from Part 1 of JWST contamination control implementation. In addition to optics, instruments, and thermal vacuum testing, JWST also requires contamination control for a spacecraft that must be vented carefully in order to maintain solar array and thermal radiator thermal properties; a tennis court-sized sunshield made with 1-2 mil Kapton™ layers that must be manufactured and maintained clean; an observatory that must be integrated, stowed and transported to South America; and a rocket that typically launches commercial payloads without contamination sensitivity. An overview of plans developed to implement contamination control for the JWST spacecraft, sunshield, observatory and launch vehicle will be presented.

Morphometric analysis of pulp size in maxillary permanent central incisors correlated with age: An indirect digital study.

PubMed

Ravindra, S V; Mamatha, G P; Sunita, J D; Balappanavar, Aswini Y; Sardana, Varun

2015-01-01

Teeth are hardest part of the body and are least affected by the taphonomic process. They are considered as one of the reliable methods of identification of a person in forensic sciences. The aim of the following study is to establish morphometeric measurements by AutoCad 2009 (Autodesk, Inc) of permanent maxillary central incisors in different age groups of Udaipur population. Hospital-based descriptive cross-sectional study carried out in Udaipur. A study was carried out on 308 subjects of both genders with the age range of 9-68 years. Standardized intra-oral radiographs were made by paralleling technique and processed. The radiographs were scanned and the obtained images were standardized to the actual size of radiographic film. This was followed by measuring them using software AutoCad 2009. F-test, post-hoc test, Pearson's correlation test. For left maxillary central incisor, the total pulp area was found to be of 38.41 ± 12.88 mm and 14.32 ± 7.04 mm respectively. For right maxillary central incisor, the total pulp size was 38.39 ± 14.95 mm and 12.35 ± 5 mm respectively. Males (32.50, 32.87 mm(2)) had more pulp area when compared with females (28.82, 30.05 mm(2)). There was a decrease in total pulp area with increasing age which may be attributed to secondary dentin formation.

Solar activity and oscillation frequency splittings

NASA Technical Reports Server (NTRS)

Woodard, M. F.; Libbrecht, K. G.

1993-01-01

Solar p-mode frequency splittings, parameterized by the coefficients through order N = 12 of a Legendre polynomial expansion of the mode frequencies as a function of m/L, were obtained from an analysis of helioseismology data taken at Big Bear Solar Observatory during the 4 years 1986 and 1988-1990 (approximately solar minimum to maximum). Inversion of the even-index splitting coefficients confirms that there is a significant contribution to the frequency splittings originating near the solar poles. The strength of the polar contribution is anti correlated with the overall level or solar activity in the active latitudes, suggesting a relation to polar faculae. From an analysis of the odd-index splitting coefficients we infer an uppor limit to changes in the solar equatorial near-surface rotatinal velocity of less than 1.9 m/s (3 sigma limit) between solar minimum and maximum.

The Effects of Propellant Slosh Dynamics on the Solar Dynamics Observatory

NASA Technical Reports Server (NTRS)

Mason, Paul; Starin, Scott R.

2011-01-01

The Solar Dynamics Observatory (SDO) mission, which is part of the Living With a Star program, was successfully launched and deployed from its Atlas V launch vehicle on February 11, 2010. SDO is an Explorer-class mission now operating in a geosynchronous orbit (GEO). The basic mission is to observe the Sun for a very high percentage of the 5-year mission (10-year goal) with long stretches of uninterrupted observations and with constant, high-data-rate transmission to a dedicated ground station located in White Sands, New Mexico. Almost half of SDO's launch mass was propellant, contained in two large tanks. To ensure performance with this amount of propellant, a slosh analysis was performed prior to launch. This paper provides an overview of the SDO slosh analysis, the on-orbit experience, and the lessons learned.

The Effects of Propellant Slosh Dynamics on the Solar Dynamics Observatory

NASA Technical Reports Server (NTRS)

Mason, Paul; Starin, Scott R.

2011-01-01

The Solar Dynamics Observatory (SOO) mission, which is part of the Living With a Star program, was successfully launched and deployed from its Atlas V launch vehicle on February 11, 2010. SOO is an Explorer-class mission now operating in a geosynchronous orbit (GEO). The basic mission is to observe the Sun for a very high percentage of the 5-year mission (10-year goal) with long stretches of uninterrupted observations and with constant, high-data-rate transmission to a dedicated ground station located in White Sands, New Mexico. Almost half of SDO's launch mass was propellant, contained in two large tanks. To ensure performance with this amount of propellant, a slosh analysis was performed prior to launch. This paper provides an overview of the SDO slosh analysis, the on-orbit experience, and the lessons learned.

Within the International Collaboration CHAIN: a Summary of Events Observed with Flare Monitoring Telescope (FMT) in Peru

NASA Astrophysics Data System (ADS)

Ishitsuka, J.; Asai, A.; Morita, S.; Terrazas, R.; Cabezas, D.; Gutierrez, V.; Martinez, L.; Buleje, Y.; Loayza, R.; Nakamura, N.; Takasao, S.; Yoshinaga, Y.; Hillier, A.; Otsuji, K.; Shibata, K.; Ishitsuka, M.; Ueno, S.; Kitai, R.; Ishii, T.; Ichimoto, K.; Nagata, S.; Narukage, N.

2014-02-01

In 2008 we inaugurated the new Solar Observatory in collaboration with Faculty of Sciences of San Luis Gonzaga de Ica National University, 300 km south of Lima. In March of 2010 a Flare Monitoring Telescope of Hida Observatory of Kyoto University arrived to Ica, part of CHAIN Project (Continuous H-alpha Imaging Network). In October of the same year we hosted the First FMT Workshop in Ica, then in July of 2011 the Second FMT Workshop was opened. Since that we are focused on two events registered by FMT in Peru to publish results. FMT is a good tool to introduce young people from universities into scientific knowledge; it is good also for education in Solar Physics and outreach. Details of this successful collaboration will be explained in this presentation.

Data Distribution System (DDS) and Solar Dynamic Observatory Ground Station (SDOGS) Integration Manager

NASA Technical Reports Server (NTRS)

Pham, Kim; Bialas, Thomas

2012-01-01

The DDS SDOGS Integration Manager (DSIM) provides translation between native control and status formats for systems within DDS and SDOGS, and the ASIST (Advanced Spacecraft Integration and System Test) control environment in the SDO MOC (Solar Dynamics Observatory Mission Operations Center). This system was created in response for a need to centralize remote monitor and control of SDO Ground Station equipments using ASIST control environment in SDO MOC, and to have configurable table definition for equipment. It provides translation of status and monitoring information from the native systems into ASIST-readable format to display on pages in the MOC. The manager is lightweight, user friendly, and efficient. It allows data trending, correlation, and storing. It allows using ASIST as common interface for remote monitor and control of heterogeneous equipments. It also provides failover capability to back up machines.

KSC-06pd2263

NASA Image and Video Library

2006-10-10

KENNEDY SPACE CENTER, FLA. - With a convoy of escorts, the STEREO spacecraft is transported to Launch Pad 17-B on Cape Canaveral Air Force Station. At the pad the spacecraft will be lifted into the mobile service tower. STEREO stands for Solar Terrestrial Relations Observatory and comprises two spacecraft. The STEREO mission is the first to take measurements of the sun and solar wind in 3-dimension. This new view will improve our understanding of space weather and its impact on the Earth. The STEREO mission is managed by Goddard Space Flight Center. The Applied Physics Laboratory designed and built the spacecraft. The laboratory will maintain command and control of the observatories throughout the mission, while NASA tracks and receives the data, determines the orbit of the satellites, and coordinates the science results. STEREO is expected to lift off Oct. 25. Photo credit: NASA/George Shelton

The Solar Dynamics Observatory Education and Public Outreach Program: The First Years

NASA Astrophysics Data System (ADS)

Wawro, M.; Drobnes, E.; van Doren, A.; Scherrer, D. K.

2010-12-01

The Solar Dynamics Observatory (SDO) Education and Public Outreach (E/PO) program began as a series of discrete programs implemented by each of the instrument teams and has evolved into a well-rounded program with a full suite of national and international programs: student, teacher, and journalist workshops, international research programs, family programs, etc. In this presentation, we provide an overview of our philosophy and approach and of some of the programs developed and implemented prior to launch. In conclusion we will summarize our successes, our failures, our lessons learned, and present guiding principles in the hope that future missions will use our platform as a guide to build upon for future programs, incorporating their own content to enhance the public's appreciation of the science that NASA does and its benefit to society.

70 Years of Sunspot Observations at the Kanzelhöhe Observatory: Systematic Study of Parameters Affecting the Derivation of the Relative Sunspot Number

NASA Astrophysics Data System (ADS)

Pötzi, Werner; Veronig, Astrid M.; Temmer, Manuela; Baumgartner, Dietmar J.; Freislich, Heinrich; Strutzmann, Heinz

2016-11-01

The Kanzelhöhe Observatory (KSO) was founded during World War II by the Deutsche Luftwaffe (German Airforce) as one station of a network of observatories that were set up to provide information on solar activity in order to better assess the actual conditions of the Earth's ionosphere in terms of radio-wave propagation. Solar observations began in 1943 with photographs of the photosphere and drawings of sunspots, plage regions, and faculae, as well as patrol observations of the solar corona. At the beginning, all data were sent to Freiburg (Germany). After WW II, international cooperation was established and the data were sent to Zurich, Paris, Moscow, and Greenwich. Relative sunspot numbers have been derived since 1944. The agreement between relative sunspot numbers derived at KSO and the new International Sunspot Number (ISN) (SILSO World Data Center in International Sunspot Number Monthly Bulletin and online catalogue, 1945 - 2015) lies within {≈} 10 %. However, revisiting the historical data, we also find periods with larger deviations. The reasons for the deviations were twofold: On the one hand, a major instrumental change took place during which the instrument was relocated and modified. On the other hand, a period of frequent replacements of personnel caused significant deviations; this clearly shows the importance of experienced observers. In the long term, the instrumental improvements led to better image quality. Additionally, we find a long-term trend towards better seeing conditions that began in 2000.

Deep Space Climate Observatory (DSCOVR) lifted off from Cape Canaveral

NASA Image and Video Library

2015-02-13

KSC-2015-1341 (02/11/2015) --- The SpaceX Falcon 9 rocket carrying NOAA’s Deep Space Climate Observatory spacecraft, or DSCOVR, lifts off from Space Launch Complex 40 at Cape Canaveral Air Force Station in Florida. Liftoff occurred at 6:03 p.m. EST. DSCOVR is a partnership between NOAA, NASA and the U.S. Air Force, and will maintain the nation's real-time solar wind monitoring capabilities. To learn more about DSCOVR, visit www.nesdis.noaa.gov/DSCOVR. Photo credit: NASA/Ben Smegelsky

Orders of magnitude: A history of NACA and NASA, 1915-1976

NASA Technical Reports Server (NTRS)

Anderson, F. W.

1976-01-01

A brief history of aeronautics and space exploration is presented. The Federal government's role in contributing, by research and development, to the advancement of aeronautics and space exploration is emphasized. The flight of man is traced from Kitty Hawk to walks and rides on the surface of the moon. Orbiting Solar Observatories, Orbiting Observatories, planetary exploration (Mariner Space Probes, Pioneer Space Probes) the Earth Resources Program, and Skylab are included. The development of the space shuttle is also discussed.

Comparison of solar photovoltaic and nuclear reactor power systems for a human-tended lunar observatory

NASA Technical Reports Server (NTRS)

Hickman, J. M.; Bloomfield, H. S.

1989-01-01

Photovoltaic and nuclear surface power systems were examined at the 20 to 100 kW power level range for use at a human-tended lunar astronomical observatory, and estimates of the power system masses were made. One system, consisting of an SP-100 thermoelectric nuclear power supply integrated with a lunar lander, is recommended for further study due to its low system mass, potential for modular growth, and applicability to other surface power missions, particularly in the Martian system.

The Next Generation of Chromospheric Measurements

NASA Astrophysics Data System (ADS)

Tarbell, T. D.

2005-05-01

I discuss the new measurements which we know will happen, from missions or observatories which are being developed now, as well as the measurements which should happen for further progress. The future is promising, with new missions such as Solar-B, SDO, and SunRise, and new or upgraded observatories, such as SVST, DOT, GREGOR, ATST, and FASR. I also point out significant needs for the future, such as detailed chromospheric spectroscopy of the type which would have been provided by NEXUS or similar instruments.

Sensor lighting considerations for earth observatory satellite missions

NASA Technical Reports Server (NTRS)

Cooley, J. L.

1972-01-01

Facets of sensor lighting conditions for Earth observatory satellite missions are considered. Assuming onboard sensors of a given width viewing perpendicular to the subsatellite ground track along sun-synchronous orbits with various nodes, the ground trace of the ends of the sensor coverage were found, as well as the variation in solar illumination on the ground across the line covered by the sensor during the day for any point along the orbit. The changes with season and variation during the year were also found.

Gravity research at Cottrell observatory

NASA Technical Reports Server (NTRS)

Tuman, V. S.; Anderson, J. D.; Lau, E. L.

1977-01-01

The Cottrell gravity research observatory and work in progress are described. Equipment in place and equipment to be installed, the cryogenic gravity meter (CGM), concrete pads to support the vertical seismometer, CGM, and guest experiments, techniques of data analysis, and improvements needed in the CGM are discussed. Harmonic earth eigenvibrations with multipole moments are examined and their compatibility with a fictitious black hole binary system (of which the primary central mass is assigned a value one million solar masses) located 400 light-years away is shown by calculations.

Comparison of solar photovoltaic and nuclear reactor power systems for a human-tended lunar observatory

NASA Technical Reports Server (NTRS)

Hickman, J. M.; Bloomfield, H. S.

1989-01-01

Photovoltaic and nuclear surface power systems were examined at the 20 to 100 kW power level range for use at a human-tended lunar astronomical observatory, andestimates of the power system masses were made. One system, consisting of an SP-100 thermoelectric nuclear power supply integrated with a lunar lander, is recommended for further study due to its low system mass, potential for modular growth, and applicability to other surface power missions, particularly in the Martian system.

STS-37 Gamma Ray Observatory (GRO) grappled by RMS

NASA Image and Video Library

1991-04-07

Backdropped against the Earth's surface, the Gamma Ray Observatory (GRO) with its solar array (SA) panels deployed is grappled by the remote manipulator system (RMS) during STS-37 systems checkout. GRO's four complement instruments are visible: the Energetic Gamma Ray Experiment Telescope (EGRET) (at the bottom); the Imaging Compton Telescope (COMPTEL) (center); the Oriented Scintillation Spectrometer Experiment (OSSE) (top); and Burst and Transient Source Experiment (BATSE) (on four corners). The view was taken by STS-37 crew through an aft flight deck overhead window.

Obituary: Horace Welcome Babcock, 1912-2003

NASA Astrophysics Data System (ADS)

Vaughan, Arthur Harris

2003-12-01

Horace Welcome Babcock died in Santa Barbara, California on 29 August 2003, fifteen days short of his ninety-first birthday. An acclaimed authority on solar and stellar magnetism and the originator of ingenious advances in astronomical instrumentation in his earlier career, he served as Director of Mount Wilson and Palomar (later Hale) Observatories from 1964 until his retirement in 1978. The founding of the Carnegie Institution of Washington's Las Campanas Observatory in Chile was the culmination of his directorship. Horace was born in Pasadena California on 13 September 1912, the only child of Harold Delos Babcock and Mary G. Henderson. His father, an electrical engineer and physicist by training, had been hired by George Ellery Hale to work at the recently founded Mount Wilson Solar Observatory beginning in 1909. Thus Horace spent much of his boyhood on Mount Wilson in the company of astronomers. Horace developed an early interest in astronomy, worked as a volunteer solar observer at Mount Wilson and published his first paper in 1932, with his father. He was fascinated by fine mechanisms and by optical and electrical instruments. After graduating from Caltech with a degree in structural engineering in 1934, he earned his PhD in astronomy at Lick Observatory in 1938. His dissertation provided the first measurement of the rotational velocity curve and a derivation of the mass-to-luminosity ratio for M31; this work is still cited in reviews of the study of ``dark matter." Horace served as a research assistant at Lick Observatory (1938 39) and an Instructor at the University of Chicago's McDonald and Yerkes Observatories (1939--41) under Otto Struve. He undertook radar-related wartime electronics work at the MIT Radiation Laboratory (1941 42) and then worked on aircraft rocket launchers as part of the Caltech Rocket Project (1942 45). This project brought him into contact with Ira S. Bowen, head of the project's Photographic Division. Impressed with his knowledge of electronics, Bowen invited Horace to join the scientific staff of the Mount Wilson and Palomar Observatories starting on 1 January 1946, the day Bowen took up his duties as Director. The appointment required Horace to spend about half his time developing instrumentation Bowen deemed necessary for the Observatory, leaving him otherwise free to pursue independent research in astronomy. Horace headed the Mount Wilson grating ruling laboratory (earlier headed by his father) from 1948 until 1963. Under Horace's supervision, the ruling engines were further perfected and equipped with interferometric control to produce the largest and most efficient diffraction gratings ever made up to that time. The Carnegie Institution supported this activity and supplied ``Babcock Gratings" free of charge to some two-dozen observatories and laboratories around the world, in addition to those installed at the Mount Wilson and Palomar Observatories. Horace invented and built automatic guiders for astronomical telescopes and the first electronic exposure meter for astronomical spectroscopy. Well ahead of his time, he proposed and explored experimentally the possibility of using adaptive optics to overcome the blurring effects of turbulence in the Earth's atmosphere. Any historical account of the status of adaptive optics today must begin with a reference to Horace Babcock's 1953 paper. In his first independent research venture as a new staff member beginning in 1946, Horace devised and successfully applied a method for detecting, for the first time, magnetic fields in stars other than the Sun. Thus began an extensive study of magnetic stars that attracted many followers and brought worldwide recognition to its author. In 1952 he devised the first photoelectric solar magnetograph, which allowed the first detection of the Sun's weak general magnetic field. His subsequent researches in collaboration with Harold Babcock demonstrated that the Sun's general dipolar field reverses polarity in successive sunspot cycles. Until about 1957 this work had been done at the Hale Solar Laboratory on Holladay Road in Pasadena. Improved models of the magnetograph developed by Robert F. Howard, in collaboration with Horace, went into operation in the 150-foot solar tower telescope at Mount Wilson in 1959 and later, and similar instruments are now employed at many other solar observatories. In 1961 Horace proposed an explanation of the Sun's 22-year magnetic cycle that contained many of the features still embodied in contemporary theoretical models of the phenomenon. The advance in our understanding of solar and stellar magnetism brought forth by Horace Babcock is a worthy sequel to the pioneering efforts initiated by George E. Hale early in the twentieth century. Faced with the growing obsolescence of the Carnegie Institution of Washington's facilities at Mount Wilson along with the competition from Caltech's 200-inch telescope, the Carnegie Trustees in 1963 adopted the idea of founding a major observatory in the Southern Hemisphere as its master plan for modernizing the astronomical facilities of the Institution. Upon becoming Director of the Mount Wilson and Palomar Observatories in 1964, Horace Babcock embraced the job of carrying out this plan, although it meant giving up his own science. Beginning in 1963, and with his usual ingenuity, Horace developed apparatus for measuring astronomical ``seeing." In collaboration with John Irwin and others, he carried out site surveys in Chile, Australia and New Zealand with the aim of selecting the best available location for the anticipated array of large telescopes. Some five years of exploration led, in 1968, to the selection and purchase of a 276 square-kilometer tract on Cerro Las Campanas in north central Chile as the site for the new observatory. Babcock and Irwin had first climbed to its summit, on foot, in October 1966. The team Horace assembled to build the observatory and its infrastructure proved equal to the high standards he set, and they got the job done. The Swope 1-meter telescope was placed into operation at Las Campanas in 1971. The Irénée du Pont 2.5-meter Telescope was completed and dedicated in 1976. The Las Campanas Observatory is the current site of two 6.5 meter optical telescopes constructed there in a collaboration between the Carnegie Institution of Washington, the University of Arizona, Harvard University, the University of Michigan and the Massachusetts Institute of Technology; they were placed into operation in 2000 and 2002. That Las Campanas offers unsurpassed astronomical seeing, and its infrastructure provides ample capacity for even larger telescopes of the future, stands as a testimony to Horace Babcock's vision and stubborn tenacity in acquiring and developing the best possible site for the Carnegie Southern Observatory. For several years, Horace owned a 26-foot sailboat, which he kept at Redondo Beach. It was his private domain and escape. On many occasions, he invited younger colleagues to sail with him. The boat was equipped with an automatic pilot of Horace's design. It electronically controlled the vessel's heading by sensing the Earth's magnetic field direction relative to the intended course and drove a servomotor to adjust the tiller accordingly. The device was not unlike the automatic guider Horace had built for the 200-inch telescope. Horace was elected to the National Academy of Sciences in 1954. He was awarded the National Academy's Henry Draper Medal in 1957; the Catherine Wolfe Bruce Gold Medal of the Astronomical Society of the Pacific in 1969; the Royal Astronomical Society's Eddington Medal in 1958 and its Gold Medal in 1970; and the George Ellery Hale Prize of the Solar Physics Division of the AAS in 1992. Horace leaves a daughter Ann L. Babcock and son Bruce H. Babcock by a first marriage, a son Kenneth L. Babcock by a second marriage (to Elizabeth M. Jackson, who survives him), and a granddaughter. Both marriages ended in divorce. Those who worked with Horace and knew him well were familiar with his uncommonly reserved nature, and indeed also with his display of hot temper on rare occasions. One familiar with the distinguished scientific accomplishments of his earlier career could recognize in Horace an abiding modesty about them. At a personal level he was gracious and generous. In conversation and at meetings, he considered his words with meticulous care before enunciating them. He could be noticeably ill at ease in public speaking, particularly if an occasion called for extemporaneous remarks. His published writings stand as masterpieces of lucid exposition. In his later years, he was a popular speaker at gatherings of students and amateur astronomers, to whom he offered entertaining and remarkably informative personal stories about his scientific endeavors and early life experiences at Mount Wilson Observatory.

Alfvén Wave Heating Model of an Active Region and Comparisons with the EIS Observations

NASA Astrophysics Data System (ADS)

Lawless, A. P.; Asgari-Targhi, M.

2013-12-01

We study the generation and dissipation of Alfvén waves in open and closed field lines using the images from the Solar Dynamics Observatory's (SDO) Atmospheric Imaging Assembly (AIA) (van Ballegouijen et al. 2011; Asgari-Targhi & van Ballegouijen 2012; Asgari et al. 2013). The goal is to search for observational evidence of Alfvén waves in the solar corona and to understand their role in coronal heating. We focus on one particular active region on the 10th of December 2007. Using the MDI magnetogram and the potential field modeling of this region, we create three-dimensional MHD models for several open and closed field lines in different locations in the active region. For each model, we compute the temperature, pressure, magnetic field strength, average heating rate, and other parameters along the loop. We then compare these results with the EIS observations. This research is supported by the NSF grant for the Solar physics REU Program at the Smithsonian Astrophysical Observatory (AGS-1263241) and contract SP02H1701R from Lockheed-Martin to SAO.