Passive ranging redundancy reduction in diurnal weather conditions

NASA Astrophysics Data System (ADS)

Cha, Jae H.; Abbott, A. Lynn; Szu, Harold H.

2013-05-01

Ambiguity in binocular ranging (David Marr's paradox) may be resolved by using two eyes moving from side to side behind an optical bench while integrating multiple views. Moving a head from left to right with one eye closed can also help resolve the foreground and background range uncertainty. That empirical experiment implies redundancy in image data, which may be reduced by adopting a 3-D camera imaging model to perform compressive sensing. Here, the compressive sensing concept is examined from the perspective of redundancy reduction in images subject to diurnal and weather variations for the purpose of resolving range uncertainty at all weather conditions such as the dawn or dusk, the daytime with different light level or the nighttime at different spectral band. As an example, a scenario at an intersection of a country road at dawn/dusk is discussed where the location of the traffic signs needs to be resolved by passive ranging to answer whether it is located on the same side of the road or the opposite side, which is under the influence of temporal light/color level variation. A spectral band extrapolation via application of Lagrange Constrained Neural Network (LCNN) learning algorithm is discussed to address lost color restoration at dawn/dusk. A numerical simulation is illustrated along with the code example.

KSC-07pd1241

NASA Image and Video Library

2007-05-17

KENNEDY SPACE CENTER, FLA. -- In the Astrotech Space Operations facility, Orbital Science technicians verify that a computer chip is securely bonded to a side brace on the Dawn spacecraft. The silicon chip holds the names of more than 360,000 space enthusiasts worldwide who signed up to participate in a virtual voyage to the asteroid belt and is about the size of an American five-cent coin. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

KSC-07pd1240

NASA Image and Video Library

2007-05-17

KENNEDY SPACE CENTER, FLA. -- In the Astrotech Space Operations facility, a computer chip is bonded to a side brace on the Dawn spacecraft. The silicon chip holds the names of more than 360,000 space enthusiasts worldwide who signed up to participate in a virtual voyage to the asteroid belt and is about the size of an American five-cent coin. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/Jim Grossmann

System III variations in apparent distance of Io plasma torus from Jupiter

NASA Technical Reports Server (NTRS)

Dessler, A. J.; Sandel, B. R.

1992-01-01

System III variations in apparent distance of the Io plasma torus from Jupiter are examined on the basis of data obtained from UVS scans across Jupiter's satellite system. The displacement of the dawn and dusk ansae are found to be unexpectedly complex. The displacements are unequal and both ansae are in motion with the motion of the approaching ansa being the lesser of the two. The radial motions, as measured from either the center of Jupiter or the offset-tilted dipole, are of unequal magnitude and have the System III periodicity. It is concluded that the cross-tail electric field that causes these torus motions is concentrated on the dusk ansa, varied with the System III period, and shows magnetic-anomaly phase control. It is found that the dawn-dust asymmetry in brightness is not explained simply by the cross-tail electric field. It is concluded that there is a heating mechanism that causes the dusk side of the Io plasma torus to be brighter than the dawn side.

Pre-Dawn Martian Sky

NASA Technical Reports Server (NTRS)

1997-01-01

On Sol 39 there were wispy blue clouds in the pre-dawn sky of Mars, as seen by the Imager for Mars Pathfinder (IMP). The color image was made by taking blue, green, and red images and then combining them into a single color image. The clouds appear to have a bluish side and a greenish side because they moved (in the wind from the northeast) between images. This picture was made an hour and twenty minutes before sunrise -- the sun is not shining directly on the water ice clouds, but they are illuminated by the dawn twilight.

Mars Pathfinder is the second in NASA's Discovery program of low-cost spacecraft with highly focused science goals. The Jet Propulsion Laboratory, Pasadena, CA, developed and manages the Mars Pathfinder mission for NASA's Office of Space Science, Washington, D.C. JPL is a division of the California Institute of Technology (Caltech). The Imager for Mars Pathfinder (IMP) was developed by the University of Arizona Lunar and Planetary Laboratory under contract to JPL. Peter Smith is the Principal Investigator.

Magnetic Flux Circulation During Dawn-Dusk Oriented Interplanetary Magnetic Field

NASA Technical Reports Server (NTRS)

Mitchell, E. J.; Lopez, R. E.; Fok, M.-C.; Deng, Y.; Wiltberger, M.; Lyon, J.

2010-01-01

Magnetic flux circulation is a primary mode of energy transfer from the solar wind into the ionosphere and inner magnetosphere. For southward interplanetary magnetic field (IMF), magnetic flux circulation is described by the Dungey cycle (dayside merging, night side reconnection, and magnetospheric convection), and both the ionosphere and inner magnetosphere receive energy. For dawn-dusk oriented IMF, magnetic flux circulation is not well understood, and the inner magnetosphere does not receive energy. Several models have been suggested for possible reconnection patterns; the general pattern is: dayside merging; reconnection on the dayside or along the dawn/dusk regions; and, return flow on dayside only. These models are consistent with the lack of energy in the inner magnetosphere. We will present evidence that the Dungey cycle does not explain the energy transfer during dawn-dusk oriented IMF. We will also present evidence of how magnetic flux does circulate during dawn-dusk oriented IMF, specifically how the magnetic flux reconnects and circulates back.

Sodium Velocity Maps on Mercury

NASA Technical Reports Server (NTRS)

Potter, A. E.; Killen, R. M.

2011-01-01

The objective of the current work was to measure two-dimensional maps of sodium velocities on the Mercury surface and examine the maps for evidence of sources or sinks of sodium on the surface. The McMath-Pierce Solar Telescope and the Stellar Spectrograph were used to measure Mercury spectra that were sampled at 7 milliAngstrom intervals. Observations were made each day during the period October 5-9, 2010. The dawn terminator was in view during that time. The velocity shift of the centroid of the Mercury emission line was measured relative to the solar sodium Fraunhofer line corrected for radial velocity of the Earth. The difference between the observed and calculated velocity shift was taken to be the velocity vector of the sodium relative to Earth. For each position of the spectrograph slit, a line of velocities across the planet was measured. Then, the spectrograph slit was stepped over the surface of Mercury at 1 arc second intervals. The position of Mercury was stabilized by an adaptive optics system. The collection of lines were assembled into an images of surface reflection, sodium emission intensities, and Earthward velocities over the surface of Mercury. The velocity map shows patches of higher velocity in the southern hemisphere, suggesting the existence of sodium sources there. The peak earthward velocity occurs in the equatorial region, and extends to the terminator. Since this was a dawn terminator, this might be an indication of dawn evaporation of sodium. Leblanc et al. (2008) have published a velocity map that is similar.

Dawn XMO2 Image 32

NASA Image and Video Library

2017-02-10

This image captures the day-night boundary, or terminator, in the north polar region of Ceres. The north pole itself, which lies just slightly left of center in this view, is barely sunlit, even though the local time at its location is 11:06 a.m. The north polar region is densely cratered, and some crater floors remain in permanent shadow. Some of those permanently shadowed craters contain bright deposits, as described in a 2016 Nature Astronomy study by scientists on NASA's Dawn mission. The best example of these bright deposits was found by Dawn in an unnamed and geologically young, 4-mile- (6-kilometer-) wide crater located at 86.2 degrees north latitude, 80.0 degrees east longitude (the small, sharply defined crater just right of center). This picture was obtained by the Dawn spacecraft on October 17, 2016, from an altitude of about 923 miles (1,486 kilometers). The image is located at 89 degrees north latitude, 86 degrees east longitude. http://photojournal.jpl.nasa.gov/catalog/PIA21397

Ground-Based Observation of Mercury's Sodium at Haleakala Observatory in 2013–2017

NASA Astrophysics Data System (ADS)

Kameda, S.; Kagitani, M.

2018-05-01

In this study, daily variation in Mercury's sodium exosphere was observed at the Haleakala Observatory in Hawaii. We confirmed the seasonal variation of the column density of sodium atoms over the dawn side differs from that over the dusk side.

Galileo view of Moon orbiting the Earth taken from 3.9 million miles

NASA Technical Reports Server (NTRS)

1992-01-01

Eight days after its encounter with the Earth, the Galileo spacecraft was able to look back and capture this remarkable view of the Moon in orbit about the Earth, taken from a distance of about 6.2 million kilometers (3.9 million miles). The picture was constructed from images taken through the violet, red, and 1.0-micron infrared filters. The Moon is in the foreground, moving from left to right. The brightly-colored Earth contrasts strongly with the Moon, which reflects only about one-third as much sunlight as the Earth. Contrast and color have been computer-enhanced for both objects to improve visibility. Antarctica is visible through clouds (bottom). The Moon's far side is seen; the shadowy indentation in the dawn terminator is the south-Pole/Aitken Basin, one of the largest and oldest lunar impact features. Alternate Jet Propulsion Laboratory (JPL) number is P-41508.

Dawn Color Topography of Ahuna Mons on Ceres

NASA Image and Video Library

2016-03-11

These color topographic views show variations in surface height around Ahuna Mons, a mysterious mountain on Ceres. The views are colorized versions of PIA20348 and PIA20349. They represent an update to the view in PIA19976, which showed the mountain using data from an earlier, higher orbit. Both views were made using images taken by NASA's Dawn spacecraft during its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) from the surface. The resolution of the component images is about 120 feet (35 meters) per pixel. Elevations span a range of about 5.5 miles (9 kilometers) from the lowest places in the region to the highest terrains. Blue represents the lowest elevation, and brown is the highest. The streaks running down the side of the mountain, which appear white in the grayscale view, are especially bright parts of the surface (the brightness does not relate to elevation). The elevations are from a shape model generated using images taken at varying sun and viewing angles during Dawn's lower-resolution, high-altitude mapping orbit (HAMO) phase. The side perspective view was generated by draping the image mosaics over the shape model. http://photojournal.jpl.nasa.gov/catalog/PIA20399

KSC-07pd1596

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians secure all sides of the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

KSC-07pd1595

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, a technician secures one side of the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

KSC-07pd1594

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, a technician secures one side of the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

Dawn Survey Orbit Image 42

NASA Image and Video Library

2015-08-06

This image of Ceres, taken by NASA's Dawn spacecraft, features a large, steep-sided mountain and several intriguing bright spots. The mountain's height is estimated to be about 4 miles (6 kilometers), which is a revision of the previous estimate of 3 miles (5 kilometers). It is the highest point seen on Ceres so far. The image was obtained on June 25, 2015 from an altitude of 2,700 miles (4,400 kilometers) above Ceres and has a resolution of 1,400 feet (410 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19615

Occia Crater

NASA Image and Video Library

2012-05-10

This image from NASA Dawn spacecraft of asteroid Vesta shows Occia crater, located in Vesta Gegania quadrangle, in Vesta southern hemisphere. A distinctive butterfly pattern is seen consisting of two separate lobes of ejecta on the opposite sides.

Effect of the Solar UV/EUV Heating on the Intensity and Spatial Distribution of Jupiter's Synchrotron Radiation

NASA Astrophysics Data System (ADS)

Kita, Hajime; Misawa, H.; Tsuchiya, F.; Tao, C.; Morioka, A.

2012-10-01

Jupiter's synchrotron radiation (JSR) is the emission from relativistic electrons, and it is the most effective probe for remote sensing of Jupiter's radiation belt from the Earth. Recent observations reveal short term variations of JSR with the time scale of days to weeks. Brice and McDonough (1973) proposed that the solar UV/EUV heating for Jupiter's upper atmosphere causes enhancement of total flux density. If such a process occurs at Jupiter, it is also expected that diurnal wind system produces dawn-dusk asymmetry of the JSR brightness distribution. Preceding studies confirmed that the short term variations in total flux density correspond to the solar UV/EUV. However, the effect of solar UV/EUV heating on the brightness distribution has not been confirmed. Hence, the purpose of this study is to confirm the solar UV/EUV heating effect on total flux density and brightness distribution. We made radio imaging analysis using the National Radio Astronomy Observatory (NRAO) archived data of the Very Large Array (VLA) obtained in 2000, and following results were shown. 1, Total flux density varied corresponding to the solar UV/EUV. 2, Dawn side emission was brighter than dusk side emission almost every day. 3, Variations of the dawn-dusk asymmetry did not correspond to the solar UV/EUV. In order to explain the second result, we estimate the diurnal wind velocity from the observed dawn-dusk ratio by using the model brightness distribution of JSR. Estimated neutral wind velocity is 46+/-11 m/s, which reasonably corresponds to the numerical simulation of Jupiter's upper atmosphere. In order to explain the third result, we examined the effect of the global convection electric field driven by tailward outflow of plasma in Jupiter's magnetosphere. As the result, it is suggested that typical fluctuation of the convection electric field strength was enough to cause the observed variations of the dawn-dusk asymmetry.

Galileo view of Moon orbiting the Earth taken from 3.9 million miles

NASA Image and Video Library

1992-12-16

Eight days after its encounter with the Earth, the Galileo spacecraft was able to look back and capture this remarkable view of the Moon in orbit about the Earth, taken from a distance of about 6.2 million kilometers (3.9 million miles). The picture was constructed from images taken through the violet, red, and 1.0-micron infrared filters. The Moon is in the foreground, moving from left to right. The brightly-colored Earth contrasts strongly with the Moon, which reflects only about one-third as much sunlight as the Earth. Contrast and color have been computer-enhanced for both objects to improve visibility. Antarctica is visible through clouds (bottom). The Moon's far side is seen; the shadowy indentation in the dawn terminator is the south-Pole/Aitken Basin, one of the largest and oldest lunar impact features. Alternate Jet Propulsion Laboratory (JPL) number is P-41508. View appears in the Space News Roundup v32 n1 p1, 01-11-93.

Dawn-dusk asymmetry induced by the Parker spiral angle in the plasma dynamics around comet 67P/Churyumov-Gerasimenko

NASA Astrophysics Data System (ADS)

Behar, E.; Tabone, B.; Nilsson, H.

2018-05-01

When interacting, the solar wind and the ionised atmosphere of a comet exchange energy and momentum. Our aim is to understand the influence of the average Parker spiral configuration of the solar wind magnetic field on this interaction. We compare the theoretical expectations of an analytical generalised gyromotion with Rosetta observations at comet 67P/Churyumov-Gerasimenko. A statistical approach allows one to overcome the lack of upstream solar wind measurement. We find that additionally to their acceleration along (for cometary pick-up ions) or against (for solar wind ions) the upstream electric field orientation and sense, the cometary pick-up ions are drifting towards the dawn side of the coma, while the solar wind ions are drifting towards the dusk side of the coma, independent of the heliocentric distance. The dynamics of the interaction is not taking place in a plane, as often assumed in previous works.

Dawn HAMO Image 70

NASA Image and Video Library

2015-12-04

This view from NASA's Dawn spacecraft shows different types of terrain located side by side on Ceres: a smooth terrain at right with numerous small impact craters, and a less-cratered, hummocky terrain at left. A huge crater chain crosses the scene diagonally from upper left to lower right. The smooth terrain, which is in the western part of Yalode impact basin, is interrupted by a set of roughly parallel furrows and ridges at upper right. These linear features are perpendicular to another set of smaller, fainter linear markings, which appear just below them. An impact into the hummocky terrain formed a crater, seen at left, 14 miles (22 kilometers) in diameter with a central peak. A great deal of material has slumped down the walls of the crater -- a phenomenon called mass wasting. The crater's impact ejecta forms a smooth blanket around its rim, which takes on a streaky texture leading away from the crater toward lower right. The image was taken during in Dawn's High Altitude Mapping Orbit (HAMO) phase from an altitude of 911 miles (1,466 kilometers) on Oct. 6, 2015. Image resolution is 394 feet (120 meters) per pixel. The image is centered at 37 degrees south latitude, 279 degrees east longitude. http://photojournal.jpl.nasa.gov/catalog/PIA20133

Ionosphere of Venus - First observations of the dayside ion composition near dawn and dusk

NASA Technical Reports Server (NTRS)

Taylor, H. A., Jr.; Brinton, H. C.; Bauer, S. J.; Hartle, R. E.; Donahue, T. M.; Cloutier, P. A.; Michel, F. C.; Daniell, R. E., Jr.; Blackwell, B. H.

1979-01-01

Independent Bennett radio-frequency ion mass spectrometers on the Pioneer Venus bus and orbiter spacecraft obtained in situ measurements of the composition of the ionosphere of Venus. The spectrometer on the bus explored the dawn region while the spectrometer on the orbiter explored the duskside region. Information on the ion composition in the topside, the lower ionosphere, and the upper ionosphere is presented. Below the O(+) peak near 200 km, the ions are found to exhibit scale heights consistent with a neutral gas temperature of about 180 K near the terminator. In the upper ionosphere, scale heights of all species reflect the effects of plasma transport.

Ahuna Mons: Side View

NASA Image and Video Library

2016-09-01

Ceres' lonely mountain, Ahuna Mons, is seen in this simulated perspective view. The elevation has been exaggerated by a factor of two. The view was made using enhanced-color images from NASA's Dawn mission. Images taken using blue (440 nanometers), green (750 nanometers) and infrared (960 nanometers) spectral filters were combined to create the view. The spacecraft's framing camera took the images from Dawn's low-altitude mapping orbit, from an altitude of 240 miles (385 kilometers) in August 2016. The resolution of the component images is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20915

Oxo Crater: Side View

NASA Image and Video Library

2016-09-01

Ceres' lonely mountain, Ahuna Mons, is seen in this simulated perspective view. The elevation has been exaggerated by a factor of two. The view was made using enhanced-color images from NASA's Dawn mission. Images taken using blue (440 nanometers), green (750 nanometers) and infrared (960 nanometers) spectral filters were combined to create the view. The spacecraft's framing camera took the images from Dawn's low-altitude mapping orbit, from an altitude of 240 miles (385 kilometers) in August 2016. The resolution of the component images is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20915

The Magnetic Local Time Distribution of Energetic Electrons in the Radiation Belt Region

NASA Astrophysics Data System (ADS)

Allison, H. J.

2017-12-01

Using fourteen years of electron flux data from the National Oceanic and Atmospheric Administration Polar Operational Environmental Satellites (POES), a statistical study of the magnetic local time (MLT) distribution of the electron population is performed across a range of activity levels, defined by AE, AE*, Kp, solar wind velocity (Vsw), and VswBz. Three electron energies (>30, >100, and >300 keV) are considered. Dawn-dusk flux asymmetries larger than order of magnitude were observed for >30 and >100 keV electrons. For >300 keV electrons, dawn-dusk asymmetries were primarily due to a decrease in the average dusk-side flux beyond L* ˜ 4.5 that arose with increasing activity. For the >30 keV population, substorm injections enhance the dawn-side flux, which may not reach the dusk-side as the electrons can be on open drift paths and lost to the magnetopause. The asymmetries in the >300 keV population are attributed to the combination of magnetopause shadowing and >300 keV electron injections by large electric fields. We suggest that 3D radiation belt models could set the minimum energy boundary (Emin) to 30 keV or above at L* ˜6 during periods of low activity. However, for more moderate conditions, Emin should be larger than 100 keV and, for very extreme activities, ˜300 keV. Our observations show the extent that in-situ electron flux readings may vary during active periods due to the MLT of the satellite and highlight the importance of 4D radiation belt models to fully understand radiation belt processes.

Topographic View of Ceres Mountain

NASA Image and Video Library

2015-09-30

This view, made using images taken by NASA's Dawn spacecraft, features a tall conical mountain on Ceres. Elevations span a range of about 5 miles (8 kilometers) from the lowest places in this region to the highest terrains. Blue represents the lowest elevation, and brown is the highest. The white streaks seen running down the side of the mountain are especially bright parts of the surface. The image was generated using two components: images of the surface taken during Dawn's High Altitude Mapping Orbit (HAMO) phase, where it viewed the surface at a resolution of about 450 feet (140 meters) per pixel, and a shape model generated using images taken at varying sun and viewing angles during Dawn's lower-resolution Survey phase. The image of the region is color-coded according to elevation, and then draped over the shape model to give this view. http://photojournal.jpl.nasa.gov/catalog/PIA19976

Dark Material Associated with and between Craters

NASA Image and Video Library

2011-11-18

This image from NASA Dawn spacecraft shows areas of dark material which are both associated with impact craters and between these craters on asteroid Vesta. Dark material is seen cropping out of the rims and sides of the larger craters.

Application of a global magnetospheric-ionospheric current model for dayside and terminator Pi2 pulsations

NASA Astrophysics Data System (ADS)

Imajo, S.; Yoshikawa, A.; Uozumi, T.; Ohtani, S.; Nakamizo, A.; Chi, P. J.

2017-12-01

Pi2 magnetic oscillations on the dayside are considered to be produced by the ionospheric current that is driven by Pi2-associated electric fields from the high-latitude region, but this idea has not been quantitatively tested. The present study numerically tested the magnetospheric-ionospheric current system for Pi2 consisting of field-aligned currents (FACs) localized in the nightside auroral region, the perpendicular magnetospheric current flowing in the azimuthal direction, and horizontal ionospheric currents driven by the FACs. We calculated the spatial distribution of the ground magnetic field produced by these currents using the Biot-Savart law in a stationary state. The calculated magnetic field reproduced the observational features reported by previous studies; (1) the sense of the H component does not change a wide range of local time sectors at low latitudes; (2) the amplitude of the H component on the dayside is enhanced at the equator; (3) The D component reverses its phase near the dawn and dusk terminators; (4) the meridian of the D-component phase reversal near the dusk terminator is shifted more sunward than that near the dawn terminator; (5) the amplitude of the D component in the morning is larger than that in the early evening. We also derived the global distributions of observed equivalent currents for two Pi2 events. The spatial patterns of dayside equivalent currents were similar to the spatial pattern of numerically derived equivalent currents. The results indicate that the oscillation of the magnetospheric-ionospheric current system is a plausible explanation of Pi2s on the dayside and near the terminator. These results are included in an accepted paper by Imajo et al. [2017JGR, DOI: 10.1002/2017JA024246].

A statistical study of ion pitch-angle distributions

NASA Technical Reports Server (NTRS)

Sibeck, D. G.; Mcentire, R. W.; Lui, A. T. Y.; Krimigis, S. M.

1987-01-01

Preliminary results of a statistical study of energetic (34-50 keV) ion pitch-angle distributions (PADs) within 9 Re of earth provide evidence for an orderly pattern consistent with both drift-shell splitting and magnetopause shadowing. Normal ion PADs dominate the dayside and inner magnetosphere. Butterfly PADs typically occur in a narrow belt stretching from dusk to dawn through midnight, where they approach within 6 Re of earth. While those ion butterfly PADs that typically occur on closed drift paths are mainly caused by drift-shell splitting, there is also evidence for magnetopause shadowing in observations of more frequent butterfly PAD occurrence in the outer magnetosphere near dawn than dusk. Isotropic and gradient boundary PADs terminate the tailward extent of the butterfly ion PAD belt.

Magnetotail Structure and its Internal Particle Dynamics During Northward IMF

NASA Technical Reports Server (NTRS)

Ashour-Abdalla, M.; Raeder, J.; El-Alaoui, M.; Peroomian, V.

1998-01-01

This study uses Global magnetohydrodynamic (MHD) simulations driven by solar wind data along with Geotail observations of the magnetotail to investigate the magnetotail's response to changes in the interplanetary magnetic field (IMF); observed events used in the study occurred on March 29, 1993 and February 9, 1995. For events from February 9, 1995, we also use the time-dependent MHD magnetic and electric fields and the large-scale kinetic (LSK) technique to examine changes in the Geotail ion velocity distributions. Our MHD simulation shows that on March 29, 1993, during a long period of steady northward IMF, the tail was strongly squeezed and twisted around the Sun-Earth axis in response to variations in the IMF B(sub y) component. The mixed (magnetotail and magnetosheath) plasma observed by Geotail results from the spacecraft's close proximity to the magnetopause and its frequent crossings of this boundary. In our second example (February 9, 1995) the IMF was also steady and northward, and in addition had a significant B(sub y) component. Again the magnetotail was twisted, but not as strongly as on March 29, 1993. The Geotail spacecraft, located approximately 30 R(sub E) downtail, observed highly structured ion distribution functions. Using the time-dependent LSK technique, we investigate the ion sources and acceleration mechanisms affecting the Geotail distribution functions during this interval. At 1325 UT most ions are found to enter the magnetosphere on the dusk side earthward of Geotail with a secondary source on the dawn side in the low latitude boundary layer (LLBL). A small percentage come from the ionosphere. By 1347 UT the majority of the ions come from the dawn side LLBL. The distribution functions measured during the later time interval are much warmer, mainly because particles reaching the spacecraft from the dawn side are affected by nonadiabatic scattering and acceleration in the neutral sheet.

Dawn Mission: A Journey in Space and Time

NASA Technical Reports Server (NTRS)

Russell, C. T.; Coradini, A.; DeSanctis, M. C.; Feldman, W. C.; Jaumann, R.; Konopliv, A. S.; McCord, T. B.; McFadden, L. A.; McSween, H. Y.; Mottola, S.

2003-01-01

By successively orbiting both 4 Vesta and 1 Ceres the Dawn mission directly addresses the longstanding goals of NASA and the planetary community to understand the origin and evolution of the solar system by obtaining geophysical and geochemical data on diverse main belt asteroids. Ceres and Vesta are two complementary terrestrial protoplanets (one apparently "wet" and one "dry"), whose accretion was terminated by the formation of Jupiter. Ceres is little changed since it formed in the early solar system, while Vesta has experienced significant heating and differentiation. Both have remained intact over the age of the solar system, thereby retaining a record of events and processes from the time of planet formation. Detailed study of the geophysics and geochemistry of these two bodies provides critical benchmarks for the early solar system conditions and processes that shaped its subsequent evolution. Dawn provides the missing context for both primitive and evolved meteoritic data, thus playing a central role in understanding terrestrial planet formation and the evolution of the asteroid belt. Dawn is to be launched in May 2006 arriving at Vesta in 2010 and Ceres in 2014, stopping at each to make 11 months of orbital measurements. The spacecraft uses solar electric propulsion both in cruise and in orbit to make most efficient use of its xenon propellant. The spacecraft carries a framing camera, visible and infrared mapping spectrometer, gamma ray/neutron spectrometer, a laser altimeter, magnetometer, and radio science.

Radial and azimuthal distribution of Io's oxygen neutral cloud observed by Hisaki/EXCEED

NASA Astrophysics Data System (ADS)

Koga, R.; Tsuchiya, F.; Kagitani, M.; Sakanoi, T.; Yoneda, M.; Yoshikawa, I.; Yoshioka, K.; Murakami, G.; Yamazaki, A.; Kimura, T.; Smith, H. T.

2017-12-01

We report the spatial distributions of oxygen neural cloud surrounding Jupiter's moon Io and along Io's orbit observed by the HISAKI satellite. Atomic oxygen and sulfur in Io's atmosphere escape from the exobase and move to corona (< 5.8 Io radii, the boundary where Jupiter's gravity begins to dominate) and neutral clouds (> 5.8 Io radii) mainly due to atmospheric sputtering. Io plasma torus is formed by ionization of these atoms by electron impact and charge exchange processes. It is essential to examine the dominant source of Io plasma torus, particularly in the vicinity of Io (<5.8 Io radii; atmosphere and corona) or the region away from Io (>5.8 Io radii; extended neutral clouds). The spatial distribution of oxygen and sulfur neutral clouds is important to understand the source. The extreme ultraviolet spectrometer called EXCEED (Extreme Ultraviolet Spectroscope for Exospheric Dynamics) installed on the Hisaki satellite observed Io plasma torus continuously in 2014-2015, and we carried out the monitoring of the distribution of atomic oxygen emission at 130.4 nm. The emission averaged over the distance range of 4.5-6.5 Jovian radii on the dawn and dusk sides strongly depends on the Io phase angle (IPA), and has a emission peak between IPA of 60-90 degrees on the dawn side, and between 240-270 degrees on the dusk side, respectively. It also shows the asymmetry with respect to Io's position: the intensity averaged for IPA 60-90 degrees (13.3 Rayleighs (R)) is 1.2 times greater than that for IPA 90-120 degrees (11.1 R) on the dawn side. The similar tendency is found on the dusk side. Weak atomic oxygen emission (4 R) uniformly distributes in every IPA. We also examined the radial distribution of the oxygen neutral cloud during the same period and found the emission peak near Io's orbit with decreasing the intensity toward 8.0 Jupiter radii. The results show the high density component of the oxygen neutral cloud is concentrated around Io and extends mainly toward leading side of Io. In addition, the low density neutrals uniformly exist along Io's orbit. Both components extend radially outward up to 8 Jovian radii with decreasing the density. In the presentation, we give the estimation of spatial distribution of oxygen neutral density and the oxygen ion source rate in the Io plasma torus.

Intrinsic Dawn-Dusk Asymmetry of Magnetotail Thin Current Sheet

NASA Astrophysics Data System (ADS)

Lu, S.; Pritchett, P. L.; Angelopoulos, V.; Artemyev, A.

2017-12-01

Magnetic reconnection and its related phenomena (flux ropes, dipolarization fronts, bursty bulk flows, particle injections, etc.) occur more frequently on the duskside in the Earth's magnetotail. Magnetohydrodynamic simulations attributed the asymmetry to the nonuniform ionospheric conductance through global scale magnetosphere-ionosphere interaction. Hybrid simulations, on the other hand, found an alternative responsible mechanism: the Hall effect in the magnetotail thin current sheet, but left an open question: What is the physical origin of the asymmetric Hall effect? The answer could be the temperature difference on the two sides and/or the dawn-dusk transportation of magnetic flux and plasmas. In this work, we use 3-D particle-in-cell simulations to further explore the magnetotail dawn-dusk asymmetry. The magnetotail equilibrium contains a dipole magnetic field and a current sheet region. The simulation is driven by a symmetric and localized (in the y direction) high-latitude electric field, under which the current sheet thins with a decrease of Bz. During the same time, a dawn-dusk asymmetry is formed intrinsically in the thin current sheet, with a smaller Bz, a stronger Hall effect (indicated by the Hall electric field Ez), and a stronger cross-tail current jy on the duskside. The deep origin of the asymmetry is also shown to be dominated by the dawnward E×B drift of magnetic flux and plasmas. A direct consequence of this intrinsic dawn-dusk asymmetry is that it favors magnetotail reconnection and related phenomena to preferentially occur on the duskside.

Observation of Neutral Sodium Above Mercury During the Transit of November 8, 2006

NASA Technical Reports Server (NTRS)

Potter, A. E.; Killen, R. M.; Reardon, Kevin P.; Bida, T. A.

2013-01-01

We mapped the absorption of sunlight by sodium vapor in the exosphere of Mercury during the transit of Mercury on November 8, 2006, using the IBIS Interferometric BIdimensional Spectrometer at the Dunn Solar Telescope operated by the National Solar Observatory at Sunspot, New Mexico. The measurements were reduced to line-of-sight equivalent widths for absorption at the sodium D2 line around the shadow of Mercury. The sodium absorption fell off exponentially with altitude up to about 600 km. However there were regions around north and south polar-regions where relatively uniform sodium absorptions extended above 1000 km. We corrected the 0-600 km altitude profiles for seeing blur using the measured point spread function. Analysis of the corrected altitude distributions yielded surface densities, zenith column densities, temperatures and scale heights for sodium all around the planet. Sodium absorption on the dawn side equatorial terminator was less than on the dusk side, different from previous observations of the relative absorption levels. We also determined Earthward velocities for sodium atoms, and line widths for the absorptions. Earthward velocities resulting from radiation pressure on sodium averaged 0.8 km/s, smaller than a prediction of 1.5 km/s. Most line widths were in the range of 20 mA after correction for instrumental broadening, corresponding to temperatures in the range of 1000 K.

Does Solar Wind also Drive Convection in Jupiter's Magnetosphere?

NASA Astrophysics Data System (ADS)

Khurana, K. K.

2001-05-01

Using a simple model of magnetic field and plasma velocity, Brice and Ioannidis [1970] showed that the corotation electric field exceeds convection electric field throughout the Jovian magnetosphere. Since that time it has been tacitly assumed that Jupiter's magnetosphere is driven from within. If Brice and Ioannidis conjecture is correct then one would not expect major asymmetries in the field and plasma parameters in the middle magnetosphere of Jupiter. Yet, new field and plasma observations from Galileo and simultaneous auroral observations from HST show that there are large dawn/dusk and day/night asymmetries in many magnetospheric parameters. For example, the magnetic observations show that a partial ring current and an associated Region-2 type field-aligned current system exist in the magnetosphere of Jupiter. In the Earth's magnetosphere it is well known that the region-2 current system is created by the asymmetries imposed by a solar wind driven convection. Thus, we are getting first hints that the solar wind driven convection is important in Jupiter's magnetosphere as well. Other in-situ observations also point to dawn-dusk asymmetries imposed by the solar wind. For example, first order anisotropies in the Energetic Particle Detector show that the plasma is close to corotational on the dawn side but lags behind corotation in the dusk sector. Magnetic field data show that the current sheet is thin and highly organized on the dawn side but thick and disturbed on the dusk side. I will discuss the reasons why Brice and Ioannidis calculation may not be valid. I will show that both the magnetic field and plasma velocity estimates used by Brice and Ioannidis were rather excessive. Using more modern estimates of the field and velocity values I show that the solar wind convection can penetrate as deep as 40 RJ on the dawnside. I will present a new model of convection that invokes in addition to a distant neutral line spanning the whole magnetotail, a near-Jupiter neutral line only on the dawnside. I will discuss how the internal and external drivers together set up a convection system and transport plasma and magnetic flux in Jupiter's magnetosphere. I will explore the consequences of this convection system on the flows, current sheet and the Jovian aurorae.

NASA's Dawn Mission to Asteroid 4 Vesta

NASA Technical Reports Server (NTRS)

McFadden, Lucyann A.

2011-01-01

NASA's Dawn Mission to asteroid 4 Vesta is part of a 13-year robotic space project designed to reveal the nature of two of the largest asteroids in the Main Asteroid Belt of our Solar System. Ceres and Vesta are two complementary terrestrial protoplanets whose accretion was probably terminated by the formation of Jupiter. They provide a bridge in our understanding between the rocky bodies of the inner solar system and the icy bodies of the outer solar system. Ceres appears to be undifferentiated Vesta has experienced significant heating and likely differentiation. Both formed very early in history of the solar system and while suffering many impacts have remained intact, thereby retaining a record of events and processes from the time of planet formation. Detailed study of the geophysics and geochemistry of these two bodies provides critical benchmarks for early solar system conditions and processes that shaped its subsequent evolution. Dawn provides the missing context for both primitive and evolved meteoritic data, thus playing a central role in understanding terrestrial planet formation and the evolution of the asteroid belt. Dawn is to he launched in 2006 arriving at Vesta in 20l0 and Ceres in 2014, stopping at each to make 11 months of orbital measurements. The spacecraft uses solar electric propulsion, both in cruise and in orbit, to make most efficient use of its xenon propellant. The spacecraft carries a framing camera, visible and infrared mapping spectrometer, gamma ray/neutron magnetometer, and radio science.

KSC-07pd1598

NASA Image and Video Library

2007-06-20

KENNEDY SPACE CENTER, FLA. -- At Astrotech, the Dawn spacecraft is on display for a media showing. On each side are the folded solar array panels. The "box" in the upper center is the visual and infrared mapping spectrometer, which is designed to measure how much radiation of different "colors" is reflected or emitted by an object. At the bottom, under cover, is one of the ion propulsion thrusters. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/Kim Shiflett

Dawn 2013-2015 Double-sided Mission Events Calendar

NASA Image and Video Library

2007-01-01

The mosaic of Visible and Infrared Spectrometer (VIR) data shows the location of the data acquired by VIR during the HAMO (high-altitude mapping orbit) phase of NASA's Dawn mission. VIR can image Vesta in a number of different wavelengths of light, ranging from the visible to the infrared part of the electromagnetic spectrum. This mosaic shows the images taken at a wavelength of 550 nanometers, which is in the visible part of the electromagnetic spectrum. During HAMO VIR obtained more than 4.6 million spectra of Vesta. It is clear from this image that the VIR observations are widely distributed across Vesta, which results in a global view of the spectral properties of Vesta's surface. http://photojournal.jpl.nasa.gov/catalog/PIA19368

The Role of the Upper Atmosphere for Dawn-Dusk and Interhemispheric Differences in the Coupled Magnetosphere-Ionosphere-Thermosphere System

NASA Astrophysics Data System (ADS)

Foerster, M.; Doornbos, E.; Haaland, S.

2016-12-01

Solar wind and IMF interaction with the geomagnetic field sets up a large-scale plasma circulation in the Earth's magnetosphere and the magnetically tightly connected ionosphere. The ionospheric ExB ion drift at polar latitudes accelerates the neutral gas as a nondivergent momentum source primarily in force balance with pressure gradients, while the neutral upper thermosphere circulation is essentially modified by apparent forces due to Earth's rotation (Coriolis and centrifugal forces) as well as advection and viscous forces. The apparent forces affect the dawn and dusk side asymmetrically, favouring a large dusk-side neutral wind vortex, while the non-dipolar portions of the Earth's magnetic field constitute significant hemispheric differences in magnetic flux and field configurations that lead to essential interhemispheric differences of the ion-neutral interaction. We present statistical studies of both the high-latitude ionospheric convection and the upper thermospheric circulation patterns based on measurements of the electron drift instrument (EDI) on board the Cluster satellites and by the accelerometer on board the CHAMP, GOCE, and Swarm spacecraft, respectively.

Electric drive systems including smoothing capacitor cooling devices and systems

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

Dede, Ercan Mehmet; Zhou, Feng

An electric drive system includes a smoothing capacitor including at least one terminal, a bus bar electrically coupled to the at least one terminal, a thermoelectric device including a first side and a second side positioned opposite the first side, where the first side is thermally coupled to at least one of the at least one terminal and the bus bar, and a cooling element thermally coupled to the second side of the thermoelectric device, where the cooling element dissipates heat from the thermoelectric device.

Observation of relativistic electron loss induced by EMIC waves in the outer radiation belt: Arase and PWING induction magnetometer array collaboration

NASA Astrophysics Data System (ADS)

Kurita, S.; Yoshizumi, M.; Kazuo, S.; Higashio, N.; Mitani, T.; Takashima, T.; Matsuoka, A.; Teramoto, M.; Shinohara, I.

2017-12-01

EMIC waves are generated by temperature anisotropy of energetic ions near the magnetic equator and satellite observations show that the waves tend to be observed on the dusk side and noon side magnetosphere. EMIC waves can propagate from the magnetosphere to the ground and they are observed by ground-based magnetometers as Pc1 pulsation. It has been pointed out that EMIC waves can resonate with relativistic electrons through anomalous cyclotron resonance, and cause strong pitch angle scattering of radiation belt electrons. It has been considered that precipitation loss of relativistic electrons by pitch angle scattering induced by EMIC waves is an important loss mechanism of radiation belt electrons. We report on the observation of relativistic electron loss observed by the Arase satellite on the dawn side magnetosphere during a geomagnetic disturbance, which is likely to be related to an EMIC wave activity. During the event, the EMIC wave activity in conjunction with the relativistic electron loss is identified from observation by the ground-based induction magnetometer array deployed by the PWING project. The magnetometer array observation reveals that EMIC waves are distributed in the wide magnetic local time range from the dusk to midnight sector. It is suggested that drifting relativistic electrons are scattered into the loss cone by the EMIC waves on the dusk to midnight sector before they arrive at the Arase satellite located on the dawn side. We will discuss the impact of loss caused by EMIC wave-induced precipitation loss on the overall flux variation of radiation belt electrons during the geomagnetic disturbance.

Turbulence in a Global Magnetohydrodynamic Simulation of the Earth's Magnetosphere during Northward and Southward Interplanetary Magnetic Field

NASA Technical Reports Server (NTRS)

El-Alaoui, M.; Richard, R. L.; Ashour-Abdalla, M.; Walker, R. J.; Goldstein, M. L.

2012-01-01

We report the results of MHD simulations of Earth's magnetosphere for idealized steady solar wind plasma and interplanetary magnetic field (IMF) conditions. The simulations feature purely northward and southward magnetic fields and were designed to study turbulence in the magnetotail plasma sheet. We found that the power spectral densities (PSDs) for both northward and southward IMF had the characteristics of turbulent flow. In both cases, the PSDs showed the three scale ranges expected from theory: the energy-containing scale, the inertial range, and the dissipative range. The results were generally consistent with in-situ observations and theoretical predictions. While the two cases studied, northward and southward IMF, had some similar characteristics, there were significant differences as well. For southward IMF, localized reconnection was the main energy source for the turbulence. For northward IMF, remnant reconnection contributed to driving the turbulence. Boundary waves may also have contributed. In both cases, the PSD slopes had spatial distributions in the dissipative range that reflected the pattern of resistive dissipation. For southward IMF there was a trend toward steeper slopes in the dissipative range with distance down the tail. For northward IMF there was a marked dusk-dawn asymmetry with steeper slopes on the dusk side of the tail. The inertial scale PSDs had a dusk-dawn symmetry during the northward IMF interval with steeper slopes on the dawn side. This asymmetry was not found in the distribution of inertial range slopes for southward IMF. The inertial range PSD slopes were clustered around values close to the theoretical expectation for both northward and southward IMF. In the dissipative range, however, the slopes were broadly distributed and the median values were significantly different, consistent with a different distribution of resistivity.

Magnetotail Fast Flow Occurrence Rate and Dawn-Dusk Asymmetry at XGSM ˜ -60 RE

NASA Astrophysics Data System (ADS)

Kiehas, S. A.; Runov, A.; Angelopolos, V.; Hietala, H.; Korovinksiy, D.

2018-03-01

As a direct result of magnetic reconnection, plasma sheet fast flows act as primary transporter of mass, flux, and energy in the Earth's magnetotail. During the last decades, these flows were mainly studied within XGSM>-60RE, as observations near or beyond lunar orbit were limited. By using 5 years (2011-2015) of ARTEMIS (Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moons Interaction with the Sun) data, we statistically investigate earthward and tailward flows at around 60 RE downtail. A significant fraction of fast flows is directed earthward, comprising 43% (vx>400 km/s) to 56% (vx>100 km/s) of all observed flows. This suggests that near-Earth and midtail reconnection are equally probable of occurring on either side of the ARTEMIS downtail distance. For fast convective flows (v⊥x>400 km/s), this fraction of earthward flows is reduced to about 29%, which is in line with reconnection as source of these flows and a downtail decreasing Alfvén velocity. More than 60% of tailward convective flows occur in the dusk sector (as opposed to the dawn sector), while earthward convective flows are nearly symmetrically distributed between the two sectors for low AL (>-400 nT) and asymmetrically distributed toward the dusk sector for high AL (<-400 nT). This indicates that the dawn-dusk asymmetry is more pronounced closer to Earth and moves farther downtail during high geomagnetic activity. This is consistent with similar observations pointing to the asymmetric nature of tail reconnection as the origin of the dawn-dusk asymmetry of flows and other related observables. We infer that near-Earth reconnection is preferentially located at dusk, whereas midtail reconnection (X >- 60RE) is likely symmetric across the tail during weak substorms and asymmetric toward the dusk sector for strong substorms, as the dawn-dusk asymmetric nature of reconnection onset in the near-Earth region progresses downtail.

Large-scale irregularities of the winter polar topside ionosphere according to data from Swarm satellites

NASA Astrophysics Data System (ADS)

Lukianova, R. Yu.; Bogoutdinov, Sh. R.

2017-11-01

An analysis of the electron density measurements ( Ne) along the flyby trajectories over the high-latitude region of the Northern Hemisphere under winter conditions in 2014 and 2016 has shown that the main large-scale structure observed by Swarm satellites is the tongue of ionization (TOI). At the maximum of the solar cycle ( F 10.7 = 160), the average value of Ne in the TOI region at an altitude of 500 km was 8 × 104 cm-3. Two years later, at F 10.7 = 100, Ne 5 × 104 cm-3 and Ne 2.5 × 104 cm-3 were observed at altitudes of 470 and 530 km, respectively. During the dominance of the azimuthal component of the interplanetary magnetic field, the TOI has been observed mainly on the dawn or dusk side depending on the sign of B y . Simultaneous observations of the convective plasma drift velocity in the polar cap show the transpolar flow drift to the dawn ( B y < 0) or dusk side ( B y < 0). Observations and numerical simulation of the Ne distribution have confirmed the significant role of the electric field of the magnetospheric convection in the generation of large-scale irregularities in the polar ionosphere.

Structural and dynamic properties of the C-terminal region of the Escherichia coli RNA chaperone Hfq: integrative experimental and computational studies.

PubMed

Wen, Bin; Wang, Weiwei; Zhang, Jiahai; Gong, Qingguo; Shi, Yunyu; Wu, Jihui; Zhang, Zhiyong

2017-08-09

In Escherichia coli, hexameric Hfq is an important RNA chaperone that facilitates small RNA-mediated post-transcriptional regulation. The Hfq monomer consists of an evolutionarily conserved Sm domain (residues 1-65) and a flexible C-terminal region (residues 66-102). It has been recognized that the existence of the C-terminal region is important for the function of Hfq, but its detailed structural and dynamic properties remain elusive due to its disordered nature. In this work, using integrative experimental techniques, such as nuclear magnetic resonance spectroscopy and small-angle X-ray scattering, as well as multi-scale computational simulations, new insights into the structure and dynamics of the C-terminal region in the context of the Hfq hexamer are provided. Although the C-terminal region is intrinsically disordered, some residues (83-86) are motionally restricted. The hexameric core may affect the secondary structure propensity of the C-terminal region, due to transient interactions between them. The residues at the rim and the proximal side of the core have significantly more transient contacts with the C-terminal region than those residues at the distal side, which may facilitate the function of the C-terminal region in the release of double-stranded RNAs and the cycling of small non-coding RNAs. Structure ensembles constructed by fitting the experimental data also support that the C-terminal region prefers to locate at the proximal side. From multi-scale simulations, we propose that the C-terminal region may play a dual role of steric effect (especially at the proximal side) and recruitment (at the both sides) in the binding process of RNA substrates. Interestingly, we have found that these motionally restricted residues may serve as important binding sites for the incoming RNAs that is probably driven by favorable electrostatic interactions. These integrative studies may aid in our understanding of the functional role of the C-terminal region of Hfq.

Pre-dawn stomatal opening does not substantially enhance early-morning photosynthesis in Helianthus annuus.

PubMed

Auchincloss, Lisa; Easlon, Hsien M; Levine, Diedre; Donovan, Lisa; Richards, James H

2014-06-01

Most C3 plant species have partially open stomata during the night especially in the 3-5 h before dawn. This pre-dawn stomatal opening has been hypothesized to enhance early-morning photosynthesis (A) by reducing diffusion limitations to CO2 at dawn. We tested this hypothesis in cultivated Helianthus annuus using whole-shoot gas exchange, leaf level gas exchange and modelling approaches. One hour pre-dawn low-humidity treatments were used to reduce pre-dawn stomatal conductance (g). At the whole-shoot level, a difference of pre-dawn g (0.40 versus 0.17 mol m(-2) s(-1)) did not significantly affect A during the first hour after dawn. Shorter term effects were investigated with leaf level gas exchange measurements and a difference of pre-dawn g (0.10 versus 0.04 mol m(-2) s(-1)) affected g and A for only 5 min after dawn. The potential effects of a wider range of stomatal apertures were explored with an empirical model of the relationship between A and intercellular CO2 concentration during the half-hour after dawn. Modelling results demonstrated that even extremely low pre-dawn stomatal conductance values have only a minimal effect on early-morning A for a few minutes after dawn. Thus, we found no evidence that pre-dawn stomatal opening enhances A.

Distinct sources of injections in the polar cusp observed by Cluster

NASA Astrophysics Data System (ADS)

Escoubet, C. Philippe; Reme, Henri; Dunlop, Malcolm; Daly, Patrick; Laakso, Harri; Berchem, Jean; Richard, Robert; Taylor, Matthew; Trattner, Karlheinz; Grison, Benjamin; Dandouras, Iannis; Fazakerley, Andrew; Pitout, Frederic; Masson, Arnaud

The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process takes place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s and the density around 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions in the dispersions, we obtain an altitude of the sources of these ions between 14 and 20 RE. Using Tsyganenko model, these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 10 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere.

New simulation of QSO X-ray heating during the Cosmic Dawn

NASA Astrophysics Data System (ADS)

Ross, Hannah E.; Dixon, Keri; Iliev, Ilian; Mellema, Garrelt

2018-05-01

The upcoming radio interferometer Square Kilometre Array is expected to directly detect the redshifted 21-cm signal from the Cosmic Dawn for the first time. In this era temperature fluctuations from X-ray heating of the neutral intergalactic medium can impact this signal dramatically. Previously, in Ross et al. (2017), we presented the first large-volume, 244 h-1 Mpc=349 Mpc a side, fully numerical radiative transfer simulations of X-ray heating. This work is a follow-up where we now also consider QSO-like sources in addition to high mass X-ray binaries. Images of the two cases are clearly distinguishable at SKA1-LOW resolution and have RMS fluctuations above the expected noise. The inclusion of QSOs leads to a dramatic increase in non-Gaussianity of the signal, as measured by the skewness and kurtosis of the 21-cm signal. We conclude that this increased non-Gaussianity is a promising signature of early QSOs.

DAWN: Dynamic Ad-hoc Wireless Network

DTIC Science & Technology

2016-06-19

DAWN: Dynamic Ad-hoc Wireless Network The DAWN (Dynamic Ad-hoc Wireless Networks) project is developing a general theory of complex and dynamic... wireless communication networks. To accomplish this, DAWN adopts a very different approach than those followed in the past and summarized above. DAWN... wireless communication networks. The members of DAWN investigated difference aspects of wireless mobile ad hoc networks (MANET). The views, opinions and/or

Evolution of convection vortices associated with sudden impulses observed by SuperDARN

NASA Astrophysics Data System (ADS)

Hori, T.; Shinbori, A.; Nishitani, N.; Fujita, S.

2014-12-01

Spatial evolution of transient ionospheric convection induced by sudden impulses (SIs) recorded by ground magnetometers is studied statistically by using SuperDARN (SD) data. An advantage of using SD data instead of ground magnetic fields is that ionospheric flows measured by the radars are not virtually biased by the spatially-varying ionospheric conductance or the magnetospheric currents. First we surveyed the Sym-H index for Jan., 2007 to Dec., 2012 to identify SI events with a peak amplitude |dSym-H| greater than 10 nT. Next we searched all SD data over the northern hemisphere during the SI events for ionospheric backscatters which give us the light-of-sight velocity of horizontal ionospheric flows. For each SI event, the collected ionospheric flow data were sorted into the four periods: the pre-SI period, the pre-Main Impulse (MI), middle-MI, and post-MI periods. In the present study, we examine the differences in flow velocity between the pre-SI period and the three MI periods to clarify how ionospheric flows change in association with SIs. As a result, the ionospheric flow shifts eastward on the dusk side and westward on the dawn side at the higher latitudes during positive SIs (SI+), while it shows a roughly westward/eastward shift on the dusk/dawn side, respectively, during negative SIs (SI-). These polarities of flow shifts are basically consistent with the higher latitude portions of the DP current for the MI phase as shown by Araki [1994] and Araki and Nagano [1988]. In terms of temporal evolution, the SI-induced transient flows remain slightly longer for SI- than for SI+. These findings suggest that the compression and expansion of the magnetosphere affect in different manners the magnetosphere-ionosphere coupled convection system.

What Drives Pakistan’s Interest in Afghanistan?

DTIC Science & Technology

2011-05-19

2010), 13. 172 Kamran Shafi, “Putting on a Brave Face and Standing Tall,” http://www.dawn.com/wps/wcm/connect/dawn-content-library/dawn/the-newspaper...columnists/ kamran -shafi- putting-on-a-brave-face-and-standing-tall-480 (accessed September 10, 2010). 59 include sanctuary, to militant...Shafi, Kamran . “Putting on a Brave Face and Standing Tall.” http://www.dawn.com/wps/wcm/connect/dawn-content-library/dawn/the- newspaper

Saturnian Dawn

NASA Image and Video Library

2017-06-26

NASA's Cassini spacecraft peers toward a sliver of Saturn's sunlit atmosphere while the icy rings stretch across the foreground as a dark band. This view looks toward the unilluminated side of the rings from about 7 degrees below the ring plane. The image was taken in green light with the Cassini spacecraft wide-angle camera on March 31, 2017. The view was obtained at a distance of approximately 620,000 miles (1 million kilometers) from Saturn. Image scale is 38 miles (61 kilometers) per pixel. https://photojournal.jpl.nasa.gov/catalog/PIA21334

Advances In Engineering Science, Volume 2.

DTIC Science & Technology

1976-11-01

UNDRAINED CLAY BEHAVIOR .... ............ .. 95 Jean-Herve Prevost and Kaare H~eg THEORY OF ORTHODONTIC MOTIONS...compo- nents at a lower level are terminal nodes of a tree. The bracketed numbers on the right hand side of the terminating nodes are the number of...primitive data objects in each instance of the defined object. The bracketed numbers on the right hand side of the non-terminal nodes in the tree are the

Left-sided incarcerated Amyand's hernia with cecum and terminal ileum: a case report.

PubMed

Bekele, Kebebe; Markos, Desalegn

2017-01-01

Amyand's hernia, which is the presence of a normal or pathological appendix as a part of an inguinal hernia, is a rare clinical entity. We are reporting a very rare case of left-sided incarcerated Amyand's hernia with cecum and terminal ileum involvement. A 4-year-old male child with left inguinal swelling of 2-year duration presented to Goba Referral Hospital. Two days before the patient visited our hospital, the swelling had become irreducible and caused severe groin pain. He had abdominal cramps, bilious vomiting, and mild abdominal distention, but passed feces. With the diagnosis of left-sided incarcerated inguinal hernia, the patient was investigated and prepared for surgical management. During the operative procedure, we identified the presence of appendix, cecum, and terminal ileum in the scrotum as the herniated component. After the sack was dissected, since there was also appendicitis, an appendectomy was performed. Then, high ligation of sack was done after cecum and ileum were reduced. After 3 uneventful postoperative days in the hospital, the patient was discharged. The patient was followed-up for 6 months, and he did not develop any complications. Left-sided incarcerated Amyand's hernia with cecum and terminal ileum involvement is a rare clinical entity. Even though it is not common, appendicitis is one of the comorbidities that can be seen in patients with left-sided incarcerated Amyand's hernia with cecum and terminal ileum. Surgeons should have a high index of clinical suspicion and be aware of the potential involvement of appendix, cecum, and ileum as part of an incarcerated hernia during surgery, even in the left inguinal region. In this case, left-sided incarcerated inguinal hernia which involved inflamed appendix, cecum, and terminal ileum was successfully managed using an inguinal approach.

Plasma Observations During the Mars Atmospheric Plume Event of March-April 2012

NASA Technical Reports Server (NTRS)

Andrews, D. J.; Barabash, S.; Edberg, N. J. T.; Gurnett, D. A.; Hall, B. E. S.; Holmstrom, M.; Lester, M.; Morgan, D. D.; Opgenoorth, H. J.; Ramstad, R.;

Degradation pattern of photosystem II reaction center protein D1 in intact leaves. The major photoinhibition-induced cleavage site in D1 polypeptide is located amino terminally of the DE loop.

PubMed

Kettunen, R; Tyystjärvi, E; Aro, E M

1996-08-01

Photoinhibition-induced degradation of the D1 protein of the photosystem II reaction center was studied in intact pumpkin (Cucurbita pepo L.) leaves. Photoinhibition was observed to cause the cleavage of the D1 protein at two distinct sites. The main cleavage generated an 18-kD N-terminal and a 20-kD C-terminal degradation fragment of the D1 protein. this cleavage site was mapped to be located clearly N terminally of the DE loop. The other, less-frequent cleavage occurred at the DE loop and produced the well-documented 23-kD, N-terminal D1 degradation product. Furthermore, the 23-kD, N-terminal D1 fragment appears to be phosphorylated and can be detected only under severe photoinhibition in vivo. Comparison of the D1 degradation pattern after in vivo photoinhibition to that after in vitro acceptor-side and donor-side photoinhibition, performed with isolated photosystem II core particles, gives indirect evidence in support of donor-side photoinhibition in intact leaves.

Asymmetric Kelvin-Helmholtz Instability at Jupiter's Magnetopause Boundary: Implications for Corotation-Dominated Systems

NASA Astrophysics Data System (ADS)

Zhang, B.; Delamere, P. A.; Ma, X.; Burkholder, B.; Wiltberger, M.; Lyon, J. G.; Merkin, V. G.; Sorathia, K. A.

2018-01-01

The multifluid Lyon-Fedder-Mobarry (MFLFM) global magnetosphere model is used to study the interactions between solar wind and rapidly rotating, internally driven Jupiter magnetosphere. The MFLFM model is the first global simulation of Jupiter magnetosphere that captures the Kelvin-Helmholtz instability (KHI) in the critically important subsolar region. Observations indicate that Kelvin-Helmholtz vortices are found predominantly in the dusk sector. Our simulations explain that this distribution is driven by the growth of KHI modes in the prenoon and subsolar region (e.g., >10 local time) that are advected by magnetospheric flows to the dusk sector. The period of density fluctuations at the dusk terminator flank (18 magnetic local time, MLT) is roughly 1.4 h compared with 7.2 h at the dawn flank (6 MLT). Although the simulations are only performed using parameters of the Jupiter's magnetosphere, the results may also have implications for solar wind-magnetosphere interactions at other corotation-dominated systems such as Saturn. For instance, the simulated average azimuthal speed of magnetosheath flows exhibit significant dawn-dusk asymmetry, consistent with recent observations at Saturn. The results are particularly relevant for the ongoing Juno mission and the analysis of dawnside magnetopause boundary crossings for other planetary missions.

Ionosphere of venus: first observations of the dayside ion composition near dawn and dusk.

PubMed

Taylor, H A; Brinton, H C; Bauer, S J; Hartle, R E; Donahue, T M; Cloutier, P A; Michel, F C; Daniell, R E; Blackwell, B H

1979-02-23

The first in situ measurements of the composition of the ionosphere of Venus are provided by independent Bennett radio-frequency ion mass spectrometers on the Pioneer Venus bits and orbiter spacecraft, exploring the dawn and duskside regions, respectively. An extensive composition of ion species, rich in oxygen, nitrogen, and carbon chemistry is idenitified. The dominant topside ion is O(+), with C(+), N(+), H(+), and He(+) as prominent secondary ions. In the lower ionosphere, the ionzization peak or F(1) layer near 150 kilometers reaches a concentration of about 5 x l0(3) ions per cubic centimeter, and is composed of the dominant molecular ion, O(2)(+), with NO(+), CO(+), and CO(2)(+), constituting less than 10 percent of the total. Below the O(+) peak near 200 kilometers, the ions exhibit scale heights consistent with a neutral gas temperature of about 180 K near the terminator. In the upper ionosphere, scale heights of all species reflect the effects of plasma transport, which lifts the composition upward to the often abrupt ionopause, or thermal ion boundary, which is observed to vary in height between 250 to 1800 kilometers, in response to solar wind dynamics.

Epithermal Neutron Evidence for a Diurnal Surface Hydration Process in the Moon's High Latitudes

NASA Technical Reports Server (NTRS)

McClanahan, T. P.; Mitrofanov, I. G.; Boynton, W. V.; Chin, G.; Parsons, A.; Starr, R. D.; Evans, L. G.; Sanin, A.; Litvak, M.; Livengood, T.

2015-01-01

We report evidence from epithermal neutron flux observations that show that the Moon's high latitude surfaces are being actively hydrated, dehydrated and rehydrated in a diurnal cycle. The near-surface hydration is indicated by an enhanced suppression of the lunar epithermal neutron leakage flux on the dayside of the dawn terminator on poleward-facing slopes (PFS). At 0600 to 0800 local-time, hydrogen concentrations within the upper 1 meter of PFS are observed to be maximized relative to equivalent equator-facing slopes (EFS). During the lunar day surface hydrogen concentrations diminish towards dusk and then rebuild overnight. Surface hydration is determined by differential comparison of the averaged EFS to PFS epithermal neutron count rates above +/- 75 deg latitude. At dawn the contrast bias towards PFS is consistent with at least 15 to 25 parts-per-million (ppm) hydrogen that dissipates by dusk. We review several lines of evidence derived from temperature and epithermal neutron data by a correlated analysis of observations from the Lunar Reconnaissance Orbiter's (LRO) Lunar Exploration Neutron Detector (LEND) that were mapped as a function of lunar local-time, Lunar Observing Laser Altimeter (LOLA) topography and Diviner (DLRE) surface temperature.

A Vortical Dawn Flank Boundary Layer for Near-Radial IMF: Wind Observations on 24 October 2001

NASA Technical Reports Server (NTRS)

Farrugia, C. J.; Gratton, F. T.; Gnavi, G.; Torbert, R. B.; Wilson, Lynn B., III

2014-01-01

We present an example of a boundary layer tailward of the dawn terminator which is entirely populated by rolled-up flow vortices. Observations were made by Wind on 24 October 2001 as the spacecraft moved across the region at the X plane approximately equal to -13 Earth radii. Interplanetary conditions were steady with a near-radial interplanetary magnetic field (IMF). Approximately 15 vortices were observed over the 1.5 hours duration of Wind's crossing, each lasting approximately 5 min. The rolling up is inferred from the presence of a hot tenuous plasma being accelerated to speeds higher than in the adjoining magnetosheath, a circumstance which has been shown to be a reliable signature of this in single-spacecraft observations. A blob of cold dense plasma was entrained in each vortex, at whose leading edge abrupt polarity changes of field and velocity components at current sheets were regularly observed. In the frame of the average boundary layer velocity, the dense blobs were moving predominantly sunward and their scale size along the X plane was approximately 7.4 Earth radii. Inquiring into the generation mechanism of the vortices, we analyze the stability of the boundary layer to sheared flows using compressible magnetohydrodynamic Kelvin-Helmholtz theory with continuous profiles for the physical quantities. We input parameters from (i) the exact theory of magnetosheath flow under aligned solar wind field and flow vectors near the terminator and (ii) the Wind data. It is shown that the configuration is indeed Kelvin-Helmholtz (KH) unstable. This is the first reported example of KH-unstable waves at the magnetopause under a radial IMF.

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In Astrotech's Payload Processing Facility, technicians help secure the Dawn spacecraft onto a moveable stand. Dawn will be moved into clean room C for unbagging and further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In Astrotech's Payload Processing Facility, an overhead crane lifts the Dawn spacecraft from its transporter. Dawn will be moved into clean room C for unbagging and further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C

DRUG ABUSE WARNING NETWORK (DAWN) DATABASE

EPA Science Inventory

The Drug Abuse Warning Network (DAWN) is an ongoing drug abuse data collection system sponsored by SAMHSA's Office of Applied Studies. DAWN collects data from: (1) hospital emergency departments (EDs) and (2) medical examiners (MEs). The DAWN ED component relies on a nationally r...

Arbitrary grammars generating context-free languages

NASA Technical Reports Server (NTRS)

Baker, B. S.

1972-01-01

If G is a grammar such that in each noncontext-free rule of G, the right side contains a string of terminals longer than any terminal string appearing between two nonterminals in the left side; then the language generated by G is context-free. Six previous results follow as simple corollaries of this theorem.

Observational test of shock drift and Fermi acceleration on a seed particle population upstream of earth's bow shock

NASA Technical Reports Server (NTRS)

Anagnostopoulos, G. C.; Sarris, E. T.; Krimigis, S. M.

1988-01-01

The efficiency of proposed shock acceleration mechanisms as they operate at the bow shock in the presence of a seed energetic particle population was examined using data from simultaneous observations of energetic solar-origin protons, carried out by the IMP 7 and 8 spacecraft in the vicinity of the quasi-parallel (dawn) and quasi-perpendicular (dusk) regions of the earth's bow shock, respectively. The results of observations (which include acceleration effects in the intensities of the energetic protons with energies as high as 4 MeV observed at the vicinity of the dusk bow shock, but no evidence for any particle acceleration at the energy equal to or above 50 keV at the dawn side of the bow shock) indicate that the acceleration of a seed particle population occurs only at the quasi-perpendicular bow shock through shock drift acceleration and that the major source of observed upstream ion populations is the leakage of magnetospheric ions of energies not less than 50 keV, rather than in situ acceleration.

Dawn Fields of View of Asteroid Vesta

NASA Image and Video Library

2007-01-01

This graphic from NASA's Dawn shows fields of view of Dawn instruments from Survey orbit (red), High Altitude Mapping Orbit (green), and Low Altitude Mapping Orbit (blue) and is part of the Mission Art series from NASA's Dawn mission. http://photojournal.jpl.nasa.gov/catalog/PIA19371

Mercury's Exosphere During MESSENGER's Second Flyby: Detection of Magnesium and Distinct Distributions of Neutral Species

NASA Technical Reports Server (NTRS)

McClintock, William E.; Vervack, Ronald J., Jr.; Bradley, E. Todd; Killen, Rosemary M.; Mouawad, Nelly; Sprague, Ann L.; Burger, Matthew H.; Solomon, Sean C.; Izenberg, Noam R.

2009-01-01

During MESSENGER's second Mercury flyby, the Mercury Atmospheric and Surface Composition Spectrometer observed emission from Mercury's neutral exosphere. These observations include the first detection of emission from magnesium. Differing spatial distributions for sodium, calcium, and magnesium were revealed by observations beginning in Mercury's tail region, approximately 8 Mercury radii anti-sunward of the planet, continuing past the nightside, and ending near the dawn terminator. Analysis of these observations, supplemented by observations during the first Mercury flyby as well as those by other MESSENGER instruments, suggests that the distinct spatial distributions arise from a combination of differences in source, transfer, and loss processes.

WAKE ISLAND AIRFIELD TERMINAL, BUILDING 1502 LOOKING EAST WITH PHOTO ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

WAKE ISLAND AIRFIELD TERMINAL, BUILDING 1502 LOOKING EAST WITH PHOTO SCALE CENTERED ON BUILDING (12/30/2008) - Wake Island Airfield, Terminal Building, West Side of Wake Avenue, Wake Island, Wake Island, UM

Coulomb repulsion in short polypeptides.

PubMed

Norouzy, Amir; Assaf, Khaleel I; Zhang, Shuai; Jacob, Maik H; Nau, Werner M

2015-01-08

Coulomb repulsion between like-charged side chains is presently viewed as a major force that impacts the biological activity of intrinsically disordered polypeptides (IDPs) by determining their spatial dimensions. We investigated short synthetic models of IDPs, purely composed of ionizable amino acid residues and therefore expected to display an extreme structural and dynamic response to pH variation. Two synergistic, custom-made, time-resolved fluorescence methods were applied in tandem to study the structure and dynamics of the acidic and basic hexapeptides Asp6, Glu6, Arg6, Lys6, and His6 between pH 1 and 12. (i) End-to-end distances were obtained from the short-distance Förster resonance energy transfer (sdFRET) from N-terminal 5-fluoro-l-tryptophan (FTrp) to C-terminal Dbo. (ii) End-to-end collision rates were obtained for the same peptides from the collision-induced fluorescence quenching (CIFQ) of Dbo by FTrp. Unexpectedly, the very high increase of charge density at elevated pH had no dynamical or conformational consequence in the anionic chains, neither in the absence nor in the presence of salt, in conflict with the common view and in partial conflict with accompanying molecular dynamics simulations. In contrast, the cationic peptides responded to ionization but with surprising patterns that mirrored the rich individual characteristics of each side chain type. The contrasting results had to be interpreted, by considering salt screening experiments, N-terminal acetylation, and simulations, in terms of an interplay of local dielectric constant and peptide-length dependent side chain charge-charge repulsion, side chain functional group solvation, N-terminal and side chain charge-charge repulsion, and side chain-side chain as well as side chain-backbone interactions. The common picture that emerged is that Coulomb repulsion between water-solvated side chains is efficiently quenched in short peptides as long as side chains are not in direct contact with each other or the main chain.

Magnetotail Structure and its Internal Particle Dynamics During Northward IMF

NASA Technical Reports Server (NTRS)

Ashour-Abdalia, M.; El-Alaoui, M.; Peroomian, V.

1998-01-01

This study uses Global magnetohydrodynamic (MHD) simulations driven by solar wind data along with Geotail observations of the magnetotail to investigate the magnetotail's response to changes in the interplanetary magnetic field (IMF); observed events used in the study occurred on March 29, 1993 and February 9, 1995. For events from February 9, 1995, we also use the time-dependent MHD magnetic and electric fields and the large-scale kinetic (LSK) technique to examine changes in the Geotail ion velocity distributions. Our MHD simulation shows that on March 29, 1993, during a long period of steady northward IMF, the tail was strongly squeezed and twisted around the Sun-Earth axis in response to variations in the IMF B(sub y) component. The mixed (magnetotail and magnetosheath) plasma observed by Geotail results from the spacecraft's close proximity to the magnetopause and its frequent crossings of this boundary. In our second example (February 9, 1995) the IMF was also steady and northward, and in addition had a significant B(sub y) component. Again the magnetotail was twisted, but not as strongly as on March 29, 1993. The Geotail spacecraft, located approximately 30 R(sub E) downtail, observed highly structured ion distribution functions. Using the time-dependent LSK technique, we investigate the ion sources and acceleration mechanisms affecting the Geotail distribution functions during this interval. At 1325 UT most ions are found to enter the magnetosphere on the dusk side earthward of Geotail with a secondary source on the dawn side in the low latitude boundary layer (LLBL). A small percentage come from the ionosphere. By 1347 UT the majority of the ions come from the dawn side LLBL. The distribution functions measured during the later time interval are much warmer, mainly because particles reaching the spacecraft from the dawnside are affected by nonadiabatic scattering and acceleration in the neutral sheet.

Bilateral Activity-Dependent Interactions in the Developing Corticospinal System

PubMed Central

Friel, Kathleen M.; Martin, John H.

2009-01-01

Activity-dependent competition between the corticospinal (CS) systems in each hemisphere drives postnatal development of motor skills and stable CS tract connections with contralateral spinal motor circuits. Unilateral restriction of motor cortex (M1) activity during an early postnatal critical period impairs contralateral visually guided movements later in development and in maturity. Silenced M1 develops aberrant connections with the contralateral spinal cord whereas the initially active M1, in the other hemisphere, develops bilateral connections. In this study, we determined whether the aberrant pattern of CS tract terminations and motor impairments produced by early postnatal M1 activity restriction could be abrogated by reducing activity-dependent synaptic competition from the initially active M1 later in development. We first inactivated M1 unilaterally between postnatal weeks 5–7. We next inactivated M1 on the other side from weeks 7–11 (alternate inactivation), to reduce the competitive advantage that this side may have over the initially inactivated side. Alternate inactivation redirected aberrant contralateral CS tract terminations from the initially silenced M1 to their normal spinal territories and reduced the density of aberrant ipsilateral terminations from the initially active side. Normal movement endpoint control during visually guided locomotion was fully restored. This reorganization of CS terminals reveals an unsuspected late plasticity after the critical period for establishing the pattern of CS terminations in the spinal cord. Our findings show that robust bilateral interactions between the developing CS systems on each side are important for achieving balance between contralateral and ipsilateral CS tract connections and visuomotor control. PMID:17928450

Using the Atwood machine to study Stokes' law

NASA Astrophysics Data System (ADS)

Greenwood, Margaret Stautberg; Fazio, Frances; Russotto, Marie; Wilkosz, Aaron

1986-10-01

A sphere, on one side of an Atwood machine, is immersed in glycerin and permitted to fall. We timed the descent and measured the terminal speed. We varied the mass m2 on the other side of the Atwood machine and plotted a graph of the terminal speed versus mass m2. Both the slope and the intercept yield the viscosity.

Role of LiCoO 2 Surface Terminations in Oxygen Reduction and Evolution Kinetics

DOE PAGES

Han, Binghong; Qian, Danna; Risch, Marcel; ...

2015-03-22

Oxygen reduction reaction (ORR) and oxygen evolution reaction (OER) activities of LiCoO 2 nanorods with sizes in the range from 9 to 40 nm were studied in alkaline solution. The sides of these nanorods were terminated with low-index surfaces such as (003) while the tips were terminated largely with high-index surfaces such as (104) as revealed by high-resolution transmission electron microscopy. Electron energy loss spectroscopy demonstrated that low-spin Co 3+ prevailed on the sides, while the tips exhibited predominantly high- or intermediate-spin Co 3+. We correlated the electronic and atomic structure to higher specific ORR and OER activities at themore » tips as compared to the sides, which was accompanied by more facile redox of Co 2+/3+ and higher charge transferred per unit area. These findings highlight the critical role of surface terminations and electronic structures of transition metal oxides on the ORR and OER activity.« less

Cluster Observations of Particle Injections in the Exterior Cusp

NASA Astrophysics Data System (ADS)

Escoubet, C. P.; Grison, B.; Berchem, J.; Trattner, K. J.; Lavraud, B.; Pitout, F.; Soucek, J.; Richard, R. L.; Laakso, H. E.; Masson, A.; Dunlop, M. W.; Dandouras, I. S.; Reme, H.; Fazakerley, A. N.; Daly, P. W.

2014-12-01

The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process takes place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s with the density of order 5 cm-3. The four Cluster spacecraft had an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions, which leads to energy dispersions, we obtain distances of the ion sources between 14 and 20 RE from the spacecraft. Using Tsyganenko model, we find that these sources are located on the dusk flank, past the terminator. The first injection by C3 is seen at approximately the same time as the 2nd injection on C1 but their sources at the magnetopause were separated by more than 7 RE. This would imply that two distinct sources were active at the same time on the dusk flank of the magnetosphere. In addition, a flow reversal was observed at the magnetopause on C4 which would be an indication that reconnection is taking place near the exterior cusp.

Application of VSC-HVDC with Shunt Connected SMES for Compensation of Power Fluctuation

NASA Astrophysics Data System (ADS)

Linn, Zarchi; Kakigano, Hiroaki; Miura, Yushi; Ise, Toshifumi

This paper describes the application of VSC-HVDC (High Voltage DC Transmission using Voltage Source Converter) with shunt connected SMES (Superconducting Magnetic Energy Storage) for compensation of power fluctuation caused by fluctuating power source such as photovoltaics and wind turbines. The objectives of this proposed system is to smooth out fluctuating power in one terminal side of HVDC in order to avoid causing power system instability and frequency deviation by absorbing or providing power according to the system requirement while another terminal side power is fluctuated. The shunt connected SMES charges and discharges the energy to and from the dc side and it compensates required power of fluctuation to obtain constant power flow in one terminal side of VSC-HVDC system. This system configuration has ability for power system stabilization in the case of power fluctuation from natural energy source. PSCAD/EMTDC simulation is used to evaluate the performance of applied system configuration and control method.

PolarWindsII_DAWN_DC8_1

Atmospheric Science Data Center

2018-04-18

... Layer Winds Surface Winds Upper Level Winds Wind Profiles LIDAR Calibration/Validation Order Data:  ... Model Barrier Flow Case Study DAWN Coherent Wind Profiling Flights DAWN Overview and Preliminary Flight Results ...

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In clean room C of Astrotech's Payload Processing Facility, technicians dressed in "bunny suits," or clean-room attire, begin working on the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

Native Chemical Ligation Strategy to Overcome Side Reactions during Fmoc-Based Synthesis of C-Terminal Cysteine-Containing Peptides.

PubMed

Lelièvre, Dominique; Terrier, Victor P; Delmas, Agnès F; Aucagne, Vincent

2016-03-04

The Fmoc-based solid phase synthesis of C-terminal cysteine-containing peptides is problematic, due to side reactions provoked by the pronounced acidity of the Cα proton of cysteine esters. We herein describe a general strategy consisting of the postsynthetic introduction of the C-terminal Cys through a key chemoselective native chemical ligation reaction with N-Hnb-Cys peptide crypto-thioesters. This method was successfully applied to the demanding peptide sequences of two natural products of biological interest, giving remarkably high overall yields compared to that of a state of the art strategy.

Dawn Usage, Scheduling, and Governance Model

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

Louis, S

2009-11-02

This document describes Dawn use, scheduling, and governance concerns. Users started running full-machine science runs in early April 2009 during the initial open shakedown period. Scheduling Dawn while in the Open Computing Facility (OCF) was controlled and coordinated via phone calls, emails, and a small number of controlled banks. With Dawn moving to the Secure Computing Facility (SCF) in fall of 2009, a more detailed scheduling and governance model is required. The three major objectives are: (1) Ensure Dawn resources are allocated on a program priority-driven basis; (2) Utilize Dawn resources on the job mixes for which they were intended;more » and (3) Minimize idle cycles through use of partitions, banks and proper job mix. The SCF workload for Dawn will be inherently different than Purple or BG/L, and therefore needs a different approach. Dawn's primary function is to permit adequate access for tri-lab code development in preparation for Sequoia, and in particular for weapons multi-physics codes in support of UQ. A second purpose is to provide time allocations for large-scale science runs and for UQ suite calculations to advance SSP program priorities. This proposed governance model will be the basis for initial time allocation of Dawn computing resources for the science and UQ workloads that merit priority on this class of resource, either because they cannot be reasonably attempted on any other resources due to size of problem, or because of the unavailability of sizable allocations on other ASC capability or capacity platforms. This proposed model intends to make the most effective use of Dawn as possible, but without being overly constrained by more formal proposal processes such as those now used for Purple CCCs.« less

Thrust Direction Optimization: Satisfying Dawn's Attitude Agility Constraints

NASA Technical Reports Server (NTRS)

Whiffen, Gregory J.

2013-01-01

The science objective of NASA's Dawn Discovery mission is to explore the two largest members of the main asteroid belt, the giant asteroid Vesta and the dwarf planet Ceres. Dawn successfully completed its orbital mission at Vesta. The Dawn spacecraft has complex, difficult to quantify, and in some cases severe limitations on its attitude agility. The low-thrust transfers between science orbits at Vesta required very complex time varying thrust directions due to the strong and complex gravity and various science objectives. Traditional thrust design objectives (like minimum (Delta)V or minimum transfer time) often result in thrust direction time evolutions that can not be accommodated with the attitude control system available on Dawn. This paper presents several new optimal control objectives, collectively called thrust direction optimization that were developed and necessary to successfully navigate Dawn through all orbital transfers at Vesta.

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

The Dawn spacecraft is seen here in clean room C of Astrotech's Payload Processing Facility. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

Solar maximum mission fine pointing sun sensor dawn and dusk errors flight data and model analysis

NASA Technical Reports Server (NTRS)

Kulp, D. R.

1988-01-01

SMM flight system control errors occurring at spacecraft dawn and dusk are analyzed. The errors are associated with the fine pointing sun sensor (FPSS), which is a primary component of the SMM attitude control system. It is shown that the source of the FPSS dawn/dusk distortion is the incomplete masking of sunlight reflected off the earth by the optical baffle covering the FPSS sensor heads onboard the SMM during periods of orbit dawn and dusk. For the most part, the modeled behavior of the FPSS under dawn and dusk lighting conditions matches the observed behavior in the SMM flight data.

Ionospheric convection signatures observed by DE 2 during northward interplanetary magnetic field

NASA Technical Reports Server (NTRS)

Heelis, R. A.; Hanson, W. B.; Reiff, P. H.; Winningham, J. D.

1986-01-01

Observations of the ionospheric convection signature at high latitudes are examined during periods of prolonged northward interplanetary magnetic field (IMF). The data from Dynamics Explorer 2 show that a four-cell convection pattern can frequently be observed in a region that is displaced to the sunward side of the dawn-dusk meridian regardless of season. In the eclipsed ionosphere, extremely structured or turbulent flow exists with no identifiable connection to a more coherent pattern that may simultaneously exist in the dayside region. The two highest-latitude convection cells that form part of the coherent dayside pattern show a dependence on the y component of the IMF. This dependence is such that a clockwise circulating cell displaced toward dawn dominates the high-latitude region when B(Y) is positive. Anti-clockwise circulation displaced toward dusk dominates the highest latitudes when B(Y) is negative. Examination of the simultaneously observed energetic particle environment suggests that both open and closed field lines may be associated with the high-latitude convection cells. On occasions these entire cells can exist on open field lines. The existence of closed field lines in regions of sunward flow is also apparent in the data.

Dawn LAMO Image 19

NASA Image and Video Library

2016-02-03

Tupo Crater on Ceres is seen in this view from NASA Dawn spacecraft. This crater, located in the southern hemisphere of Ceres, was named for the Polynesian god of turmeric. Dawn captured the scene on Dec. 24, 2015.

1. Occident Terminal Elevator and annex, (l)1930/workhouse and annex 1925 ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. Occident Terminal Elevator and annex, (l)-1930/workhouse and annex 1925 with train shed Peavey Duluth Terminal Annex on left 1930-workhouse 1908 (white silos). - Occident Terminal Elevator & Storage Annex, South side of second slip, north from outer end of Rice's Point, east of Garfield Avenue, Duluth, St. Louis County, MN

Smooth pond-like deposits on asteroid 4 Vesta: First results from the Dawn mission.

NASA Astrophysics Data System (ADS)

Hiesinger, H.; Ruesch, O.; Jaumann, R.; Nathues, A.; Raymond, C. A.; Russell, C. T.

2012-04-01

The Dawn spacecraft arrived at Vesta on July 16, 2011 to study the asteroid with a Framing Camera (FC), a Visible & Infrared Spectrometer (VIR), and a Gamma Ray and Neutron Detector (GRaND) [1]. Dawn provides the first high-resolution data from its survey orbit, high-altitude mapping orbit (HAMO), and low-altitude mapping orbit (LAMO). FC data revealed smooth pond-like deposits of ambiguous origin, similar to deposits on other asteroids, including Eros and Itokawa [2,3]. Several scenarios for the origin of these deposits can be tested with Dawn data, including volcanism, impact sedimentation, impact melt deposition, dust levitation and transport, seismic shaking, or landslides. We measured 83 small (~7 km2 average size) smooth deposits distributed across the surface of Vesta. Most ponds on Vesta occur on the floors of impact craters and in irregular depressions. We did not observe inflow of material into the depressions. Most of these deposits have well-defined geological contacts, indicating that they are younger than the surrounding terrain. However, lunar impact melt pools that formed contemporaneously with surrounding ejecta blankets show similar stratigraphic relationships. Sometimes the albedo of these ponds is lower than the surrounding terrain, in other cases the ponds are indistinguishable from the adjacent terrain. The ponds preferentially occur in a band between -10 and 30 degrees latitude with fewer ponds north of ~30 degrees and even fewer ponds in the southern hemisphere, i.e., the Rheasilvia region. The largest cluster of ponds occurs in the vicinity of the Marcia impact crater, which is part of the so-called snowman craters. Similar, but smaller (<230 m diameter) smooth ponds were also reported from the surface of asteroid Eros [2]. Robinson et al. [2] found that most smooth ponds on Eros occur in equatorial regions and concluded that the most likely process for their formation is electrostatic levitation and redistribution of the finest regolith components (<100 µm). Sierks et al. [4] argued that along the terminator, particularly strong electric fields can develop between the sun-lit and shaded areas, e.g., within craters, resulting in particle motion from sun-lit to dark regions. Dust levitation and transport was also discussed for asteroid 25143 Itokawa [3]. [1] Russell et al., (2007), Earth Moon Planets, 101; [2] Robinson et al., (2002), Met. Planet. Sci., 37; [3] Yano et al., (2006), Science, 312; [4] Sierks et al., (2011), Space Sci. Rev., doi:10.1007/s11214-011-9745-4. This research has been supported by the German Space Agency (DLR) and NASA. We would like to thank the Dawn Operations Team for their success-ful planning and acquisition of high-quality Vesta data.

RNA circularization reveals terminal sequence heterogeneity in a double-stranded RNA virus.

PubMed

Widmer, G

1993-03-01

Double-stranded RNA viruses (dsRNA), termed LRV1, have been found in several strains of the protozoan parasite Leishmania. With the aim of constructing a full-length cDNA copy of the viral genome, including its terminal sequences, a protocol based on PCR amplification across the 3'-5' junction of circularized RNA was developed. This method proved to be applicable to dsRNA. It provided a relatively simple alternative to one-sided PCR, without loss of specificity inherent in the use of generic primers. LRV1 terminal nucleotide sequences obtained by this method showed a considerable variation in length, particularly at the 5' end of the positive strand, as well as the potential for forming 3' overhangs. The opposite genomic end terminates in 0, 1, or 2 TCA trinucleotide repeats. These results are compared with terminal sequences derived from one-sided PCR experiments.

Dawn Blue Glow Artist Concept

NASA Image and Video Library

2015-03-02

This artist concept shows NASA Dawn spacecraft arriving at the dwarf planet Ceres. Dawn travels through space using a technology called ion propulsion, with ions glowing with blue light are accelerated out of an engine, giving the spacecraft thrust.

Artist Rendering of NASA Dawn Spacecraft Approaching Mars

NASA Image and Video Library

2009-05-23

Artist rendering of NASA's Dawn spacecraft approaching Mars. Dawn, part of NASA's Discovery Program of competitively selected missions, was launched in 2007 to orbit the large asteroid Vesta and the dwarf planet Ceres. The two bodies have very different properties from each other. By observing them both with the same set of instruments, Dawn will probe the early solar system and specify the properties of each body. http://photojournal.jpl.nasa.gov/catalog/PIA18152

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In clean room C of Astrotech's Payload Processing Facility, a worker wears a "bunny suit," or clean-room attire, next to the Dawn spacecraft, which will be unbagged and undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

Vesta in the Light of Dawn, But Without HEDS?

NASA Technical Reports Server (NTRS)

McSween, H. Y.; Mittlefehldt, D. W.

2014-01-01

The derivation of HEDs from Vesta is strongly supported by Dawn data [1], and these meterorites have made interpretations of Dawn spectra much more rigorous. Compared to the Moon, where samples became available after geologic mapping, the exploration of Vesta has been backwards. But what if HEDs had not been available or identified as vestan samples? What petrologic and geochemical predictions would have been possible using Dawn data, without the benefit of HEDs?

Offshore Wind Measurements Using Doppler Aerosol Wind Lidar (DAWN) at NASA Langley Research Center

NASA Technical Reports Server (NTRS)

Beyon, Jeffrey Y.; Koch, Grady J.; Kavaya, Michael J.

2014-01-01

The latest flight demonstration of Doppler Aerosol Wind Lidar (DAWN) at NASA Langley Research Center (LaRC) is presented. The goal of the campaign was to demonstrate the improvement of DAWN system since the previous flight campaign in 2012 and the capabilities of DAWN and the latest airborne wind profiling algorithm APOLO (Airborne Wind Profiling Algorithm for Doppler Wind Lidar) developed at LaRC. The comparisons of APOLO and another algorithm are discussed utilizing two and five line-of-sights (LOSs), respectively. Wind parameters from DAWN were compared with ground-based radar measurements for validation purposes. The campaign period was June - July in 2013 and the flight altitude was 8 km in inland toward Charlotte, NC, and offshores in Virginia Beach, VA and Ocean City, MD. The DAWN system was integrated into a UC12B with two operators onboard during the campaign.

Dawn's Exploration of Vesta

NASA Technical Reports Server (NTRS)

Rayman, Marc D.; Mase, Robert A.

2012-01-01

On 16 July 2011, after completing nearly four years of interplanetary flight, Dawn entered orbit around (4) Vesta, the second most massive body in the main asteroid belt. Dawn used solar electric propulsion to spiral to a series of six different orbits to accomplish its science campaign. Although the transfers to progressively lower orbits presented significant challenges, all were executed smoothly. During its nearly 14 months in orbit, Dawn spiraled down to 210 km above the surface and back up, before initiating the gradual departure to travel to dwarf planet (1) Ceres for a 2015 rendezvous. Dawn's exploration of Vesta has shown it to be geologically complex and fascinating, resembling terrestrial planets more than typical asteroids. Among the principal features is a 500-km diameter impact basin within which is the second tallest mountain known in the solar system. This paper presents Dawn's operations at Vesta and summarizes the principal findings.

Offshore wind measurements using Doppler aerosol wind lidar (DAWN) at NASA Langley Research Center

NASA Astrophysics Data System (ADS)

Beyon, Jeffrey Y.; Koch, Grady J.; Kavaya, Michael J.

2014-06-01

The latest flight demonstration of Doppler Aerosol Wind Lidar (DAWN) at NASA Langley Research Center (LaRC) is presented. The goal of the campaign was to demonstrate the improvement of DAWN system since the previous flight campaign in 2012 and the capabilities of DAWN and the latest airborne wind profiling algorithm APOLO (Airborne Wind Profiling Algorithm for Doppler Wind Lidar) developed at LaRC. The comparisons of APOLO and another algorithm are discussed utilizing two and five line-of-sights (LOSs), respectively. Wind parameters from DAWN were compared with ground-based radar measurements for validation purposes. The campaign period was June - July in 2013 and the flight altitude was 8 km in inland toward Charlotte, NC, and offshores in Virginia Beach, VA and Ocean City, MD. The DAWN system was integrated into a UC12B with two operators onboard during the campaign.

Thrust Direction Optimization: Satisfying Dawn's Attitude Agility Constraints

NASA Technical Reports Server (NTRS)

Whiffen, Gregory J.

2013-01-01

The science objective of NASA's Dawn Discovery mission is to explore the giant asteroid Vesta and the dwarf planet Ceres, the two largest members of the main asteroid belt. Dawn successfully completed its orbital mission at Vesta. The Dawn spacecraft has complex, difficult to quantify, and in some cases severe limitations on its attitude agility. The low-thrust transfers between science orbits at Vesta required very complex time varying thrust directions due to the strong and complex gravity and various science objectives. Traditional low-thrust design objectives (like minimum change in velocity or minimum transfer time) often result in thrust direction time evolutions that cannot be accommodated with the attitude control system available on Dawn. This paper presents several new optimal control objectives, collectively called thrust direction optimization that were developed and turned out to be essential to the successful navigation of Dawn at Vesta.

Airfoil-Shaped Fluid Flow Tool for Use in Making Differential Measurements

NASA Technical Reports Server (NTRS)

England, John Dwight (Inventor); Kelley, Anthony R. (Inventor); Cronise, Raymond J. (Inventor)

2014-01-01

A fluid flow tool includes an airfoil structure and a support arm. The airfoil structure's high-pressure side and low-pressure side are positioned in a conduit by the support arm coupled to the conduit. The high-pressure and low-pressure sides substantially face opposing walls of the conduit. At least one measurement port is formed in the airfoil structure at each of its high-pressure side and low-pressure side. A first manifold, formed in the airfoil structure and in fluid communication with each measurement port so-formed at the high-pressure side, extends through the airfoil structure and support arm to terminate and be accessible at the exterior wall of the conduit. A second manifold, formed in the airfoil structure and in fluid communication with each measurement port so-formed at the low-pressure side, extends through the airfoil structure and support arm to terminate and be accessible at the exterior wall of the conduit.

Warfare, genocide, and ethnic conflict: a Darwinian approach.

PubMed

Dimijian, Gregory G

2010-07-01

As the 21st century dawns, I reflect on the history of humankind with growing concern about the need to understand the underlying biological and cultural roots of ethnic conflict and warfare. In the many studies of human conflict, innate biological predispositions have been neglected. This article is the third part of a series of seminars for medical residents at the University of Texas Southwestern Medical School at Dallas (see http://adarwinstudygroup.org/). The series starts with in-depth coverage of Darwinian natural and sexual selection, with examples from the domestication of animals and plants and the crisis of antibiotic resistance. The series strives to show how biology has been neglected in the study of the we-they orientation of human behavior, with its devastating consequences. The subject material is profoundly disturbing, as it looks at "human nature" and contrasts the "dark side" of human behavior with the opposite, profoundly caring and loving side.

First results from the Giotto magnetometer experiment at comet Halley

NASA Technical Reports Server (NTRS)

Neubauer, F. M.; Glassmeier, K. H.; Pohl, M.; Raeder, J.; Acuna, M. H.; Burlaga, L. F.; Ness, N. F.

1986-01-01

The Giotto magnetometer experiment at comet Halley has for the first time provided magnetic field measurements in all the important spatial regions characterizing the front-side interaction between the solar-wind magnetoplasma and a cometary atmosphere. Upstream waves of cometary origin have been observed at distances greater than two million km from the comet, both inbound and outbound. A cometary bow shock has been identified at 1.15 million inbound on the dawn side and a thick quasi-parallel cometary bow shock outbound. A turbulent magnetosheath has been observed further inside. A magnetic pile-up region has been identified inside 135,000 km, inbound, and 263,000 km, outbound, with fields up to 57 and 65 nT, respectively. A cavity region with essentially zero magnetic field has been discovered, with a width of 8500 km along the trajectory around closest approach.

KSC-07pd1299

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. -- At Astrotech's Payload Processing Facility, technicians check the Dawn spacecraft as it is lowered onto a transporter. Dawn will be moved to the Hazardous Processing Facility for fueling. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Charisse Nahser

KSC-07pd1305

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. -- Inside Astrotech's Hazardous Processing Facility, technicians check the Dawn spacecraft as it is lowered onto a scale for weighing. Next, Dawn will be prepared for fueling. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Charisse Nahser

KSC-07pd1300

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. --At Astrotech's Payload Processing Facility, technicians maneuver the shipping container to place around the Dawn spacecraft, at right. Dawn will be moved to the Hazardous Processing Facility for fueling. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Charisse Nahser

Prioritizing Strategic Interests in South Asia

DTIC Science & Technology

2010-06-01

rolled out “Aghaz-e-Haqooq Balochistan ”—its by far the most serious fallout from the conflict in Afghanistan is the increasing radicalization of...Foreign Policy, August 2006, available at <www.foreignpolicy.com/ story/cms.php?story_id=3578>. 17 “Aghaz-e-Haqooq Balochistan Package,” Dawn. com...November 16, 2009, available at <www.dawn.com/ wps/wcm/connect/dawn-content-library/dawn/news/ pakistan/13+aghaz-e-haqooq+ balochistan +package- za-05

Three-terminal graphene single-electron transistor fabricated using feedback-controlled electroburning

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

Puczkarski, Paweł; Gehring, Pascal, E-mail: pascal.gehring@materials.ox.ac.uk; Lau, Chit S.

2015-09-28

We report room-temperature Coulomb blockade in a single layer graphene three-terminal single-electron transistor fabricated using feedback-controlled electroburning. The small separation between the side gate electrode and the graphene quantum dot results in a gate coupling up to 3 times larger compared to the value found for the back gate electrode. This allows for an effective tuning between the conductive and Coulomb blocked state using a small side gate voltage of about 1 V. The technique can potentially be used in the future to fabricate all-graphene based room temperature single-electron transistors or three terminal single molecule transistors with enhanced gate coupling.

Synthesis of novel vitamin K derivatives with alkylated phenyl groups introduced at the ω-terminal side chain and evaluation of their neural differentiation activities.

PubMed

Sakane, Rie; Kimura, Kimito; Hirota, Yoshihisa; Ishizawa, Michiyasu; Takagi, Yuta; Wada, Akimori; Kuwahara, Shigefumi; Makishima, Makoto; Suhara, Yoshitomo

2017-11-01

Vitamin K is an essential cofactor of γ-glutamylcarboxylase as related to blood coagulation and bone formation. Menaquinone-4, one of the vitamin K homologues, is biosynthesized in the body and has various biological activities such as being a ligand for steroid and xenobiotic receptors, protection of neuronal cells from oxidative stress, and so on. From this background, we focused on the role of menaquinone in the differentiation activity of progenitor cells into neuronal cells and we synthesized novel vitamin K derivatives with modification of the ω-terminal side chain. We report here new vitamin K analogues, which introduced an alkylated phenyl group at the ω-terminal side chain. These compounds exhibited potent differentiation activity as compared to control. Copyright © 2017 The Author(s). Published by Elsevier Ltd.. All rights reserved.

Electron pitch angle distributions throughout the magnetosphere as observed on Ogo 5.

NASA Technical Reports Server (NTRS)

West, H. I., Jr.; Buck, R. M.; Walton, J. R.

1973-01-01

A survey of the equatorial pitch angle distributions of energetic electrons is provided for all local times out to radial distances of 20 earth radii on the night side of the earth and to the magnetopause on the day side of the earth. In much of the inner magnetosphere and in the outer magnetosphere on the day side of the earth, the normal loss cone distribution prevails. The effects of drift shell splitting - i.e., the appearance of pitch angle distributions with minimums at 90 deg, called butterfly distributions - become apparent in the early afternoon magnetosphere at extended distances, and the distribution is observed in to 5.5 earth radii in the nighttime magnetosphere. Inside about 9 earth radii the pitch angle effects are quite energy-dependent. Beyond about 9 earth radii in the premidnight magnetosphere during quiet times the butterfly distribution is often observed. It is shown that these electrons cannot survive a drift to dawn without being considerably modified. The role of substorm activity in modifying these distributions is identified.

Dawn simulation and bright light in the treatment of SAD: a controlled study.

PubMed

Avery, D H; Eder, D N; Bolte, M A; Hellekson, C J; Dunner, D L; Vitiello, M V; Prinz, P N

2001-08-01

Some small controlled studies have found that dawn simulation is effective in treating seasonal affective disorder (SAD). With a larger sample size and a longer duration of treatment, we compared dawn simulation with bright light therapy and a placebo condition in patients with SAD. Medication-free patients with SAD were randomly assigned to one of three conditions: bright light therapy (10,000 lux for 30 min, from 6:00 AM to 6:30 AM), dawn simulation (1.5 hour dawn signal from 4:30 AM to 6:00 AM peaking at 250 lux), and a placebo condition, a dim red light (1.5 hour dawn signal from 4:30 am to 6:00 AM peaking at 0.5 lux.) Over the subsequent 6 weeks, the subjects were blindly rated by a psychiatrist using the Structured Interview Guide for the Hamilton Depression Rating-Seasonal Affective Disorder Version (SIGH-SAD). We modeled the profiles of the remissions (SIGH-SAD < or = 8) and response (> or =50% decrease in SIGH-SAD) to treatment over time using Cox proportional hazards models. The sample consisted of 95 subjects who were randomized to the three conditions: bright light (n = 33), dawn simulation (n = 31) and placebo (n = 31). Dawn simulation was associated with greater remission (p <.05) and response (p <.001) rates compared to the placebo. Bright light did not differ significantly from the placebo. Dawn simulation was associated with greater remission (p <.01) and response (p <.001) rates compared to the bright light therapy. The mean daily hours of sunshine during the week before each visit were associated with a significant increase in likelihood of both remission (p <.001) and response (p <.001). Dawn simulation was associated with greater remission and response rates compared to the placebo and compared to bright light therapy. The hours of sunshine during the week before each assessment were associated with a positive clinical response.

South Melea Planum, By The Dawn's Early Light

NASA Technical Reports Server (NTRS)

1999-01-01

MOC 'sees' by the dawn's early light! This picture was taken over the high southern polar latitudes during the first week of May 1999. The area shown is currently in southern winter darkness. Because sunlight is scattered over the horizon by aerosols--dust and ice particles--suspended in the atmosphere, sufficient light reaches regions within a few degrees of the terminator (the line dividing night and day) to be visible to the Mars Global Surveyor Mars Orbiter Camera (MOC) when the maximum exposure settings are used.

This image shows a bright, wispy cloud hanging over southern Malea Planum. This cloud would not normally be visible, since it is currently in darkness. At the time this picture was taken, the sun was more than 5.7o below the northern horizon. The scene covers an area 3 kilometers (1.9 miles) wide. Again, the illumination is from the top.

In this frame, the surface appears a relatively uniform gray. At the time the picture was acquired, the surface was covered with south polar wintertime frost. The highly reflective frost, in fact, may have contributed to the increased visibility of this surface.

This 'twilight imaging' technique for viewing Mars can only work near the terminator; thus in early May only regions between about 67oS and 74oS were visible in twilight images in the southern hemisphere, and a similar narrow latitude range could be imaged in the northern hemisphere. MOC cannot 'see' in the total darkness of full-borne night.

Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

South Melea Planum, By The Dawn's Early Light

NASA Technical Reports Server (NTRS)

1999-01-01

MOC 'sees' by the dawn's early light! This picture was taken over the high southern polar latitudes during the first week of May 1999. The area shown is currently in southern winter darkness. Because sunlight is scattered over the horizon by aerosols--dust and ice particles--suspended in the atmosphere, sufficient light reaches regions within a few degrees of the terminator (the line dividing night and day) to be visible to the Mars Global Surveyor Mars Orbiter Camera (MOC) when the maximum exposure settings are used.

This picture shows a polygonally-patterned surface on southern Malea Planum. At the time the picture was taken, the sun was more than 4.5o below the northern horizon. The scene covers an area 3 kilometers (1.9 miles) wide, with the illumination from the top of the picture.

In this frame, the surface appears a relatively uniform gray. At the time the picture was acquired, the surface was covered with south polar wintertime frost. The highly reflective frost, in fact, may have contributed to the increased visibility of this surface.

This 'twilight imaging' technique for viewing Mars can only work near the terminator; thus in early May only regions between about 67oS and 74oS were visible in twilight images in the southern hemisphere, and a similar narrow latitude range could be imaged in the northern hemisphere. MOC cannot 'see' in the total darkness of full-borne night.

Malin Space Science Systems and the California Institute of Technology built the MOC using spare hardware from the Mars Observer mission. MSSS operates the camera from its facilities in San Diego, CA. The Jet Propulsion Laboratory's Mars Surveyor Operations Project operates the Mars Global Surveyor spacecraft with its industrial partner, Lockheed Martin Astronautics, from facilities in Pasadena, CA and Denver, CO.

76 FR 48834 - Michigan Consolidated Gas Company and Dawn Gateway Pipeline, LLC; Notice of Application

Federal Register 2010, 2011, 2012, 2013, 2014

2011-08-09

...'s Belle River-St. Clair Pipeline into the new 21-mile long Dawn Gateway Pipeline system, which... & Optimization, DTE Pipeline/Dawn Gateway LLC, One Energy Plaza, Detroit, MI 48226, phone (313) 235-6531 or e...

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In clean room C of Astrotech's Payload Processing Facility, a worker wearing a "bunny suit," or clean-room attire, begins removing the protective cover surrounding the Dawn spacecraft. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

Dawn Spacecraft Processing

NASA Image and Video Library

2007-04-10

In clean room C of Astrotech's Payload Processing Facility, a worker wearing a "bunny suit," or clean-room attire, looks over the Dawn spacecraft after removing the protective cover, at bottom right. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C.

KSC-07pd0858

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Payload Processing Facility, an overhead crane lifts the Dawn spacecraft from its transporter. Dawn will be moved into clean room C for unbagging and further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

KSC-07pd1304

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. -- Inside Astrotech's Hazardous Processing Facility, technicians check the progress of the Dawn spacecraft as it is lifted off the transporter. Dawn will be moved to a scale for weighing and then prepared for fueling. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Charisse Nahser

[Correlation study between obesity and dawn phenomenon in patients with type 2 diabetes].

PubMed

Guo, Zhenhong; Xu, Jie; Wang, Jingyu; Han, Fei; Zhang, Yi; Yang, X iaoyun; Yang, Shaohua; Chang, Bai; Yang, Juhong; Shan, Chunyan; Chen, Liming; Chang, Baocheng; Xu, Yanguang

2016-01-01

To investigate the correlation between the frequency of dawn phenomenon and obesity in patients with type 2 diabetes. This study was conducted in 98 patients with type 2 diabetes admitted to the Metabolic Disease Hospital of Tianjin Medical University from 2011 to 2014. The subjects were divided into 3 groups according to BMI: the normal weight (BMI 18.5-23.9 kg/m(2), n = 30), the overweight(BMI 24-27.9 kg/m(2), n = 33)and the obesity (BMI ≥ 28.0 kg/m(2), n = 35). All participants underwent continuous glucose monitoring for 72 h. Fasting plasma glucose(FPG), insulin and C-peptide were tested. Frequency of dawn phenomenon among the 3 groups was calculated, and the correlations between dawn phenomenon and its related factors were analyzed. The frequency of dawn phenomenon in type 2 diabetes increased with the increase of BMI in the 3 groups (P < 0.05) with 33.3% in the normal weight, 78.8% in the overweight and 88.6% in the obesity groups, respectively. The dawn phenomenon was positively correlated with BMI (r = 0.424, P < 0.05), Homeostasis model assessment of insulin resistance(HOMA-IR) (r = 0.781, P < 0.05), waist circumference (r = 0.394, P < 0.05), fasting C-peptide (r = 0.254, P < 0.05)and TG (r = 0.220, P < 0.05). It was negatively correlated with the course of diabetes mellitus (r = -0.278, P<0.05) and HDL-C (r = -0.268, P < 0.05). No correlation could be viewed between the dawn phenomenon and age, LDL-C, glycosylated hemoglobin A1c(HbA1c), TC and FPG (P > 0.05). The dawn phenomenon is closely associated with obesity and insulin resistance. The frequency of dawn phenomenon increases with BMI.

Dawn HAMO Image 75

NASA Image and Video Library

2015-12-11

This view from NASA Dawn spacecraft shows high northern latitudes on Ceres. Dawn acquired the image on Oct. 17, 2015, from an altitude of 915 miles 1,470 kilometers. It has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20138

KSC-07pd1645

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians lower the upper canister over the Dawn spacecraft. After enclosure, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1636

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, the Dawn spacecraft has been wrapped with a protective cover before it is enclosed in a canister. Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1646

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians secure the upper canister over the Dawn spacecraft. Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1644

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians begin lowering the upper canister over the Dawn spacecraft. After enclosure, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

The magnetospheric lobe at geosynchronous orbit

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

Thomsen, M.F.; Bame, S.J.; McComas, D.J.

1994-09-01

On rare occasions, satellites at geosynchronous altitude enter the magnetospheric lobe, characterized by extremely low ion fluxes between 1 eV and 40 keV and electron fluxes above a few hundred eV. One year of plasma observations from two simultaneously operating spacecraft at synchronous orbit is surveyed for lobe encounters. A total of 34 full encounters and 56 apparent near encounters are identified, corresponding to {approximately}0.06% of the total observation time. Unlike energetic particle (E>40 keV) dropouts studied earlier, there is a strong tendency for the lobe encounters to occur postmidnight, as late as 07 local time. The two spacecraft encountermore » the lobe with different rates and in different seasons. These occurrence properties are not simply explicable in terms of the orbital geometry in either the solar magnetic or the geocentric solar magnetospheric coordinate system. A composite coordinate system which previously organized more energetic particle dropouts is somewhat more successful in organizing the lobe encounters, suggesting that solar wind distortion of the magnetic equatorial plane away from the dipole location and toward the antisolar direction may be largely responsible for these dropouts. The authors results further suggest that this distortion persists even sunward of the dawn-dusk terminator. However, a simple dawn-dusk symmetric distortion does not fully account for all the seasonal and local time asymmetries in the occurrence of the lobe encounters; thus there is probably an additional dawn-dusk asymmetry in the distorted field. The lobe encounters are strongly associated with magnetospheric activity and tend to occur in association with rare magnetosheath encounters at synchronous orbit. It thus appears that the presence of the lobe at geosynchronous orbit is the result of major, probably asymmetric modifications of the magnetospheric field geometry in times of strong disturbance. 19 refs., 7 figs., 1 tab.« less

Ceres From Dawn, Processed

NASA Image and Video Library

2015-01-19

This processed image, taken Jan. 13, 2015, shows the dwarf planet Ceres as seen from the Dawn spacecraft. The image hints at craters on the surface of Ceres. Dawn framing camera took this image at 238,000 miles 383,000 kilometers from Ceres. http://photojournal.jpl.nasa.gov/catalog/PIA19167

Structure and wettability property of the growth and nucleation surfaces of thermally treated freestanding CVD diamond films

NASA Astrophysics Data System (ADS)

Pei, Xiaoqiang; Cheng, Shaoheng; Ma, Yibo; Wu, Danfeng; Liu, Junsong; Wang, Qiliang; Yang, Yizhou; Li, Hongdong

2015-08-01

This paper reports the surface features and wettability properties of the (1 0 0)-textured freestanding chemical vapor deposited (CVD) diamond films after thermal exposure in air at high temperature. Thermal oxidation at proper conditions eliminates selectively nanodiamonds and non-diamond carbons in the films. The growth side of the films contains (1 0 0)-oriented micrometer-sized columns, while its nucleation side is formed of nano-sized tips. The examined wettability properties of the as-treated diamond films reveal a hydrophilicity and superhydrophilicity on the growth surface and nucleation surface, respectively, which is determined by oxygen termination and geometry structure of the surface. When the surface termination is hydrogenated, the wettability of nucleation side converted from superhydrophilicity to high hydrophobicity, while the hydrophilicity of the growth side does not change significantly. The findings open a possibility for realizing freestanding diamond films having not only novel surface structures but also multifunction applications, especially proposed on the selected growth side or nucleation side in one product.

Asymmetry of nonlinear interactions of solar MHD discontinuities with the bow shock

NASA Astrophysics Data System (ADS)

Grib, S. A.; Pushkar, E. A.

2006-07-01

Oblique interaction between the solar fast shock wave, which is a typical nonstationary strong discontinuity in the interplanetary space, and the bow shock front upstream of an Earth-type planetary magnetosphere is studied. Attention has been paid to the qualitative and quantitative (with respect to the proton density distribution) dawn-dusk (or morning-evening) asymmetry of the discontinuities refracted into the magnetosheath, which originates in the ecliptic plane on different sides of the Sun-Earth line. The results under discussion have been corroborated experimentally by the gas-kinetic pattern of the bow-shock front and the WIND and ISEE 3 spacecraft measurements of the plasma density.

Brave new worlds

NASA Astrophysics Data System (ADS)

Boss, Alan

2009-03-01

Are we alone? There is perhaps no more important single scientific question. People have pondered this issue from the very dawn of sentience, wondering if other, similar, beings inhabited a distant mountain range or the other side of an ocean. The history of humanity is largely one of exploration and expansion, and while at first this was limited to the Earth's surface, in the last few decades only the power of our interplanetary rockets has kept us from exploring our wider environment. As the science-fiction author Ray Bradbury proclaimed when the Viking landers arrived on Mars in July 1976, "There is life on Mars, and it is us."

Golf hand prosthesis performance of transradial amputees.

PubMed

Carey, Stephanie L; Wernke, Matthew M; Lura, Derek J; Kahle, Jason T; Dubey, Rajiv V; Highsmith, M Jason

2015-06-01

Typical upper limb prostheses may limit sports participation; therefore, specialized terminal devices are often needed. The purpose of this study was to evaluate the ability of transradial amputees to play golf using a specialized terminal device. Club head speed, X-factor, and elbow motion of two individuals with transradial amputations using an Eagle Golf terminal device were compared to a non-amputee during a golf swing. Measurements were collected pre/post training with various stances and grips. Both prosthesis users preferred a right-handed stance initially; however, after training, one preferred a left-handed stance. The amputees had slower club head speeds and a lower X-factor compared to the non-amputee golfer, but increased their individual elbow motion on the prosthetic side after training. Amputees enjoyed using the device, and it may provide kinematic benefits indicated by the increase in elbow flexion on the prosthetic side. The transradial amputees were able to swing a golf club with sufficient repetition, form, and velocity to play golf recreationally. Increased elbow flexion on the prosthetic side suggests a potential benefit from using the Eagle Golf terminal device. Participating in recreational sports can increase amputees' health and quality of life. © The International Society for Prosthetics and Orthotics 2014.

KSC-07pd1243

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers prepare the Dawn spacecraft for thermal blanket installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

KSC-07pd1242

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers prepare the Dawn spacecraft for thermal blanket installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

KSC-07pd2429

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is moved toward the opening above the Delta II rocket in the mobile service tower. Dawn will be mated with the Delta in preparation for launch. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2430

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lowered toward the awaiting Delta II rocket in the mobile service tower. Dawn will be mated with the Delta in preparation for launch. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2427

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lifted alongside the mobile service tower. At the top, Dawn will be prepared for mating with the awaiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2431

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, workers in the mobile service tower keep watch as the Dawn spacecraft is lowered toward the awaiting Delta II rocket. Dawn will be mated with the Delta in preparation for launch. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2438

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- In the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, workers remove the transportation canister from around the Dawn spacecraft. After removal of the canister, Dawn will be mated with the waiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. EDT Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jim Grossmann

KSC-07pd2426

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lifted alongside the mobile service tower. At the top, Dawn will be prepared for mating with the awaiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2424

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- The Dawn spacecraft arrives on Launch Pad 17-B at Cape Canaveral Air Force Station. At the pad, Dawn will be lifted into the mobile service tower and prepared for mating with the awaiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2442

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- In the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, the upper transportation canister is lifted away from the Dawn spacecraft. After removal of the canister, Dawn will be mated with the waiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. EDT Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jim Grossmann

KSC-07pd2425

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lifted off its transporter. Dawn will be lifted into the mobile service tower and prepared for mating with the awaiting Delta II rocket.Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd1640

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians move another segment of the lower canister onto the workstand holding the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1643

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians move the partially enclosed Dawn spacecraft into another room to complete the canning. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1638

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians move the first segment of the lower canister around the upper stage booster below the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1641

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians place another segment of the canister around the upper stage booster below the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1642

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians examine the lower canister they placed around the bottom of the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1637

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians move the first segment of the lower canister toward the stand holding the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

KSC-07pd1639

NASA Image and Video Library

2007-06-26

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians move the first segment of the lower canister around the upper stage booster below the Dawn spacecraft. When enclosed in the canister, Dawn will be transported to Launch Pad 17-B and lifted into the mobile service tower for mating with the Delta II launch vehicle. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/George Shelton

The macaque midbrain reticular formation sends side-specific feedback to the superior colliculus.

PubMed

Wang, Niping; Warren, Susan; May, Paul J

2010-04-01

The central mesencephalic reticular formation (cMRF) likely plays a role in gaze control, as cMRF neurons receive tectal input and provide a bilateral projection back to the superior colliculus (SC). We examined the important question of whether this feedback is excitatory or inhibitory. Biotinylated dextran amine (BDA) was injected into the cMRF of M. fascicularis monkeys to anterogradely label reticulotectal terminals and retrogradely label tectoreticular neurons. BDA labeled profiles in the ipsi- and contralateral intermediate gray layer (SGI) were examined electron microscopically. Postembedding GABA immunochemistry was used to identify putative inhibitory profiles. Nearly all (94.7%) of the ipsilateral BDA labeled terminals were GABA positive, but profiles postsynaptic to these labeled terminals were exclusively GABA negative. In addition, BDA labeled terminals were observed to contact BDA labeled dendrites, indicating the presence of a monosynaptic feedback loop connecting the cMRF and ipsilateral SC. In contrast, within the contralateral SGI, half of the BDA labeled terminals were GABA positive, while more than a third were GABA negative. All the postsynaptic profiles were GABA negative. These results indicate the cMRF provides inhibitory feedback to the ipsilateral side of the SC, but it has more complex effects on the contralateral side. The ipsilateral projection may help tune the "winner-take-all" mechanism that produces a unified saccade signal, while the contralateral projections may contribute to the coordination of activity between the two colliculi.

KSC-07pd1506

NASA Image and Video Library

2007-06-13

KENNEDY SPACE CENTER, FLA. -- Technicians at Astrotech are preparing the Dawn spacecraft for spin-balance testing. After the test, Dawn will then be mated to the upper stage booster, installed into a spacecraft transportation canister for the trip to Cape Canaveral Air Force Station and mated to the Delta II rocket at Launch Pad 17-B. The Dawn spacecraft will employ ion propulsion to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail these largest protoplanets that have remained intact since their formations. Ceres and Vesta reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1508

NASA Image and Video Library

2007-06-13

KENNEDY SPACE CENTER, FLA. -- At Astrotech, the Dawn spacecraft is ready for spin-balance testing. After the test, Dawn will then be mated to the upper stage booster, installed into a spacecraft transportation canister for the trip to Cape Canaveral Air Force Station and mated to the Delta II rocket at Launch Pad 17-B. The Dawn spacecraft will employ ion propulsion to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail these largest protoplanets that have remained intact since their formations. Ceres and Vesta reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1507

NASA Image and Video Library

2007-06-13

KENNEDY SPACE CENTER, FLA. -- Technicians at Astrotech check the Dawn spacecraft before spin-balance testing. After the test, Dawn will then be mated to the upper stage booster, installed into a spacecraft transportation canister for the trip to Cape Canaveral Air Force Station and mated to the Delta II rocket at Launch Pad 17-B.The Dawn spacecraft will employ ion propulsion to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail these largest protoplanets that have remained intact since their formations. Ceres and Vesta reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1505

NASA Image and Video Library

2007-06-13

KENNEDY SPACE CENTER, FLA. -- Technicians at Astrotech prepare the Dawn spacecraft for spin-balance testing. After the test, Dawn will then be mated to the upper stage booster, installed into a spacecraft transportation canister for the trip to Cape Canaveral Air Force Station and mated to the Delta II rocket at Launch Pad 17-B. The Dawn spacecraft will employ ion propulsion to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail these largest protoplanets that have remained intact since their formations. Ceres and Vesta reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

Anomalous aspects of magnetosheath flow and of the shape and oscillations of the magnetopause during an interval of strongly northward interplanetary magnetic field

NASA Technical Reports Server (NTRS)

Chen, Sheng-Hsien; Kivelson, Margaret G.; Gosling, Jack T.; Walker, Raymond T.; Lazarus, Allan J.

1992-01-01

On 15 Feb. 1978, the orientation of the interplanetary magnetic field (IMF) remained steadily northward for more than 12 hours. The ISEE 1 and 2 spacecraft were located near apogee on the dawn side flank of the magnetotail. IMP 8 was almost symmetrically located in the magnetosheath on the dusk flank and IMP 7 was upstream in the solar wind. Using plasma and magnetic field data, we show the following: (1) the magnetosheath flow speed on the flanks of the magnetotail steadily exceeded the solar wind speed by 20 percent; (2) surface waves with approximately a 5-min period and very non-sinusoidal waveform were persistently present on the dawn magnetopause and waves of similar period were present in the dusk magnetosheath; and (3) the magnetotail ceased to flare at an antisunward distance of 15 R(sub E). We propose that the acceleration of the magnetosheath flow is achieved by magnetic tension in the draped field configuration for northward IMF and that the reduction of tail flaring is consistent with a decreased amount of open magnetic flux and a larger standoff distance of the subsolar magnetopause. Results of a three-dimensional magnetohydrodynamic simulation support this phenomenological model.

Dawn song in natural and artificial continuous day: Light pollution affects songbirds at high latitudes.

PubMed

Derryberry, Elizabeth P

2017-10-01

In Focus: Da Silva, A., & Kempenaers, B. (2017). Singing from North to South: Latitudinal variation in timing of dawn singing under natural and artificial light conditions. Journal of Animal Ecology, 86, 1286-1297. doi: 10.1111/1365-2656.12739 Satellite images of the world at night show bright dots connected by glowing lines crisscrossing the globe. As these connect-the-dots become brighter and expand into more and more remote regions, much of the flora and fauna of the world are experiencing evolutionarily unprecedented levels of light at night. Light cues are essential to most physiological and behavioural processes, and so the need to measure the effects of light pollution on these processes is critical. In this issue, Da Silva and Kempenaers take on this task using an important reproductive behaviour in songbirds-dawn song. The geographic, temporal and taxonomic breadth of sampling in this study allows for a close examination of a potentially complex interaction between light pollution and natural variation in the behaviour of dawn singing across latitude, season and species. Their extensive dataset highlights complexity in how songbirds respond to light pollution. Although light pollution has a strong effect on the timing of dawn song, not all songbirds respond the same way to light pollution, and the effects of light pollution vary with changes in natural light levels. Early dawn singers show more flexibility in the timing of dawn song across the season and across latitudes than late dawn singers, and also appear less affected by light pollution at high latitudes than are late dawn singers. These findings suggest that not all songbirds are responding to artificial continuous daylight as they do to natural continuous daylight, highlighting the general need to measure the fitness effects of light pollution. © 2017 The Author. Journal of Animal Ecology © 2017 British Ecological Society.

1. View of engine terminal complex looking westnorthwest from east ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. View of engine terminal complex looking west-northwest from east side of Phillips Drive. Shown are (left to right) the south roundhouse, the machine and blacksmith shops, the storehouse, the oil house, and the coaling sation (behind the oil house in this view). - Central Railroad of New Jersey, Engine Terminal, Jersey City, Hudson County, NJ

A peptide N-terminal protection strategy for comprehensive glycoproteome analysis using hydrazide chemistry based method

PubMed Central

Huang, Junfeng; Qin, Hongqiang; Sun, Zhen; Huang, Guang; Mao, Jiawei; Cheng, Kai; Zhang, Zhang; Wan, Hao; Yao, Yating; Dong, Jing; Zhu, Jun; Wang, Fangjun; Ye, Mingliang; Zou, Hanfa

2015-01-01

Enrichment of glycopeptides by hydrazide chemistry (HC) is a popular method for glycoproteomics analysis. However, possible side reactions of peptide backbones during the glycan oxidation in this method have not been comprehensively studied. Here, we developed a proteomics approach to locate such side reactions and found several types of the side reactions that could seriously compromise the performance of glycoproteomics analysis. Particularly, the HC method failed to identify N-terminal Ser/Thr glycopeptides because the oxidation of vicinal amino alcohol on these peptides generates aldehyde groups and after they are covalently coupled to HC beads, these peptides cannot be released by PNGase F for identification. To overcome this drawback, we apply a peptide N-terminal protection strategy in which primary amine groups on peptides are chemically blocked via dimethyl labeling, thus the vicinal amino alcohols on peptide N-termini are eliminated. Our results showed that this strategy successfully prevented the oxidation of peptide N-termini and significantly improved the coverage of glycoproteome. PMID:25959593

Termination of String Rewriting Rules that have One Pair of Overlaps

NASA Technical Reports Server (NTRS)

Geser, Alfons; Bushnell, Dennis M. (Technical Monitor)

2002-01-01

This paper presents a partial solution to the long standing open problem of termination of one-rule string rewriting. Overlaps between the two sides of the rule play a central role in existing termination criteria. We characterize termination of all one-rule string rewriting systems that have one such overlap at either end. This both completes a result of Kurth and generalizes a result of Shikishima-Tsuji et al.

78 FR 77684 - Change in Bank Control Notices; Acquisitions of Shares of a Bank or Bank Holding Company

Federal Register 2010, 2011, 2012, 2013, 2014

2013-12-24

... Hennepin Avenue, Minneapolis, Minnesota 55480-0291: 1. Dawn Crane, Fosston, Minnesota, individually and as trustee; Lorri Skeie-Campbell, Rio Rancho, New Mexico, individually and as trustee; Dawn M. Skeie Crane Irrevocable Trust; Dawn Crane, as co- trustee; Lorri J. Skeie-Campbell Irrevocable Trust, Winger, and Lorri...

Dawn LAMO Image 188

NASA Image and Video Library

2016-10-07

NASA's Dawn spacecraft views Oxo Crater (6 miles, 10 kilometers wide) in this view from Ceres. Dawn took this image on June 4, 2016, from its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) above the surface. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20950

KSC-07pd1248

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers begin black light testing on the solar panels of the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

KSC-07pd1249

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers begin black light testing on the solar panels of the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

Level-2 Milestone 3244: Deploy Dawn ID Machine for Initial Science Runs

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

Fox, D

2009-09-21

This report documents the delivery, installation, integration, testing, and acceptance of the Dawn system, ASC L2 milestone 3244: Deploy Dawn ID Machine for Initial Science Runs, due September 30, 2009. The full text of the milestone is included in Attachment 1. The description of the milestone is: This milestone will be a result of work started three years ago with the planning for a multi-petaFLOPS UQ-focused platform (Sequoia) and will be satisfied when a smaller ID version of the final system is delivered, installed, integrated, tested, accepted, and deployed at LLNL for initial science runs in support of SSP mission.more » The deliverable for this milestone will be a LA petascale computing system (named Dawn) usable for code development and scaling necessary to ensure effective use of a final Sequoia platform (expected in 2011-2012), and for urgent SSP program needs. Allocation and scheduling of Dawn as an LA system will likely be performed informally, similar to what has been used for BlueGene/L. However, provision will be made to allow for dedicated access times for application scaling studies across the entire Dawn resource. The milestone was completed on April 1, 2009, when science runs began running on the Dawn system. The following sections describe the Dawn system architecture, current status, installation and integration time line, and testing and acceptance process. A project plan is included as Attachment 2. Attachment 3 is a letter certifying the handoff of the system to a nuclear weapons stockpile customer. Attachment 4 presents the results of science runs completed on the system.« less

Jets Galore

NASA Image and Video Library

2010-11-04

This enhanced image, one of the closest taken of comet Harley 2 by NASA EPOXI mission, shows jets and where they originate from the surface. There are jets outgassing from the sunward side, the night side, and along the terminator.

Continuous glucose monitoring system: dawn period calibration does not change accuracy of the method.

PubMed

Augusto, Gustavo A; Sousa, André G P; Perazo, Marcela N A; Correa-Giannella, Maria L C; Nery, Marcia; Melo, Karla F S de

2009-06-01

Continuous glucose monitoring system is a valuable instrument to measure glycemic control, which uses a retrospective calibration based upon 3 to 4 capillary glucose meter values inserted by the patient each day. We evaluated the interference of calibration during the dawn period in the system accuracy. The monitoring data were retrospectively divided into two groups: with (Group A) or without (Group B) the dawn period calibration (between 1:00 and 5:00 AM). Accuracy of the method was expressed by relative absolute difference. Thirty-four continuous glucose monitoring data were evaluated comprising a total of 112 nights. A total of 289 paired readings were analyzed - 195 in Group A and 94 in Group B. We did not find a difference in relative absolute difference (RAD%) in any analyzed period of day by adding dawn calibration. These data suggest that dawn calibration does not alter accuracy of method.

Sequential segmental terminal lenticular side-cut dissection for safe and effective small-incision lenticule extraction in thin lenticules.

PubMed

Jacob, Soosan; Agarwal, Amar; Mazzotta, Cosimo; Agarwal, Athiya; Raj, John Michael

2017-04-01

Small-incision lenticule extraction may be associated with complications such as partial lenticular dissection, torn lenticule, lenticular adherence to cap, torn cap, and sub-cap epithelial ingrowth, some of which are more likely to occur during low-myopia corrections. We describe sequential segmental terminal lenticular side-cut dissection to facilitate minimally traumatic and smooth lenticular extraction. Anterior lamellar dissection is followed by central posterior lamellar dissection, leaving a thin peripheral rim and avoiding the lenticular side cut. This is followed by sequential segmental dissection of the lenticular side cut in a manner that fixates the lenticule and provides sufficient resistance for smooth and complete dissection of the posterior lamellar cut without undesired movements of the lenticule. The technique is advantageous in thin lenticules, where the risk for complications is high, but can also be used in thick lenticular dissection using wider sweeps to separate the lenticular side cut sequentially. Copyright © 2017 ASCRS and ESCRS. Published by Elsevier Inc. All rights reserved.

KSC-07pd1306

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. -- Inside Astrotech's Hazardous Processing Facility, the Dawn spacecraft is weighed before fueling. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Charisse Nahser

KSC-07pd0851

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- Two trucks (one air-ride, one flat-bed) deliver the Dawn spacecraft, as well as additional electrical and ground support equipment and xenon ground support equipment, to Astrotech. Dawn will be moved from the truck and the shipping container removed. The spacecraft will then be moved into the high bay of the Payload Processing Facility. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

A Perfect View of Vesta: Creating Pointing Observations for the Dawn Spacecraft on Asteroid 4 Vesta

NASA Technical Reports Server (NTRS)

Hay, Katrina M.

2005-01-01

The Dawn spacecraft has a timely and clever assignment in store. It will take a close look at two intact survivors from the dawn of the solar system (asteroids 4 Vesta and 1 Ceres) to understand more about solar system origin and evolution. To optimize science return, Dawn must make carefully designed observations on approach and in survey orbit, high altitude mapping orbit, and low altitude mapping orbit at each body. In this report, observations outlined in the science plan are modeled using the science opportunity analyzer program for the Vesta encounter. Specifically, I encoded Dawn's flight rules into the program, modeled pointing profiles of the optical instruments (framing camera, visible infrared spectrometer) and mapped their fields of view onto Vesta's surface. Visualization of coverage will provide the science team with information necessary to assess feasibility of alternative observation plans. Dawn launches in summer 2006 and ends its journey in 2016. Instrument observations on Vesta in 2011 will supply detailed information about Vesta's surface and internal structure. These data will be used to analyze the formation and history of the protoplanet and, therefore, complete an important step in understanding the development of our solar system.

KSC-07pd2423

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- The Dawn spacecraft is moved out of the Astrotech Space Operations facility, on its way to Launch Pad 17-B at Cape Canaveral Air Force Station. At the pad, Dawn will be lifted into the mobile service tower and prepared for mating with the awaiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd2444

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- In the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, workers remove the lower segments of the transportation canister away from the Dawn spacecraft. After removal of the canister, Dawn will be mated with the waiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. EDT Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jim Grossmann

Plasma circulation in Jupiter's magnetosphere

NASA Astrophysics Data System (ADS)

Chané, E.

2017-12-01

We are using our three-dimensional global MHD model of Jupiter's magnetosphere to study the plasma circulation in the magnetodisk. We show that the Iogenic plasma does not travel outward axisymmetrically but rather forms a long spiral arm of high density corotating with the planet. This leads to periodic phenomena in the magnetodisk: for instance, every rotation period, a region of high density is rapidly moving outward on the pre-noon sector. This leads to shearing motions that generate field aligned currents and periodically affect the main oval in this sector.We will also show how the interplanetary magnetic field influences the position of the magnetodisk in our simulations, displacing the current sheet above and below the equatorial plan. We will discuss how this is affecting the depleted flux-tubes returning from the night-side after unloading most of their plasma in the magnetotail (Vasyliunas cycle) and see how they can then move above or below the magnetodisk when arriving at dawn and then reconnect with the interplanetary magnetic field on the day-side.

Modeling Magnetotail Ion Distributions with Global Magnetohydrodynamic and Ion Trajectory Calculations

NASA Technical Reports Server (NTRS)

El-Alaoui, M.; Ashour-Abdalla, M.; Raeder, J.; Peroomian, V.; Frank, L. A.; Paterson, W. R.; Bosqued, J. M.

1998-01-01

On February 9, 1995, the Comprehensive Plasma Instrumentation (CPI) on the Geotail spacecraft observed a complex, structured ion distribution function near the magnetotail midplane at x approximately -30 R(sub E). On this same day the Wind spacecraft observed a quiet solar wind and an interplanetary magnetic field (IMF) that was northward for more than five hours, and an IMF B(sub y) component with a magnitude comparable to that of the RAF B(sub z) component. In this study, we determined the sources of the ions in this distribution function by following approximately 90,000 ion trajectories backward in time, using the time-dependent electric and magnetic fields obtained from a global MHD simulation. The Wind observations were used as input for the MHD model. The ion distribution function observed by Geotail at 1347 UT was found to consist primarily of particles from the dawn side low latitude boundary layer (LLBL) and from the dusk side LLBL; fewer than 2% of the particles originated in the ionosphere.

Lunar Radio Telescopes: A Staged Approach for Lunar Science, Heliophysics, Astrobiology, Cosmology, and Exploration

NASA Technical Reports Server (NTRS)

Lazio, Joseph; Bowman, Judd D.; Burns, Jack O.; Farrell, W. M.; Jones, D. L.; Kasper, J. C.; MacDowall, R. J.; Stewart, K. P.; Weiler, K.

2012-01-01

Observations with radio telescopes address key problems in cosmology, astrobiology, heliophysics, and planetary science including the first light in the Universe (Cosmic Dawn), magnetic fields of extrasolar planets, particle acceleration mechanisms, and the lunar ionosphere. The Moon is a unique science platform because it allows access to radio frequencies that do not penetrate the Earth's ionosphere and because its far side is shielded from intense terrestrial emissions. The instrument packages and infrastructure needed for radio telescopes can be transported and deployed as part of Exploration activities, and the resulting science measurements may inform Exploration (e.g., measurements of lunar surface charging). An illustrative roadmap for the staged deployment of lunar radio telescopes

The Z1 truss begins its ride up the RSS on Launch Pad 39A

NASA Technical Reports Server (NTRS)

2000-01-01

With the onset of dawn, the payload canister (left) with the Integrated Truss Structure Z1 inside begins its journey up the side of the Rotating Service Structure to the Payload Changeout Room. There the Z1 truss will be removed and later transferred to Space Shuttle Discovery's payload bay. The Z1 truss is the first of 10 that will become the backbone of the International Space Station, eventually stretching the length of a football field. Along with its companion payload, the third Pressurized Mating Adapter, the Z1 is scheduled to be launched aboard Discovery Oct. 5 at 9:38 p.m. EDT.

Pre-Dawn Clouds Over Mars

NASA Image and Video Library

1997-08-28

These are more wispy blue clouds from Sol 39 as seen by the Imager for Mars Pathfinder. The bright clouds near the bottom are about 30 degrees above the horizon. The clouds are believed to be at an altitude of 10 to 15 km, and are thought to be made of small water ice particles. The picture was taken about 35 minutes before sunrise. Sojourner spent 83 days of a planned seven-day mission exploring the Martian terrain, acquiring images, and taking chemical, atmospheric and other measurements. The final data transmission received from Pathfinder was at 10:23 UTC on September 27, 1997. Although mission managers tried to restore full communications during the following five months, the successful mission was terminated on March 10, 1998. http://photojournal.jpl.nasa.gov/catalog/PIA00919

Dawn LAMO Image 175

NASA Image and Video Library

2016-09-20

NASA's Dawn spacecraft obtained this view of Laukumate Crater (19 miles, 30 kilometers wide) on Ceres on June 2, 2016. Laukumate is named for a Latvian goddess of agriculture. Dawn took this image from its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) above the surface. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20937

Dawn LAMO Image 185

NASA Image and Video Library

2016-10-04

NASA's Dawn spacecraft spies Achita Crater on Ceres in this view. Achita is named for a Nigerian god of agriculture and is 25 miles (40 kilometers) wide. Dawn took this image on June 3, 2016, from its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) above the surface. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20947

KSC-07pd1227

NASA Image and Video Library

2007-05-16

KENNEDY SPACE CENTER, FLA. -- In Hangar A&O at Cape Canaveral Air Force Station, the Delta II second stage for the Dawn spacecraft is ready for transfer to the launch pad. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/Jack Pfaller

KSC-07pd1244

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers prepare to deploy the solar panels of the Dawn spacecraft. The panels will be tested and undergo black light inspection. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

Climatology of the inter-hemispheric field-aligned currents system over the Nigeria ionosphere

NASA Astrophysics Data System (ADS)

Bolaji, O. S.; Rabiu, A. B.; Oyeyemi, E. O.; Yumoto, K.

2012-11-01

Records of the declination (D) magnetic field data for the year 2009 from the Magnetic Data Acquisition System (MAGDAS) facilities at University of Ilorin were employed for this work. From the minutes value of the D-component, the deduced hourly values of the D-component (Sq(QD)) were used to estimate its diurnal (Sq(D)) values with the most five quietest days identified. The monthly mean (MSq(D)) of the most five quietest days and their seasonal (SSq(D)) variabilities were investigated. The inter-hemispheric field aligned currents (IHFACs) exhibit downward and upward inter-hemispheric field-aligned sheet current that appears as a pair at all local times of the Sq(D), MSq(D), and SSq(D) variations. From these variabilities, the IHFACs were observed to flow from the winter to summer hemisphere during noon and dusk sector and flowing in opposite direction during the dawn sector. The Sq(D) variability patterns that were observed in May, June, August September are gentle compared to the disturbed variabilities in January, February, March and November. The highest positive (˜1.7 arc-min) and negative (˜-2.7 arc min) MSq(D) maxima values were observed in August during the dawn and noon sectors respectively. These values indicated that the IHFACs flow in August is strongly southbound (positive) and northbound (negative) in the dawn and noon sectors respectively. Dusk-side IHFACs as can be observed by MAGDAS are weakly northbound in all the seasons. The direction of IHFACs does not flip at the equinoxes but in June and November and does not become largest at solstices but in August. The IHFACs was observed to exhibit longitudinal variability, which indicated that larger amplitude of winter-to-summer IHFACs is observed to be greater in June solstice (northbound/negative IHFACs) than in the December solstice (southbound/positive IHFACs) during the noon sector.

Preliminary Geological Map of the Ac-H-5 Fejokoo Quadrangle of Ceres: An Integrated Mapping Study Using Dawn Spacecraft Data

NASA Astrophysics Data System (ADS)

Hughson, K.; Russell, C.; Williams, D. A.; Buczkowski, D.; Mest, S. C.; Scully, J. E. C.; Hiesinger, H.; Platz, T.; Ruesch, O.; Schenk, P.; Frigeri, A.; Jaumann, R.; Roatsch, T.; Preusker, F.; Nathues, A.; Hoffmann, M.; Schäfer, M.; Park, R. S.; Marchi, S.; De Sanctis, M. C.; Raymond, C. A.

2015-12-01

In order to enable methodical geologic mapping of the surface of Ceres the Dawn Science Team divided its surface into fifteen quadrangles. A preliminary map of the Fejokoo quadrangle is presented here. This region, located between 21˚-66˚N and 270-0˚E, hosts four primary features: (1) the centrally located, 90 km diameter, distinctly hexagonal impact crater Fejokoo; (2) a small unnamed crater midway up the eastern boundary of the quadrangle which contains and is surrounded by bright material; (3) an unnamed degraded crater NW of Fejokoo that contains lobate material deposits on both sides of the crater's S rim; and (4) a heavily cratered unit in the NW portion of the quadrangle. Key objectives for the ongoing mapping of this quadrangle are to assess the types of processes that may be responsible for the creation of the hexagonal Fejokoo crater, identifying the source and nature of the bright material on the eastern boundary, establishing possible mechanisms for the emplacement of lobate material deposits in Fejokoo and the unnamed crater to its NW, and establishing a detailed geological history of the quadrangle. The Fejokoo region is not associated with any major albedo feature identified by the Hubble Space Telescope (Li et al., 2006). At the time of this writing geologic mapping was performed using Framing Camera (FC) mosaics from the Approach (1.3 km/px) and Survey (415 m/px) orbits, including grayscale and color images and digital terrain models derived from stereo images. Future images from the High Altitude Mapping Orbit (140 m/px) and Low Altitude Mapping Orbit (35 m/px) will be used to refine the maps. Support of the Dawn Instrument, Operations, and Science Teams is acknowledged. This work is supported by grants from NASA, and from the German and Italian Space Agencies.

Multi-point observations of Ion Dispersions near the Exterior Cusp with Cluster

NASA Astrophysics Data System (ADS)

Escoubet, C.-Philippe; Grison, Benjamin; Berchem, Jean; Trattner, Kralheinz; Pitout, Frederic; Richard, Robert; Taylor, Matt; Soucek, Jan; Laakso, Harri; Masson, Arnaud; Dunlop, Malcolm; Dandouras, Iannis; Reme, Henri; Fazakerley, Andrew; Daly, Patrick

2014-05-01

The exterior cusp is the most external region of the polar magnetosphere in direct contact with the plasma and the magnetic field from the solar wind. Unlike the rest of the magnetopause surface, the exterior cusp is a singular region with small and turbulent magnetic field and where large entry of plasma from solar origin takes place. The main process that injects solar wind plasma into the polar cusp is now generally accepted to be magnetic reconnection. Depending on the IMF direction, this process will take place equatorward (for IMF southward), poleward (for IMF northward) or on the dusk or dawn sides (for IMF azimuthal) of the cusp. We report a Cluster crossing on 5 January 2002 near the exterior cusp on the southern dusk side. The IMF was mainly azimuthal (IMF-By around -5 nT), the solar wind speed lower than usual around 280 km/s and the density around 5 cm-3. The four Cluster spacecraft were still in the "magnetotail" configuration with two perfect tetrahedra of 2000 km around apogee and turning into an elongated configuration near the magnetopause. C4 was the first spacecraft to enter the cusp around 19:52:04 UT, followed by C2 at 19:52:35 UT, C1 at 19:54:24 UT and C3 at 20:13:15 UT. C4 and C1 observed two ion energy dispersions at 20:10 UT and 20:40 UT and C3 at 20:35 UT and 21:15 UT. Using the time of flight technique on the upgoing and downgoing ions in the dispersions, we obtain an altitude of the sources of these ions between 14 and 20 RE. Using Tsyganenko model, these sources are located on the dusk flank, past the terminator. In addition, before entering the cusp, the magnetopause crossing was characterized by a large shear in By and bipolar plasma flows, suggesting that reconnection was taking place near the exterior cusp. We will discuss the extent of the reconnection line along the flank of the magnetopause based on these observations.

Dawn Mission Education and Public Outreach: Science as Human Endeavor

NASA Astrophysics Data System (ADS)

Cobb, W. H.; Wise, J.; Schmidt, B. E.; Ristvey, J.

2012-12-01

Dawn Education and Public Outreach strives to reach diverse learners using multi-disciplinary approaches. In-depth professional development workshops in collaboration with NASA's Discovery Program, MESSENGER and Stardust-NExT missions focusing on STEM initiatives that integrate the arts have met the needs of diverse audiences and received excellent evaluations. Another collaboration on NASA ROSES grant, Small Bodies, Big Concepts, has helped bridge the learning sequence between the upper elementary and middle school, and the middle and high school Dawn curriculum modules. Leveraging the Small Bodies, Big Concepts model, educators experience diverse and developmentally appropriate NASA activities that tell the Dawn story, with teachers' pedagogical skills enriched by strategies drawn from NSTA's Designing Effective Science Instruction. Dawn mission members enrich workshops by offering science presentations to highlight events and emerging data. Teachers' awareness of the process of learning new content is heightened, and they use that experience to deepen their science teaching practice. Activities are sequenced to enhance conceptual understanding of big ideas in space science and Vesta and Ceres and the Dawn Mission 's place within that body of knowledge Other media add depth to Dawn's resources for reaching students. Instrument and ion engine interactives developed with the respective science team leads help audiences engage with the mission payload and the data each instrument collects. The Dawn Dictionary, an offering in both audio as well as written formats, makes key vocabulary accessible to a broader range of students and the interested public. Further, as Dawn E/PO has invited the public to learn about mission objectives as the mission explored asteroid Vesta, new inroads into public presentations such as the Dawn MissionCast tell the story of this extraordinary mission. Asteroid Mapper is the latest, exciting citizen science endeavor designed to invite the general public into the thrill of NASA science. Helping teachers develop a picture of the history and evolution of our understanding of the solar system, and honing in on the place of asteroids in helping us answer old questions and discover new ones, students and the general public sees the power and excitement underlying planetary science as human endeavor. Research indicates that science inquiry is powerful in the classroom and mission scientists are real-life models of science inquiry in action. Cross-curricular elements include examining research-based strategies for enhancing English language learners' ability to engage in higher order questions and a professional astronomy artist's insight into how visual analysis requires not just our eyes engaged, but our brains: comparing, synthesizing, questioning, evaluating, and wondering. Dawn Education and Public Outreach will share out perspectives and lessons learned, backed by extensive evaluation examining the efficacy of the mission's efforts.

Use of Cumulative Degradation Factor Prediction and Life Test Result of the Thruster Gimbal Assembly Actuator for the Dawn Flight Project

NASA Technical Reports Server (NTRS)

Lo, C. John; Brophy, John R.; Etters, M. Andy; Ramesham, Rajeshuni; Jones, William R., Jr.; Jansen, Mark J.

2009-01-01

The Dawn Ion Propulsion System is the ninth project in NASA s Discovery Program. The Dawn spacecraft is being developed to enable the scientific investigation of the two heaviest main-belt asteroids, Vesta and Ceres. Dawn is the first mission to orbit two extraterrestrial bodies, and the first to orbit a main-belt asteroid. The mission is enabled by the onboard Ion Propulsion System (IPS) to provide the post-launch delta-V. The three Ion Engines of the IPS are mounted on Thruster Gimbal Assembly (TGA), with only one engine operating at a time for this 10-year mission. The three TGAs weigh 14.6 kg.

Analysis of Temperature Maps of Selected Dawn Data Over the Surface of Vesta

NASA Technical Reports Server (NTRS)

Tosi, F.; Capria, M. T.; DeSanctis, M. C.; Palomba, E.; Grassi, D.; Capaccioni, F.; Ammannito, E.; Combe, J.-Ph.; Sunshine, J. M.; McCord, T. B.;

Polysaccharides from the envelopes of heterocysts and spores of the blue-green algae Anabaena variabilis and Cylindrospermum licheniforme

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

Cardemil, L.; Wolk, C.P.

The polysaccharides from the envelopes of heterocysts of Cylindrospermum licheniforme Kutz., and of heterocysts and spores of Anabaena variabilis Kutz., like those from the differentiated cells of Anabaena cylindrica Lemm., have a 1,3-linked backbone consisting of glucosyl and mannosyl residues in a molar ratio of approximately 3:1. As is the case with A. cylindrica the polysaccharides from A. variabilis and from the heterocysts of C. licheniforme have terminal xylosyl and galactosyl residues as side branches. In addition, the polysaccharide from C. licheniforme resembles that from A. cylindrica in having terminal mannosyl residues as side branches (absent from A. variabilis). Themore » polysaccharides from A. variabilis resemble that from A. cylindrica in having glucose-containing side branches (absent from the heterocyst polysaccharide from C. licheniforme), but in contrast to the polysaccharides from the other two species they also have terminal arabinosyl residues as side branches. All of the polysaccharides mentioned appear to be structurally related; we present tentative structures for those not previously investigated. In contrast, the envelope of spores of C. licheniforme contains only a largely 4-linked galactan. The bulk of this envelope is not polysaccharide in nature, and contains aromatic groups.« less

KSC-07pd1509

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- The second stage of the Delta II launch vehicle for the Dawn spacecraft arrives on Launch Pad 17-B at Cape Canaveral Air Force Station where it will be mated with the first stage. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1256

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, the Dawn spacecraft is lowered toward a work stand for solar panel installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

KSC-07pd1260

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers prepare the Dawn spacecraft for installation of its solar array panels. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

KSC-07pd0856

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Payload Processing Facility, a crane lifts the shipping container from the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

KSC-07pd1246

NASA Image and Video Library

2007-05-21

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, the solar panels of the Dawn spacecraft are extended to their full extent. The panels will be tested and undergo black light inspection. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/George Shelton

Dawn Orbit Determination Team: Modeling and Fitting of Optical Data at Vesta

NASA Technical Reports Server (NTRS)

Kennedy, Brian; Abrahamson, Matt; Ardito, Alessandro; Haw, Robert; Mastrodemos, Nicholas; Nandi, Sumita; Park, Ryan; Rush, Brian; Vaughan, Andrew

2013-01-01

The Dawn spacecraft was launched on September 27th, 2007. Its mission is to consecutively rendezvous with and observe the two largest bodies in the main asteroid belt, Vesta and Ceres. It has already completed over a year's worth of direct observations of Vesta (spanning from early 2011 through late 2012) and is currently on a cruise trajectory to Ceres, where it will begin scientific observations in mid-2015. Achieving this data collection required careful planning and execution from all Dawn operations teams. Dawn's Orbit Determination (OD) team was tasked with reconstruction of the as-flown trajectory as well as determination of the Vesta rotational rate, pole orientation and ephemeris, among other Vesta parameters. Improved knowledge of the Vesta pole orientation, specifically, was needed to target the final maneuvers that inserted Dawn into the first science orbit at Vesta. To solve for these parameters, the OD team used radiometric data from the Deep Space Network (DSN) along with optical data reduced from Dawn's Framing Camera (FC) images. This paper will de-scribe the initial determination of the Vesta ephemeris and pole using a combination of radiometric and optical data, and also the progress the OD team has made since then to further refine the knowledge of Vesta's body frame orientation and rate with these data.

Cosmic Dawn Science Interest Group

NASA Astrophysics Data System (ADS)

Lazio, T. Joseph W.; Cosmic Origins Program Analysis Group

2016-01-01

Cosmic Dawn was identified as one of the three science objectives for this decade in the _New Worlds, New Horizons_ Decadal report, and it will likely continue to be a research focus well into the next decade. Cosmic Dawn refers to the interval during which the Universe transitioned from a nearly completely neutral state back to a nearly fully ionized state and includes the time during which the first stars formed and the first galaxies assembled.The Cosmic Dawn Science Interest Group (SIG) was formed recently under the auspices of the Cosmic Origins Program Analysis Group (COPAG). The Cosmic Dawn SIG focusses on the science cases, observations, and technology development needed to address the "great mystery" of Cosmic Origins. The reach of this SIG is broad, involving the nature of the first stars and the detectability of gamma-ray bursts at high redshifts, the extent to which the first galaxies and first supermassive black holes grew together, and the technology required to pursue these questions.For further information, consult the Cosmic Dawn SIG Web site http://cd-sig.jpl.nasa.gov/ and join the mailing list (by contacting the author).Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

Effects of artificial dawn on subjective ratings of sleep inertia and dim light melatonin onset.

PubMed

Giménez, Marina C; Hessels, Martijn; van de Werken, Maan; de Vries, Bonnie; Beersma, Domien G M; Gordijn, Marijke C M

2010-07-01

The timing of work and social requirements has a negative impact on performance and well-being of a significant proportion of the population in our modern society due to a phenomenon known as social jetlag. During workdays, in the early morning, late chronotypes, in particular, suffer from a combination of a nonoptimal circadian phase and sleep deprivation. Sleep inertia, a transient period of lowered arousal after awakening, therefore, becomes more severe. In the present home study, the authors tested whether the use of an alarm clock with artificial dawn could reduce complaints of sleep inertia in people having difficulties in waking up early. The authors also examined whether these improvements were accompanied by a shift in the melatonin rhythm. Two studies were performed: Study 1: three conditions (0, 50, and 250 lux) and Study 2: two conditions (0 lux and self-selected dawn-light intensity). Each condition lasted 2 weeks. In both studies, the use of the artificial dawn resulted in a significant reduction of sleep inertia complaints. However, no significant shift in the onset of melatonin was observed after 2 weeks of using the artificial dawn of 250 lux or 50 lux compared to the control condition. A multilevel analysis revealed that only the presence of the artificial dawn, rather than shift in the dim light melatonin onset or timing of sleep offset, is related to the observed reduction of sleep inertia complaints. Mechanisms other than shift of circadian rhythms are needed to explain the positive results on sleep inertia of waking up with a dawn signal.

Sleepless in Town – Drivers of the Temporal Shift in Dawn Song in Urban European Blackbirds

PubMed Central

Nordt, Anja; Klenke, Reinhard

2013-01-01

Organisms living in urban environments are exposed to different environmental conditions compared to their rural conspecifics. Especially anthropogenic noise and artificial night light are closely linked to urbanization and pose new challenges to urban species. Songbirds are particularly affected by these factors, because they rely on the spread of acoustic information and adjust their behaviour to the rhythm of night and day, e.g. time their dawn song according to changing light intensities. Our aim was to clarify the specific contributions of artificial night light and traffic noise on the timing of dawn song of urban European Blackbirds (Turdus merula). We investigated the onset of blackbird dawn song along a steep urban gradient ranging from an urban forest to the city centre of Leipzig, Germany. This gradient of anthropogenic noise and artificial night light was reflected in the timing of dawn song. In the city centre, blackbirds started their dawn song up to 5 hours earlier compared to those in semi-natural habitats. We found traffic noise to be the driving factor of the shift of dawn song into true night, although it was not completely separable from the effects of ambient night light. We additionally included meteorological conditions into the analysis and found an effect on the song onset. Cloudy and cold weather delayed the onset, but cloud cover was assumed to reflect night light emissions, thus, amplified sky luminance and increased the effect of artificial night light. Beside these temporal effects, we also found differences in the spatial autocorrelation of dawn song onset showing a much higher variability in noisy city areas than in rural parks and forests. These findings indicate that urban hazards such as ambient noise and light pollution show a manifold interference with naturally evolved cycles and have significant effects on the activity patterns of urban blackbirds. PMID:23940759

Relationship of Topside Ionospheric Ion Outflows to Auroral Forms and Precipitations, Plasma Waves, and Convection Observed by POLAR

NASA Technical Reports Server (NTRS)

Hirahara, M.; Horwitz, J. L.; Moore, T. E.; Germany, G. A.; Spann, J. F.; Peterson, W. K.; Shelley, E. G.; Chandler, M. O.; Giles, B. L.; Craven, P. D.;

Asymmetries in the location of the Venus and Mars bow shock

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

Zhang, T.L.; Schwingenschuh, K.; Russell, C.T.

1991-02-01

An examination of observations of the position of the terminator bow shock at Venus and Mars shows that the terminator bow shock varies with the angle between the local bow shock normal and the upstream magnetic field, {theta}{sub BN}. The part of the shock on the quasi-parallel side is closer to the planet than the part on the quasi-perpendicular side, a result which had been sggested by an earlier computer simulation by Thomas and Winske (1990). This bow shock asymmetry is observed to be larger at Mars than at Venus.

A complex mechanism determines polarity of DNA replication fork arrest by the replication terminator complex of Bacillus subtilis.

PubMed

Duggin, Iain G; Matthews, Jacqueline M; Dixon, Nicholas E; Wake, R Gerry; Mackay, Joel P

2005-04-01

Two dimers of the replication terminator protein (RTP) of Bacillus subtilis bind to a chromosomal DNA terminator site to effect polar replication fork arrest. Cooperative binding of the dimers to overlapping half-sites within the terminator is essential for arrest. It was suggested previously that polarity of fork arrest is the result of the RTP dimer at the blocking (proximal) side within the complex binding very tightly and the permissive-side RTP dimer binding relatively weakly. In order to investigate this "differential binding affinity" model, we have constructed a series of mutant terminators that contain half-sites of widely different RTP binding affinities in various combinations. Although there appeared to be a correlation between binding affinity at the proximal half-site and fork arrest efficiency in vivo for some terminators, several deviated significantly from this correlation. Some terminators exhibited greatly reduced binding cooperativity (and therefore have reduced affinity at each half-site) but were highly efficient in fork arrest, whereas one terminator had normal affinity over the proximal half-site, yet had low fork arrest efficiency. The results show clearly that there is no direct correlation between the RTP binding affinity (either within the full complex or at the proximal half-site within the full complex) and the efficiency of replication fork arrest in vivo. Thus, the differential binding affinity over the proximal and distal half-sites cannot be solely responsible for functional polarity of fork arrest. Furthermore, efficient fork arrest relies on features in addition to the tight binding of RTP to terminator DNA.

KSC-07pd0860

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Payload Processing Facility, technicians roll the Dawn spacecraft into clean room C for unbagging and further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

KSC-07pd1257

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, the Dawn spacecraft, secure on a work stand, is moved to another room for solar panel installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

KSC-07pd0857

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Payload Processing Facility, a crane is being attached to the Dawn spacecraft to lift it from the transporter. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

KSC-07pd0855

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Payload Processing Facility, a crane is attached to the shipping container to remove it from around the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

KSC-07pd1254

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers prepare the Dawn spacecraft to be moved to a work stand for solar panel installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

KSC-07pd1279

NASA Image and Video Library

2007-05-24

KENNEDY SPACE CENTER, FLA. -- At Astrotech, a suspended set of solar array panels is opened prior to installation on the Dawn spacecraft. Another set was installed previously. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/George Shelton

KSC-07pd1255

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In a clean room at Astrotech, workers stand near while the Dawn spacecraft is lifted and moved toward a work stand for solar panel installation. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

KSC-07pd1259

NASA Image and Video Library

2007-05-22

KENNEDY SPACE CENTER, FLA. -- In another clean room at Astrotech, solar array panels at left are ready to be installed on the Dawn spacecraft, at right. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jack Pfaller

Geomorphological Evidence for Pervasive Ground Ice on Ceres from Dawn Observations of Craters and Flows.

NASA Astrophysics Data System (ADS)

Schmidt, B. E.; Chilton, H.; Hughson, K.; Scully, J. E. C.; Russell, C. T.; Sizemore, H. G.; Nathues, A.; Platz, T.; Bland, M. T.; Schenk, P.; Hiesinger, H.; Jaumann, R.; Byrne, S.; Schorghofer, N.; Ammannito, E.; Marchi, S.; O'Brien, D. P.; Sykes, M. V.; Le Corre, L.; Capria, M. T.; Reddy, V.; Raymond, C. A.; Mest, S. C.; Feldman, W. C.

2015-12-01

Five decades of observations of Ceres' albedo, surface composition, shape and density suggest that Ceres is comprised of both silicates and tens of percent of ice. Historical suggestions of surficial hydrated silicates and evidence for water emission, coupled with its bulk density of ~2100 kg/m3 and Dawn observations of young craters containing high albedo spots support this conclusion. We report geomorphological evidence from survey data demonstrating that evaporative and fluid-flow processes within silicate-ice mixtures are prevalent on Ceres, and indicate that its surface materials contain significant water ice. Here we highlight three classes of features that possess strong evidence for ground ice. First, ubiquitous scalloped and "breached" craters are characterized by mass wasting and by the recession of crater walls in asymmetric patterns; these appear analogous to scalloped terrain on Mars and protalus lobes formed by mass wasting in terrestrial glaciated regions. The degradation of crater walls appears to be responsible for the nearly complete removal of some craters, particularly at low latitudes. Second, several high latitude, high elevation craters feature lobed flows that emanate from cirque-shaped head walls and bear strikingly similar morphology to terrestrial rock glaciers. These similarities include lobate toes and indications of furrows and ridges consistent with ice-cored or ice-cemented material. Other lobed flows persist at the base of crater walls and mass wasting features. Many flow features evidently terminate at ramparts. Third, there are frequent irregular domes, peaks and mounds within crater floors that depart from traditional crater central peaks or peak complexes. In some cases the irregular domes show evidence for high albedo or activity, and thus given other evidence for ice, these could be due to local melt and extrusion via hydrologic gradients, forming domes similar to pingos. The global distribution of these classes of features, combined with latitudinal variation in their abundance and/or appearance, suggests that ground ice is a key controller of geology on Ceres, and that ice content within the surface and subsurface is spatially varied and/or activated by energetic events. Dawn high altitude mapping orbit (HAMO) data will provide better views.

Long term evolution of temperature in the venus upper atmosphere at the evening and morning terminators

NASA Astrophysics Data System (ADS)

Krause, P.; Sornig, M.; Wischnewski, C.; Kostiuk, T.; Livengood, T. A.; Herrmann, M.; Sonnabend, G.; Stangier, T.; Wiegand, M.; Pätzold, M.; Mahieux, A.; Vandaele, A. C.; Piccialli, A.; Montmessin, F.

2018-01-01

This paper contains a comprehensive dataset of long-term observations between 2009 and 2015 at the upper mesosphere/lower thermosphere providing temperature values at different locations of the morning and evening side of the terminator of Venus. Temperature information is obtained by line-resolved spectroscopy of Doppler broadened CO2 transitions features. Results are restricted to a pressure level of 1 μbar, ∼110 km altitude due the nature of the addressed non-LTE CO2 emission line at 10 μm. The required high spectral resolution of the instrumentation is provided by the ground-based spectrometers THIS (University of Cologne) and HIPWAC (NASA GSFC). For the first time upper mesosphere/lower thermosphere temperatures at the Venusian terminator derived from IR-het spectroscopy between 2009 and 2015 are investigated in order to clarify the local-time dependences, latitudinal dependences and the long-term trend. Measured temperatures were distributed in the range between 140 K and 240 K, with mean values equal to 199 K ± 17 K for the morning side of the terminator and 195 K ± 19 K for the evening side of the terminator. Within the uncertainty no difference between the averaged morning and evening terminator side temperature is found. In addition, no strong latitudinal dependency is observed at these near terminator local times. In contrast IR-het data from 2009 show a strong latitudinal dependency at noon, with a temperature difference of around 60 K between the equatorial and polar region (Sonnabend et al., 2012). Accord with the instruments of the Venus Express mission a northern-southern hemispherical symmetry is observed (Mahieux et al., 2012; Piccialli et al., 2015). The data shows no consistent long-term temperature trend throughout the six years of observation, but a variability in the order of tens of Kelvin for the different observing runs representing a time step of few month to two years. This is about the same order of magnitude as the variability within a single run with a typically time range of 2-10 days. This variation is not connected to the solar cycle. Sub-millimeter observations by Clancy et al. found a relation between temperatures and long-term variation in mesospheric water vapor, SO2, and sulfate aerosols (Clancy and Muhleman, 1991; Clancy et al., 2012). SO2 column densities observed by SOIR at the terminator are fairly stable over the time period of 2006-2011 (Mahieux et al., 2015), supporting the hypothesis of a relation between SO2 and temperature variations. The temperatures derived from the infrared heterodyne spectroscopy (IR-het) are compared to results from the Venus Express space mission (VEx). A consistence with the temperatures from the VEx instruments SOIR, VIRTIS and SPICAV is found. As the instruments probe different local time, SPICAV probes the pure nightside, SOIR across the terminator and IR-het the pure dayside atmosphere it is not surprising that the IR-het temperatures are mostly on the warmer side compared to results from SPICAV and SOIR.

Song trait similarity in great tits varies with social structure.

PubMed

Snijders, Lysanne; van der Eijk, Jerine; van Rooij, Erica P; de Goede, Piet; van Oers, Kees; Naguib, Marc

2015-01-01

For many animals, long-range signalling is essential to maintain contact with conspecifics. In territorial species, individuals often have to balance signalling towards unfamiliar potential competitors (to solely broadcast territory ownership) with signalling towards familiar immediate neighbours (to also maintain so-called "dear enemy" relations). Hence, to understand how signals evolve due to these multilevel relationships, it is important to understand how general signal traits vary in relation to the overall social environment. For many territorial songbirds dawn is a key signalling period, with several neighbouring individuals singing simultaneously without immediate conflict. In this study we tested whether sharing a territory boundary, rather than spatial proximity, is related to similarity in dawn song traits between territorial great tits (Parus major) in a wild personality-typed population. We collected a large dataset of automatized dawn song recordings from 72 unique male great tits, during the fertile period of their mate, and compared specific song traits between neighbours and non-neighbours. We show here that both song rate and start time of dawn song were repeatable song traits. Moreover, neighbours were significantly more dissimilar in song rate compared to non-neighbours, while there was no effect of proximity on song rate similarity. Additionally, similarity in start time of dawn song was unrelated to sharing a territory boundary, but birds were significantly more similar in start time of dawn song when they were breeding in close proximity of each other. We suggest that the dissimilarity in dawn song rate between neighbours is either the result of neighbouring great tits actively avoiding similar song rates to possibly prevent interference, or a passive consequence of territory settlement preferences relative to the types of neighbours. Neighbourhood structuring is therefore likely to be a relevant selection pressure shaping variation in territorial birdsong.

KSC-07pd0865

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In clean room C of Astrotech's Payload Processing Facility, technicians dressed in "bunny suits," or clean-room attire, begin working on the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

KSC-07pd1307

NASA Image and Video Library

2007-05-28

KENNEDY SPACE CENTER, FLA. -- The mobile service towers on Launch Pads 17-A (left) and 17-B (right) are silhouetted against the pre-dawn sky at Cape Canaveral Air Force Station. In the background are the launch gantries. Pad 17-B is the site for the launch of the Dawn spacecraft on June 30. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/Amanda Diller

KSC-07pd1212

NASA Image and Video Library

2007-05-16

KENNEDY SPACE CENTER, FLA. -- In Hangar M on Cape Canaveral Air Force Station, the first stage of the Delta II rocket that will launch the Dawn spacecraft is ready to be transferred to a transporter for its move to the launch pad. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/Jack Pfaller

KSC-07pd0864

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- The Dawn spacecraft is seen here in clean room C of Astrotech's Payload Processing Facility. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

Development and Translation of a Tissue-Engineered Disc in a Preclinical Rodent Model

DTIC Science & Technology

2013-10-01

authors Dong Hwa Kim, John T. Martin, Dawn M. Elliott, Lachlan J. Smith , and Robert L. Mauck...Replacement in a Small Animal Model with authors John T. Martin, Andrew H. Milby, Joseph A. Chiaro, Dong Hwa Kim, Nader M. Hebela, Lachlan J. Smith , Dawn... Smith , Dawn M. Elliott, and Robert L. Mauck is now in review. To carry out this study, radiopaque scaffolds were generated from a 14.3% w/v slurry

Dawn LAMO Image 182

NASA Image and Video Library

2016-09-29

NASA's Dawn spacecraft views Kupalo Crater in this view of Ceres. Kupalo, which measures 16 miles (26 kilometers) across and is located at southern mid-latitudes, is named for the Slavic god of vegetation and harvest. Dawn took this image on June 2, 2016, from its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) above the surface. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20944

Dawn LAMO Image 5

NASA Image and Video Library

2016-01-13

This view of the Cerean crater Victa was captured by NASA Dawn spacecraft on Dec. 19, 2015. The steep-walled crater is approximately 19 miles 30 kilometers in diameter, and was named for the Roman goddess of food and nourishment. Dawn took this image from its low-altitude mapping orbit (LAMO), at an approximate altitude of 240 miles (385 kilometers) above Ceres. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20195

Using Dawn to Observe SEP Events Past 2 AU

NASA Astrophysics Data System (ADS)

Villarreal, M. N.; Russell, C. T.; Prettyman, T. H.

2017-12-01

The launch of the STEREO spacecraft provided much insight into the longitudinal and radial distribution of solar energetic particles (SEPs) relative to their origin site. However, almost all of the observations of SEP events have been made exclusively near 1 AU. The Dawn mission, which orbited around Vesta before arriving at Ceres, provides an opportunity to analyze these events at much further distances. Although Dawn's Gamma Ray and Neutron Detector (GRaND) is not optimized for SEP characterization, it is sensitive to protons greater than 4 MeV, making it capable of detecting a solar energetic particle event in its vicinity. Solar energetic particles in this area of the solar system are important as they are believed to cause sputtering at bodies such as Ceres and comets (Villarreal et al., 2017; Wurz et al., 2015). In this study, we use Dawn's GRaND data from 2011-2015 when Dawn was at distances between 2-3 AU. We compare the SEP events seen by Dawn with particle measurements at 1 AU using STEREO, Wind, and ACE to understand how the SEP events evolved past 1 AU.References: Villarreal, M. N., et al. (2017), The dependence of the Cerean exosphere on solar energetic particle events, Astrophys. J. Lett., 838, L8.Wurz, P. et al. (2015), Solar wind sputtering of dust on the surface of 67P/Churyumov-Gerasimenko, A&A, 583, A22.

Dawn LAMO Image 83

NASA Image and Video Library

2016-05-06

Ceres densely cratered landscape is revealed in this image taken by the framing camera aboard NASA Dawn spacecraft. The craters show various degrees of degradation. The youngest craters have sharp rims.

Dawn LAMO Image 84

NASA Image and Video Library

2016-05-09

Ceres densely cratered landscape is revealed in this image taken by the framing camera aboard NASA Dawn spacecraft. The craters show various degrees of degradation. The youngest craters have sharp rims.

Non-parametric entrainment by natural twilight in the microchiropteran bat, Hipposideros speoris inside a cave.

PubMed

Joshi, D S; Vanlalnghaka, C

2005-01-01

The study aimed to determine the influence of repeated natural dawn and dusk twilight pulses in entraining the circadian flight activity rhythm of the microchiropteran bat, Hipposideros speoris, free-running in constant darkness in a natural cave. The bats were exposed to repeated dawn or dusk twilight pulses at eight circadian phases. All bats exposed to dawn twilight pulses were entrained by advancing transients, and the stable entrainment was reached when the onset of activity occurred about 12 h before the lights-on of the pulses, irrespective of the initial phase at which the bats were exposed to twilight. All bats exposed to dusk twilight pulses, however, were entrained by delaying transients, and the stable entrainment was reached when the onset of activity occurred about 1.6 h after the lights-on of the pulses. The entrainment caused by dawn and dusk twilight pulses is discussed in the context of the postulated two photoreceptors: the short wavelength sensitive (S) photoreceptors mediating entrainment via dusk twilight, and the medium wavelength sensitive (M) photoreceptors mediating entrainment via dawn twilight.

KSC-07pd2401

NASA Image and Video Library

2007-09-10

KENNEDY SPACE CENTER, FLA. -- At Astrotech Space Operations in Titusville, Fla., workers move the platform with the Dawn spacecraft. They are preparing to install the transportation canister around Dawn for transfer to Launch Pad 17-B at Cape Canaveral Air Force Station (CCAFS). During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Launch via a Delta II rocket is scheduled in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. Photo credit: NASA/Jim Grossmann

KSC-07pd2445

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- In the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is ready for mating with the waiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. EDT Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jim Grossmann

KSC-07pd2428

NASA Image and Video Library

2007-09-11

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft arrives at the upper level of the mobile service tower. It will be moved inside and prepared for mating with the awaiting Delta II rocket. Dawn is scheduled for launch in a window from 7:25 to 7:54 a.m. Sept. 26 from CCAFS. During its nearly decade-long mission, the Dawn mission will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. To carry out its scientific mission, the Dawn spacecraft will carry a visible camera, a visible and infrared mapping spectrometer, and a gamma ray and neutron spectrometer, whose data will be used in combination to characterize these bodies. In addition to the three instruments, radiometric and optical navigation data will provide data relating to the gravity field and thus bulk properties and internal structure of the two bodies. Data returned from the Dawn spacecraft could provide opportunities for significant breakthroughs in our knowledge of how the solar system formed. Photo credit: NASA/Jack Pfaller

KSC-07pd1514

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the second stage of the Delta II launch vehicle for the Dawn spacecraft is lowered into the hole toward the Delta first stage below. The two stages will be mated. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1512

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- The second stage of the Delta II launch vehicle for the Dawn spacecraft is lifted alongside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station. It will be mated with the first stage already in the tower. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1510

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- The second stage of the Delta II launch vehicle for the Dawn spacecraft is lifted alongside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station. It will be mated with the first stage already in the tower. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

Endomorphin-2 analogs with C-terminal esterification produce potent systemic antinociception with reduced tolerance and gastrointestinal side effects.

PubMed

Wang, Chang-Lin; Qiu, Ting-Ting; Yang, Dai-Jun; Yuan, Bi-Yu; Han, Feng-Tong; Li, Li; Gu, Ning

2017-04-01

C-terminal esterification of opioid peptides may change their opioid activities due to the modified physicochemical properties. In the present study, the pharmacological activities of C-terminal esterified endomorphin-2 (EM-2) analogs 1-3 were characterized by in vitro metabolic stability and octanol/buffer distribution assays. Also, the antinociceptive profiles in the radiant heat paw withdrawal test and related side effects of these analogs were determined. Our results showed that all three analogs significantly increased the metabolic stability and lipophilicity. Moreover, analogs 1-3 displayed potent antinociceptive activities after intracerebroventricular (i.c.v.) administration. Analogs 1 and 3 exhibited about 2-fold higher antinociception than EM-2, and differential opioid mechanisms were involved. In addition, EM-2 at 50 μmol/kg failed to produce any significant antinociceptive activity after subcutaneous (s.c.) administration, whereas equimolar dose of analogs 1-3 produced significant analgesic effects. Analog 3 showed the highest antinociceptive activity after systemic administration, which was consistent with its in vitro stability and lipophilicity. We further evaluated the antinociceptive tolerance of analogs 1-3. In acute tolerance test, analogs 1-3 shifted the dose-response curves rightward by only 1.4-3.2 fold as determined by tolerance ratio, whereas EM-2 by 5.6-fold, demonstrating reduced antinociceptive tolerance. Also, analogs 1 and 2 decreased chronic antinociceptive tolerance by central and peripheral administration of drugs. In particular, analogs 3 displayed insignificant chronic antinociceptive tolerance. Furthermore, analogs 1-3 were less prone to induce gastrointestinal side effects at analgesic doses. The present investigation gave the evidence that C-terminal esterified modifications of EM-2 will facilitate the development of novel opioid analgesics with reduced side effects. Copyright © 2016 Elsevier Ltd. All rights reserved.

Dawn at Vesta: testing the protoplanetary paradigm

USGS Publications Warehouse

Russell, C.T.; Raymond, C.A.; Coradini, A.; McSween, H.Y.; Zuber, M.T.; Nathues, A.; DeSanctis, Maria-Cristina; Jaumann, R.; Konopliv, A.S.; Preusker, F.; Asmar, S.W.; Park, R.S.; Gaskell, R.; Keller, H.U.; Mottola, S.; Roatsch, T.; Scully, J.E.C.; Smith, D.E.; Tricarico, P.; Toplis, M.J.; Christensen, U.R.; Feldman, W.C.; Lawrence, D.J.; McCoy, T.J.; Prettyman, T.H.; Reedy, R.C.; Sykes, M.E.; Titus, T.N.

2012-01-01

The Dawn spacecraft targeted 4 Vesta, believed to be a remnant intact protoplanet from the earliest epoch of solar system formation, based on analyses of howardite-eucrite-diogenite (HED) meteorites that indicate a differentiated parent body. Dawn observations reveal a giant basin at Vesta's south pole, whose excavation was sufficient to produce Vesta-family asteroids (Vestoids) and HED meteorites. The spatially resolved mineralogy of the surface reflects the composition of the HED meteorites, confirming the formation of Vesta's crust by melting of a chondritic parent body. Vesta's mass, volume, and gravitational field are consistent with a core having an average radius of 107 to 113 kilometers, indicating sufficient internal melting to segregate iron. Dawn's results confirm predictions that Vesta differentiated and support its identification as the parent body of the HEDs.

In-Flight Operation of the Dawn Ion Propulsion System - The First Nine Months

NASA Technical Reports Server (NTRS)

Garner, Charles E.; Brophy, John R.; Mikes, Steven C.; Raymond, Marc D.

2008-01-01

The Dawn mission, part of NASA's Discovery Program, has as its goal the scientific exploration of the two most massive main-belt asteroids, Vesta and Ceres. The Dawn spacecraft was launched from Cape Canaveral Air Force Station on September 27, 2007 on a Delta-II 7925H-9.5 (Delta-II Heavy) rocket that placed the 1218 kg spacecraft into an Earth-escape trajectory. On-board the spacecraft is an ion propulsion system (IPS) which will provide most of the delta-V needed for heliocentric transfer to Vesta, orbit capture at Vesta, transfer to Vesta science orbits, departure and escape from Vesta, heliocentric transfer to Ceres, orbit capture at Ceres, and transfer to Ceres science orbits. The Dawn ion engine design is based on the design validated on NASA's Deep Space 1 mission. However, because of the very substantial (11 km/s) delta-V requirements for this mission Dawn requires two engines to complete its mission objectives. The power processor units (PPU), digital control and interface units (DCIU) slice boards and the xenon control assembly (XCA) are also based on the DS1 design. The DCIUs and thrust gimbal assemblies (TGA) were developed at the Jet Propulsion Laboratory. The spacecraft was provided by Orbital Sciences Corporation, Sterling, Virginia, and the mission is managed by and operated from the Jet Propulsion Laboratory. Dawn partnered with Germany, Italy and Los Alamos National Laboratory for the science instruments. The mission is led by the principal investigator, Dr. Christopher Russell, from the University of California, Los Angeles. The first 80 days after launch were dedicated to the initial checkout of the spacecraft prior to the initiation of long-term thrusting for the heliocentric transfer to Vesta. The IPS hardware, consisting of three ion thrusters and TGAs, two PPUs and DCIUs, xenon feed system, and spacecraft control software, was investigated extensively. Thrust measurements, roll torque measurements, pointing capabilities, control characteristics, and thermal behavior of the spacecraft and IPS were carefully evaluated. The Dawn IPS fully met all its initial checkout performance objectives. Deterministic thrusting for cruise began on December 17, 2007. Over the subsequent approximately 330 days the IPS will be operated virtually continuously at full power thrusting (approximately 91 mN) leading to a Mars flyby in February 2009. The encounter with Mars provides a gravity assist for a plane change and is the only source of post-launch delta-V apart from the IPS. Following the Mars gravity assist IPS will be operated for approximately one year at full power and for 1.3 years at throttled power levels leading to rendezvous with Vesta in August of 2011. Following nine months of orbital operations with IPS providing the propulsion needed for orbit capture, science orbit transfer and orbit maintenance and Vesta escape, Dawn will transit to Ceres with an expected arrival date of February 2015. As of June 16, 2008 the ion thrusters on Dawn have operated for close to 3,846 hours and have delivered nearly 1 km/s of delta-V to the spacecraft. Dawn IPS operation has been almost flawless during the initial checkout and six months of cruise. This paper provides an overview of Dawn's mission objectives, mission and system design, and the results of the post-launch Dawn IPS mission operations through June 2008

Overview of the Martian nightside suprathermal electron depletions

NASA Astrophysics Data System (ADS)

Steckiewicz, Morgane; Garnier, Philippe; André, Nicolas; Mitchell, David; Andersson, Laila; Penou, Emmanuel; Beth, Arnaud; Fedorov, Andrei; Sauvaud, Jean-André; Mazelle, Christian; Lillis, Robert; Brain, David; Espley, Jared; McFadden, James; Halekas, Jasper; Luhmann, Janet; Soobiah, Yasir; Jakosky, Bruce

2017-04-01

Nightside suprathermal electron depletions have been observed at Mars by three spacecraft to date: Mars Global Surveyor (MGS), Mars EXpress (MEX) and the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. The global coverage of Mars by MEX and MGS at high altitudes (above approximately 250 km) revealed that these structures were mostly observed above strong crustal magnetic field sources which exclude the electrons coming from the dayside or from the tail. The MAVEN orbit now offers the possibility to observe this phenomenon at low altitudes, down to 125 km. A transition region near 170 km has been detected separating the collisional region where electron depletions are mainly due to electron absorption by atmospheric CO2 and the collisionless region where they are mainly due to closed crustal magnetic field loops. MAVEN is now in its third year of data recording and has covered a large range of latitudes, local times and solar zenith angles at low altitudes (<900km) in the nightside. These observations enable us to estimate where the EUV terminator is located, based on the observation that no electron depletions are expected above its location. Through this study the location of the EUV terminator appears to be raised on average by 125 km above the location of the geometrical terminator. However, this location is likely to be different between the dawn and dusk terminator and to vary throughout the different Martian seasons. This coverage has also allowed the observation of regions with recurrent absence of electron depletions even below the transition region near 170 km altitude. These 'no-depletion' areas are localized above the least magnetized area of Mars both in the Northern and Southern hemispheres. A modification in the CO2 density, gravity waves, or the presence of current sheets are potential drivers for that phenomenon.

The dominant role of side chains in supramolecular double helical organisation in synthetic tripeptides

NASA Astrophysics Data System (ADS)

Sharma, Ankita; Tiwari, Priyanka; Dutt Konar, Anita

2018-06-01

Peptide self-assembled nanostructures have attracted attention recently owing to their promising applications in diversified avenues. To validate the importance of sidechains in supramolecular architectural stabilization, herein this report describes the self-assembly propensities involving weak interactions in a series of model tripeptides Boc-Xaa-Aib-Yaa-OMe I-IV, (where Xaa = 4-F-Phe/NMeSer/Ile & Yaa = Tyr in peptide I-III respectively and Xaa = 4-F-Phe & Yaa = Ile in peptide IV) differing in terminal side chains. The solid state structural analysis reveals that tripeptide (I) displays supramolecular preference for double helical architecture. However, when slight modification has been introduced in the N-terminal side chains disfavour the double helical organisation (Peptide II and III). Indeed the peptides display sheet like ensemble within the framework. Besides replacement of C-terminal Tyr by Ile in peptide I even do not promote the architecture, emphasizing the dominant role of balance of side chains in stabilizing double helical organisation. The CD measurements, concentration dependant studies, NMR titrations and ROESY spectra are well in agreement with the solid state conformational investigation. Moreover the morphological experiments utilizing FE-SEM, support the heterogeneity present in the peptides. Thus this work may not only hold future promise in understanding the structure and function of neurodegenerative diseases but also assist in rational design of protein modification in biologically active peptides.

Distribution and morphological characteristics of the interstitial cells of Cajal in the ileocaecal junction of the guinea-pig.

PubMed

Miyamoto-Kikuta, Sachiko; Ezaki, Taichi; Komuro, Terumasa

2009-10-01

The guinea-pig ileocaecal junction including the valve was studied by immunohistochemistry to clarify the organization of the muscle bundles, the enteric nerves and the interstitial cells of Cajal (ICC). This region clearly exhibited characteristic features in the distribution patterns of ICC in a proximal to distal direction: (1) the thickened portion of the terminal ileum immediately adjacent to the ileocecal junction contained many ICC throughout the circular (ICC-CM) and longitudinal (ICC-LM) muscle layers, but ICC were few or absent in the rest of the ileum; (2) the ileal side of the valve contained ICC associated with the deep muscular plexus (ICC-DMP) as in the small intestine, whereas ICC-DMP were absent in the caecal side as in the caecum; (3) the valve contained many ICC-CM and ICC-LM in both the ileal and caecal sides; (4) many ICC associated with the myenteric plexus were observed in both the ileal and caecal sides of the valve, whereas they were only sparsely found in the caecum; (5) ICC were also observed around the submucosal plexus in a confined area of the terminal ileum and the ileocaecal valve. These observations provide morphological evidence that the terminal ileum and ileocaecal valve are specially equipped for their active involvement in the movement of the junctional area.

Hydrogen-terminated diamond vertical-type metal oxide semiconductor field-effect transistors with a trench gate

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

Inaba, Masafumi, E-mail: inaba-ma@ruri.waseda.jp; Muta, Tsubasa; Kobayashi, Mikinori

2016-07-18

The hydrogen-terminated diamond surface (C-H diamond) has a two-dimensional hole gas (2DHG) layer independent of the crystal orientation. A 2DHG layer is ubiquitously formed on the C-H diamond surface covered by atomic-layer-deposited-Al{sub 2}O{sub 3}. Using Al{sub 2}O{sub 3} as a gate oxide, C-H diamond metal oxide semiconductor field-effect transistors (MOSFETs) operate in a trench gate structure where the diamond side-wall acts as a channel. MOSFETs with a side-wall channel exhibit equivalent performance to the lateral C-H diamond MOSFET without a side-wall channel. Here, a vertical-type MOSFET with a drain on the bottom is demonstrated in diamond with channel current modulationmore » by the gate and pinch off.« less

Meet EPA researcher Dawn King

EPA Pesticide Factsheets

Research microbiologist Dawn King works in EPA’s National Exposure Research Laboratory where she identifies and assesses the health risk of microbial pathogens in water. This is her researchers at work profile.

Dawn HAMO Image 67

NASA Image and Video Library

2015-12-01

The tall, cone-shaped mountain Ahuna Mons is seen in this image taken by NASA's Dawn spacecraft. Ahuna Mons, named for the traditional post-harvest festival of the Sumi tribe of Nagaland in India, is about 4 miles (6 kilometers) tall and 12 miles (20 kilometers) in diameter. Dawn took this image on Oct. 14, 2015, from an altitude of 915 miles (1,470 kilometers). It has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20130

Dawn LAMO Image 158

NASA Image and Video Library

2016-08-25

An area along the rim of the crater at the center of this view from NASA Dawn spacecraft, has collapsed, producing a lobe-shaped feature where the material settled. The image is centered at approximately 52 degrees north latitude, 316 degrees east longitude. NASA's Dawn spacecraft took this image on May 28, 2016, from its low-altitude mapping orbit, at a distance of about 240 miles (385 kilometers) above the surface of Ceres. The image resolution is 120 feet (35 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20880

KSC-07pd0861

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In clean room C of Astrotech's Payload Processing Facility, a worker wears a "bunny suit," or clean-room attire, next to the Dawn spacecraft, which will be unbagged and undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

KSC-07pd0852

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- At Astrotech, the shipping container holding the Dawn spacecraft is removed from the truck. The container will then be moved into the high bay of the Payload Processing Facility and the spacecraft removed. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

KSC-07pd1281

NASA Image and Video Library

2007-05-24

KENNEDY SPACE CENTER, FLA. -- At Astrotech, workers prepare the Dawn spacecraft, at left, for installation of a second set of solar array panels, at right. Together, the panels extend 64.6 feet when fully open. Dawn is scheduled to launch June 30 aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Photo credit: NASA/George Shelton

KSC-07pd0854

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- At Astrotech, the shipping container holding the Dawn spacecraft is moved into the high bay of the Payload Processing Facility. The spacecraft will next be removed from the container. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

A three-sided rearrangeable switching network for a binary fat tree

NASA Astrophysics Data System (ADS)

Yen, Mao-Hsu; Yu, Chu; Shin, Haw-Yun; Chen, Sao-Jie

2011-06-01

A binary fat tree needs an internal node to interconnect the left-children, right-children and parent terminals to each other. In this article, we first propose a three-stage, 3-sided rearrangeable switching network for the implementation of a binary fat tree. The main component of this 3-sided switching network (3SSN) consists of a polygonal switch block (PSB) interconnected by crossbars. With the same size and the same number of switches as our 3SSN, a three-stage, 3-sided clique-based switching network is shown to be not rearrangeable. Also, the effects of the rearrangeable structure and the number of terminals on the network switch-efficiency are explored and a proper set of parameters has been determined to minimise the number of switches. We derive that a rearrangeable 3-sided switching network with switches proportional to N 3/2 is most suitable to interconnect N terminals. Moreover, we propose a new Polygonal Field Programmable Gate Array (PFPGA) that consists of logic blocks interconnected by our 3SSN, such that the logic blocks in this PFPGA can be grouped into clusters to implement different logic functions. Since the programmable switches usually have high resistance and capacitance and occupy a large area, we have to consider the effect of the 3SSN structure and the granularity of its cluster logic blocks on the switch efficiency of PFPGA. Experiments on benchmark circuits show that the switch and speed performances are significantly improved. Based on the experimental results, we can determine the parameters of PFPGA for the VLSI implementation.

Solar Terminator Waves in the Ionosphere Measured by the Wallops Island, VA Dynasonde

NASA Astrophysics Data System (ADS)

Zabotin, N. A.; Song, H.; Bullett, T. W.

2017-12-01

Solar terminator represents a unique source of atmospheric waves possessing of near-ideal coherent properties: its geometry and magnitude of the impact changes very little from day to day. This feature has been used in [Forbes et al., GRL, 2008] to obtain "snapshots" of terminator waves in the neutral atmosphere at the altitude 400 km by averaging CHAMP accelerometer data over relatively long sequences of the satellite passes. The results were represented in the geographic latitude vs local time coordinates. We apply a similar approach averaging time series of Wallops Island, VA Dynasonde Doppler data to obtain "snapshots" of terminator waves in the ionosphere in the true altitude vs local "terminator time" coordinates. The averaging is performed independently for every month of the yearlong observation period from May 2013 to April 2014. The altitude range covered is 90 km to 400 km with 2 km resolution, representing the entire bottom-side ionosphere. Individual local time segments used for the averaging were 12 hours long and all centered at the times of the sunrise or sunset terminator passing at every specific altitude. This procedure effectively suppresses all kinds of incoherent wave activity and allows one to reveal the perturbation phenomenon mainly caused by the solar terminator. This is an important advantage of this technique compared to multiple "terminator wave" studies based on simple time coincidence. Both sunrise and sunset terminator waves are easily visualized in all of the monthly images. Our results confirm observations of [Forbes et al., GRL, 2008] of the wave structures existing on both sides of the terminator. The phase fronts of the sunset terminator wave are propagating downward indicating upward movement of the terminator-related disturbance and of the wave energy generated by it. The phase fronts of the sunrise terminator waves are propagating upward indicating downward movement of the terminator-related disturbance and of the wave energy generated by it. Spectral analysis of the local time sequences reveals characteristic peaks in the terminator-related wave activity corresponding to the periods 40-60 min and 2 hours. We also analyze statistics of their horizontal wavelengths.

Dawn LAMO Image 87

NASA Image and Video Library

2016-05-12

This image from NASA Dawn spacecraft shows the rim of Occator crater, just east of the area containing the brightest spots on Ceres. The crater rim has collapsed, leaving structures geologists refer to as terraces.

NMR studies of excluded volume interactions in peptide dendrimers.

PubMed

Sheveleva, Nadezhda N; Markelov, Denis A; Vovk, Mikhail A; Mikhailova, Maria E; Tarasenko, Irina I; Neelov, Igor M; Lähderanta, Erkki

2018-06-11

Peptide dendrimers are good candidates for diverse biomedical applications due to their biocompatibility and low toxicity. The local orientational mobility of groups with different radial localization inside dendrimers is important characteristic for drug and gene delivery, synthesis of nanoparticles, and other specific purposes. In this paper we focus on the validation of two theoretical assumptions for dendrimers: (i) independence of NMR relaxations on excluded volume effects and (ii) similarity of mobilities of side and terminal segments of dendrimers. For this purpose we study 1 H NMR spin-lattice relaxation time, T 1H , of two similar peptide dendrimers of the second generation, with and without side fragments in their inner segments. Temperature dependences of 1/T 1H in the temperature range from 283 to 343 K were measured for inner and terminal groups of the dendrimers dissolved in deuterated water. We have shown that the 1/T 1H temperature dependences of inner groups for both dendrimers (with and without side fragments) practically coincide despite different densities of atoms inside these dendrimers. This result confirms the first theoretical assumption. The second assumption is confirmed by the 1/T 1H temperature dependences of terminal groups which are similar for both dendrimers.

SPERTI Terminal Building (PER604). Oblique view of front entry and ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

SPERT-I Terminal Building (PER-604). Oblique view of front entry and one side. Electrical transformers at right of building. Note "Butler" logo. Photographer: R.G. Larsen. Date: June 22, 1955. INEEL negative no. 55-1700 - Idaho National Engineering Laboratory, SPERT-I & Power Burst Facility Area, Scoville, Butte County, ID

SPERTI Terminal Building (PER604). Concrete foundation is at grade. Steel ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

SPERT-I Terminal Building (PER-604). Concrete foundation is at grade. Steel frame has been erected, and some siding has been affixed. Photographer: R.G. Larsen. Date: April 22, 1955. INEEL negative no. 55-1003 - Idaho National Engineering Laboratory, SPERT-I & Power Burst Facility Area, Scoville, Butte County, ID

Amorphous silicon cell array powered solar tracking apparatus

DOEpatents

Hanak, Joseph J.

1985-01-01

An array of an even number of amorphous silicon solar cells are serially connected between first and second terminals of opposite polarity. The terminals are connected to one input terminal of a DC motor whose other input terminal is connected to the mid-cell of the serial array. Vane elements are adjacent the end cells to selectively shadow one or the other of the end cells when the array is oriented from a desired attitude relative to the sun. The shadowing of one cell of a group of cells on one side of the mid-cell reduces the power of that group substantially so that full power from the group of cells on the other side of the mid-cell drives the motor to reorient the array to the desired attitude. The cell groups each have a full power output at the power rating of the motor. When the array is at the desired attitude the power output of the two groups of cells balances due to their opposite polarity so that the motor remains unpowered.

Dawn HAMO Image 79

NASA Image and Video Library

2015-12-17

NASA Dawn spacecraft captured this scene, showing southern mid-latitudes on Ceres, on Oct. 18, 2015, from an altitude of 915 miles 1,470 kilometers. It has a resolution of 450 feet 140 meters per pixel.

Dawn LAMO Image 73

NASA Image and Video Library

2016-04-22

This image from NASA Dawn spacecraft shows terrain within Chaminuka Crater on Ceres. Chaminuka was named for the spirit who provides rains during times of drought, according to the legends of the Shona people of Zimbabwe.

Dawn LAMO Image 55

NASA Image and Video Library

2016-03-29

This view from NASA Dawn spacecraft shows an area in mid-southern latitudes on Ceres. The crater named Juling 12 miles, 20 kilometers wide is seen at lower right. Bright material is visible along its upper walls.

Dawn LAMO Image 62

NASA Image and Video Library

2016-04-07

Tupo Crater, named for the Polynesian god of turmeric, is shown at upper left in this view of Ceres from NASA Dawn spacecraft. Just below the crater, a line of narrow troughs parallels the rim of Tupo.

KSC-07pd1384

NASA Image and Video Library

2007-06-06

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Hazardous Processing Facility, a technician monitors the loading of xenon for the ion propulsion system in the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Kim Shiflett

KSC-07pd1386

NASA Image and Video Library

2007-06-06

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Hazardous Processing Facility, a technician monitors the loading of xenon for the ion propulsion system in the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Kim Shiflett

KSC-07pd1387

NASA Image and Video Library

2007-06-06

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Hazardous Processing Facility, technicians check data during the loading of xenon for the ion propulsion system in the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Kim Shiflett

KSC-07pd1388

NASA Image and Video Library

2007-06-07

KENNEDY SPACE CENTER, FLA. -- At Astrotech's Hazardous Processing Facility, technicians are loading the Dawn spacecraft with xenon gas for the ion propulsion system. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jim Grossmann

KSC-07pd1385

NASA Image and Video Library

2007-06-06

KENNEDY SPACE CENTER, FLA. -- In Astrotech's Hazardous Processing Facility, technicians check data during the loading of xenon for the ion propulsion system in the Dawn spacecraft. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Kim Shiflett

Dawn Gateway View of Ceres

NASA Image and Video Library

2014-12-05

From about three times the distance from Earth to the moon, NASA's Dawn spacecraft spies its final destination -- the dwarf planet Ceres. The resolution of this image does not yet exceed the best views of Ceres, which were obtained by the Hubble Space Telescope (see PIA10235). Nonetheless, Ceres' spherical shape is clearly revealed here. Sunlight illuminates the dwarf planet from the right, leaving a sliver of the surface in shadow at left. A zoomed-in view is provided in Figure 1, along with the original unmagnified, uncropped view. The image was taken on Dec. 1, 2014 with the Dawn spacecraft's framing camera, using a clear spectral filter. Dawn was about 740,000 miles (1.2 million kilometers) from Ceres at the time. Ceres is 590 miles (950 kilometers) across and was discovered in 1801. http://photojournal.jpl.nasa.gov/catalog/PIA19049

Automated Spectral System for Terrain Classification, Mineralogy of Vesta from the Dawn Framing Cameras

NASA Astrophysics Data System (ADS)

Reddy, V.; Le Corre, L.; Nathues, A.; Hall, I.; Gutierrez-Marques, P.; Hoffmann, M.

2011-10-01

The Dawn mission will rendezvous with asteroid (4) Vesta in July 2011. We have developed a set of equations for extracting mean pyroxene chemistry (Ferrosilite and Wollastonite) for classifying terrains on Vesta by using the Dawn Framing Camera (FC) multi-color bands. The Automated Spectral System (ASS) utilizes pseudo-Band I minima to estimate the mean pyroxene chemistry of diogenites, and basaltic eucrites. The mean pyroxene chemistries of cumulate eucrites, and howardites overlap each other on the pyroxene quadrilateral and hence are harder to distinguish. We expect our ASS to carry a bulk of the terrain classification and mineralogy workload utilizing these equations and complement the work of DawnKey (Le Corre et al., 2011, DPS/EPSC 2011). The system will also provide surface mineral chemistry layers that can be used for mapping Vesta's surface.

Preparing for Dawn's Mission at Ceres: Challenges and Opportunities in the Exploration of a Dwarf Planet

NASA Technical Reports Server (NTRS)

Rayman, Marc D.; Mase, Robert A.

2014-01-01

After escaping from Vesta in 2012, Dawn is continuing its 2.5-year flight to dwarf planet Ceres. Investigating this second destination promises to provide a view of an intriguing world of ice and rock, likely displaying fascinating geology entirely unlike any body yet orbited by a spacecraft. Dawn spends the significant majority of the time thrusting with its ion propulsion system to deliver the 3.6 km/s required to rendezvous with Ceres. Meanwhile, the operations team has developed the sequences that will be used there. Following orbit capture in March 2015, Dawn will fly to a series of four circular polar science orbits. The orbits, ranging from about 13,500 km to 375 km in altitude, are designed to optimize the scientific observations. The overall strategy for exploring Ceres is based strongly on the extremely successful 16 months of Vesta operations, during which Dawn met or exceeded all of its objectives. Nevertheless, the loss of two of the spacecraft's four reaction wheels has necessitated some important changes. Based on a very productive hydrazine conservation campaign in the interplanetary cruise and the development of new hydrazine-efficient methods of operating at Ceres, there is good reason to expect that Dawn will be able to accomplish all of its objectives regardless of the health of the reaction wheels. This paper describes the progress in traveling to Ceres as well as the plans for exploring this giant, icy world.

Kefir and health: a contemporary perspective.

PubMed

Ahmed, Zaheer; Wang, Yanping; Ahmad, Asif; Khan, Salman Tariq; Nisa, Mehrun; Ahmad, Hajra; Afreen, Asma

2013-01-01

Kefir and its related products are renowned nutraceutical dairy products produced through fermentation of yeasts and bacteria naturally present in grains of kefir. The nutritional attributes of this self-carbonated beverage are due to presence of vital nutrients such as carbohydrates, proteins, minerals, vitamins, and some nutraceutical components. Antimicrobial activity, better gut health, anticarcinogenic activity, control on serum glucose and cholesterol, control on lactose intolerance and better immune system can be achieved through its regular consumption. Moreover, on the one side kefir is good dietetic beverage, and of particular interest of athletes, and on the other side the whole kefir is good for feeding small babies and pre-schoolers for good tolerance against disease and quick weight gain. Lots of works have been done on kefir from a health point of view. This study summarizes all the data that have been compiled to date. The purpose of this review is to gather information about microbiological, chemical, nutritional, and therapeutic aspects of kefir and kefir-like products to provide justification for its consumption. This review leads us to conclude that kefir begins a new dawn of food for the mankind.

Lunar Surface Potential Increases during Terrestrial Bow Shock Traversals

NASA Technical Reports Server (NTRS)

Collier, Michael R.; Stubbs, Timothy J.; Hills, H. Kent; Halekas, Jasper; Farrell, William M.; Delory, Greg T.; Espley, Jared; Freeman, John W.; Vondrak, Richard R.; Kasper, Justin

2009-01-01

Since the Apollo era the electric potential of the Moon has been a subject of interest and debate. Deployed by three Apollo missions, Apollo 12, Apollo 14 and Apollo 15, the Suprathermal Ion Detector Experiment (SIDE) determined the sunlit lunar surface potential to be about +10 Volts using the energy spectra of lunar ionospheric thermal ions accelerated toward the Moon. We present an analysis of Apollo 14 SIDE "resonance" events that indicate the lunar surface potential increases when the Moon traverses the dawn bow shock. By analyzing Wind spacecraft crossings of the terrestrial bow shock at approximately this location and employing current balancing models of the lunar surface, we suggest causes for the increasing potential. Determining the origin of this phenomenon will improve our ability to predict the lunar surface potential in support of human exploration as well as provide models for the behavior of other airless bodies when they traverse similar features such as interplanetary shocks, both of which are goals of the NASA Lunar Science Institute's Dynamic Response of the Environment At the Moon (DREAM) team.

Field-aligned currents, convection electric fields, and ULF-ELF waves in the cusp

NASA Technical Reports Server (NTRS)

Saflekos, N. A.; Potemra, T. A.; Kintner, P. M., Jr.; Green, J. L.

1979-01-01

Nearly simultaneous observations from the Triad and Hawkeye satellites over the Southern Hemisphere, at low altitudes near the noon meridian and close to the usual polar cusp latitudes, show that in and near the polar cusp there exist several relationships between field-aligned currents (FACs), convection electric fields, ULF-ELF magnetic noise, broadband electrostatic noise and interplanetary magnetic fields. The most important findings are (1) the FACs directed into the ionosphere in the noon-to-dusk local time sector and directed away from the ionosphere in the noon-to-dawn local time sector and identified as region-1 permanent FACs (Iijima and Potemra, 1976a) and are located equatorward of the regions of antisunward (westward) convection; (2) the observations are consistent with a two-cell convection pattern symmetric in one case (throat positioned at noon) and asymmetric in another (throat located in a sector on the forenoon side in juxtaposition to the region of strong convection on the afternoon side); and (3) fine-structure FACs are responsible for the generation of ULF-ELF noise in the polar cusp.

Positioning of the carboxamide side chain in 11-oxo-11H-indeno[1,2-b]quinolinecarboxamide anticancer agents: effects on cytotoxicity.

PubMed

Deady, L W; Desneves, J; Kaye, A J; Finlay, G J; Baguley, B C; Denny, W A

2001-02-01

A series of 11-oxo-11H-indeno[1,2-b]quinolines bearing a carboxamide-linked cationic side chain at various positions on the chromophore was studied to determine structure-activity relationships between cytotoxicity and the position of the side chain. The compounds were prepared by Pfitzinger synthesis from an appropriate isatin and 1-indanone, followed by various oxidative steps, to generate the required carboxylic acids. The 4- and 6-carboxamides (with the side chain on a terminal ring, off the short axis of the chromophore) were effective cytotoxins. The dimeric 4- and 6-linked analogues were considerably more cytotoxic than the parent monomers, but had broadly similar activities. In contrast, analogues with side chains at the 8-position (on a terminal ring but off the long axis of the chromophore) or 10-position (off the short axis of the chromophore but in a central ring) were drastically less effective. The 4,10- and 6,10-biscarboxamides had activities between those of the corresponding parent monocarboxamides. The first of these showed good activity against advanced subcutaneous colon 38 tumours in mice.

Concerning the Motion of FTEs and Attendant Signatures

NASA Technical Reports Server (NTRS)

Sibeck, David G.

2010-01-01

We employ the Cooling et al. [2001] model to predict the location, orientation, and motion of flux transfer events (FTEs) generated along finite length component and anti parallel reconnection lines for typical solar wind plasma conditions and various interplanetary magnetic field (IMF) orientations in the plane perpendicular to the SunEarth line at the solstices and equinoxes. For duskward and northward or southward IMF orientations, events formed by component reconnection originate along reconnection curves passing through the sub solar point that tilt from southern dawn to northern dusk. They maintain this orientation as they move either northward into the northern dawn quadrant or southward into the southern dusk quadrant. By contrast, events formed by antiparallel reconnection originate along reconnection curves running from northern dawn to southern dusk in the southern dawn and northern dusk quadrants and maintain these orientations as they move anti sunward into both these quadrants. Although both the component and antiparallel reconnection models can explain previously reported event orientations on the southern dusk magnetopause during intervals of northward and dawn ward IMF orientation, only the component model explains event occurrence near the subsolar magnetopause during intervals when the IMF does not point due southward.

KSC-07pd1511

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- The second stage of the Delta II launch vehicle for the Dawn spacecraft is lifted alongside the mobile service tower on Launch Pad 17-B at Cape Canaveral Air Force Station. At right can be seen the solid rocket boosters surrounding Delta's first stage. The second stage will be mated with the first stage. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

KSC-07pd1513

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, the second stage of the Delta II launch vehicle for the Dawn spacecraft arrives at the upper level of the mobile service tower. It will be moved inside the tower and mated with the first stage already in the tower. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

Dawn: An Ion-Propelled Journey to the Beginning of the Solar System

NASA Technical Reports Server (NTRS)

Brophy, John R.; Rayman, Marc D.; Pavri, Betina

2008-01-01

The Dawn mission is designed to perform a scientific investigation of the two heaviest mainbelt asteroids Vesta and Ceres. These bodies are believed to preserve records of the physical and chemical conditions present during the formation of the solar system. The mission uses an ion propulsion system to enable the single Dawn spacecraft and its complement of scientific instruments to orbit both of these asteroids. Dawn's three science instruments - the gamma ray and neutron detector, the visible and infrared mapping spectrometer, and the primary framing camera - were successfully tested after launch and are functioning normally. The ion propulsion system includes three ion thrusters of the type flown previously on NASA's Deep Space 1 mission. A minimum of two ion thrusters is necessary to accomplish the Dawn mission. Checkout of two of the ion thrusters was completed as planned within 30 days after launch. This activity confirmed that the spacecraft has two healthy ion thrusters. While further checkout activities are still in progress, the activities completed as of the end of October indicate that the spacecraft is well on its way toward being ready for the start of the thrusting-cruise phase of the mission beginning December 15th.

Dawn Orbit Determination Team : Trajectory Modeling and Reconstruction Processes at Vesta

NASA Technical Reports Server (NTRS)

Abrahamson, Matt; Ardito, Alessandro; Han, Don; Haw, Robert; Kennedy, Brian; Mastrodemos, Nicholas; Nandi, Sumita; Park, Ryan; Rush, Brian; Vaughan, Andrew

2013-01-01

The NASA Dawn spacecraft was launched on September 27, 2007 on a mission to study the asteroid belt's two largest objects, Vesta and Ceres. It is the first deep space orbiting mission to demonstrate solar-electric ion propulsion, providing the necessary delta-V to enable capture and escape from two extraterrestrial bodies. At this time, Dawn has completed its science campaign at Vesta and is currently on its journey to Ceres, where it will arrive in mid-2015. The spacecraft spent over a year in orbit around Vesta from July 2011 through August 2012, capturing science data during four dedicated orbit phases. In order to maintain the reference orbits necessary for science and enable the transfers between those orbits, precise and timely orbit determination was required. The constraints associated with low-thrust ion propulsion coupled with the relatively unknown a priori gravity and rotation models for Vesta presented unique challenges for the Dawn orbit determination team. While [1] discusses the prediction performance of the orbit determination products, this paper discusses the dynamics models, filter configuration, and data processing implemented to deliver a rapid orbit determination capability to the Dawn project.

Limits to Mercury's Magnesium Exosphere from MESSENGER Second Flyby Observations

NASA Technical Reports Server (NTRS)

Sarantos, Menelaos; Killen, Rosemary M.; McClintock, William E.; Bradley, E. Todd; Vervack, Ronald J., Jr.; Benna, Mehdi; Slavin, James A.

2011-01-01

The discovery measurements of Mercury's exospheric magnesium, obtained by the MErcury Surface. Space ENvironment, GEochemistry. and Ranging (MESSENGER) probe during its second Mercury flyby, are modeled to constrain the source and loss processes for this neutral species. Fits to a Chamberlain exosphere reveal that at least two source temperatures are required to reconcile the distribution of magnesium measured far from and near the planet: a hot ejection process at the equivalent temperature of several tens of thousands of degrees K, and a competing, cooler source at temperatures as low as 400 K. For the energetic component, our models indicate that the column abundance that can be attributed to sputtering under constant southward interplanetary magnetic field (IMF) conditions is at least a factor of five less than the rate dictated by the measurements, Although highly uncertain, this result suggests that another energetic process, such as the rapid dissociation of exospheric MgO, may be the main source of the distant neutral component. If meteoroid and micrometeoroid impacts eject mainly molecules, the total amount of magnesium at altitudes exceeding approximately 100 km is found to be consistent with predictions by impact vaporization models for molecule lifetimes of no more than two minutes. Though a sharp increase in emission observed near the dawn terminator region can be reproduced if a single meteoroid enhanced the impact vapor at equatorial dawn, it is much more likely that observations in this region, which probe heights increasingly near the surface, indicate a reservoir of volatile Mg being acted upon by lower-energy source processes.

The Morphology of the Solar Wind Magnetic Field Draping on the Dayside of Mars and Its Variability

NASA Astrophysics Data System (ADS)

Fang, Xiaohua; Ma, Yingjuan; Luhmann, Janet; Dong, Yaxue; Brain, David; Hurley, Dana; Dong, Chuanfei; Lee, Christina O.; Jakosky, Bruce

2018-04-01

The magnetic field draping pattern in the magnetosheath of Mars is of interest for what it tells us about both the solar wind interaction with the Mars obstacle and the use of the field measured there as a proxy for the upstream interplanetary magnetic field (IMF) clock angle. We apply a time-dependent, global magnetohydrodynamic model toward quantifying the spatial and temporal variations of the magnetic field draping direction on the Martian dayside above 500-km altitude. The magnetic field and plasma are self-consistently solved over one Mars rotation period, with the dynamics of the field morphology considered as the result of the rotation of the crustal field orientation. Our results show how the magnetic field direction on the plane perpendicular to the solar wind flow direction gradually departs from the IMF as the solar wind penetrates toward the obstacle and into the tail region. This clock angle departure occurs mainly inside the magnetic pileup region and tailward of the terminator plane, exhibiting significant dawn-dusk and north-south asymmetries. Inside the dayside sheath region, the field direction has the greatest departure from the IMF-perpendicular component direction downstream of the quasi-parallel bow shock, which for the nominal Parker spiral is over the dawn quadrant. Thus, the best region to obtain an IMF clock angle proxy is within the dayside magnetosheath at sufficiently high altitudes, particularly over subsolar and dusk sectors. Our results illustrate that the crustal field has only a mild influence on the magnetic field draping direction within the magnetosheath region.

Dawn LAMO Image 80

NASA Image and Video Library

2016-05-03

NASA Dawn spacecraft shows Azacca Crater has a prominent set of north-south trending fractures. Its floor is relatively smooth and its rim has terraces descending toward its floor. Azacca was named for the Haitian god of agriculture.

Dawn LAMO Image 25

NASA Image and Video Library

2016-02-11

This image, taken by NASA Dawn spacecraft, shows a densely cratered region within Meanderi Crater on Ceres. Elongated craters in the wall of the largest impact feature are likely the result of material slumping down the crater walls.

Dawn LAMO Image 33

NASA Image and Video Library

2016-02-24

NASA Dawn spacecraft captured this view of a region in the mid-southern latitudes of Ceres. The largest crater in the scene is Fluusa. Fluusa has a densely cratered floor and therefore is interpreted as an old impact feature.

Dawn LAMO Image 32

NASA Image and Video Library

2016-02-23

This image of Ceres from NASA Dawn spacecraft was taken at an oblique viewing angle relative to the surface. The crater to the upper right is named Juling which displays prominent spurs of compacted material along its walls.

High-Resolution Global Geologic Map of Ceres from NASA Dawn Mission

NASA Astrophysics Data System (ADS)

Williams, D. A.; Buczkowski, D. L.; Crown, D. A.; Frigeri, A.; Hughson, K.; Kneissl, T.; Krohn, K.; Mest, S. C.; Pasckert, J. H.; Platz, T.; Ruesch, O.; Schulzeck, F.; Scully, J. E. C.; Sizemore, H. G.; Nass, A.; Jaumann, R.; Raymond, C. A.; Russell, C. T.

2018-06-01

This presentation will discuss the completed 1:4,000,000 global geologic map of dwarf planet Ceres derived from Dawn Framing Camera Low Altitude Mapping Orbit (LAMo) images, combining 15 quadrangle maps.

On the Way to Ceres Artist Concept

NASA Image and Video Library

2013-12-03

This artist concept shows NASA Dawn spacecraft heading toward the dwarf planet Ceres. When Dawn arrives, it will be the first spacecraft to go into orbit around two destinations in our solar system beyond Earth.

Dawn LAMO Image 24

NASA Image and Video Library

2016-02-10

This image, taken by NASA Dawn spacecraft, shows the heavily cratered rim of an older, unnamed impact feature on Ceres. The crater density is almost the same inside and outside, and its wall is also quite battered by impacts.

Two short segments of Smad3 are important for specific interaction of Smad3 with c-Ski and SnoN.

PubMed

Mizuide, Masafumi; Hara, Takane; Furuya, Toshio; Takeda, Masafumi; Kusanagi, Kiyoshi; Inada, Yuri; Mori, Masatomo; Imamura, Takeshi; Miyazawa, Keiji; Miyazono, Kohei

2003-01-03

c-Ski and SnoN are transcriptional co-repressors that inhibit transforming growth factor-beta signaling through interaction with Smad proteins. Among receptor-regulated Smads, c-Ski and SnoN bind more strongly to Smad2 and Smad3 than to Smad1. Here, we show that c-Ski and SnoN bind to the "SE" sequence in the C-terminal MH2 domain of Smad3, which is exposed on the N-terminal upper side of the toroidal structure of the MH2 oligomer. The "QPSMT" sequence, located in the vicinity of SE, supports the interaction with c-Ski and SnoN. Sequences similar to SE and QPSMT are found in Smad2, but not in Smad1. The N-terminal MH1 domain and linker region of Smad3 protrude from the N-terminal upper side of the MH2 oligomer toroid. Smurf2 induces ubiquitin-dependent degradation of SnoN, since it appears to be located close to SnoN through binding to the linker region of Smad2. In contrast, transcription factors Mixer and FoxH3 (FAST1) bind to the bottom side of the Smad3 MH2 toroid; therefore, c-Ski does not affect the interaction of Smads with these transcription factors. Our findings thus demonstrate the stoichiometry of how multiple molecules can associate with the Smad oligomers and how the Smad-interacting proteins functionally interact with each other.

KSC-07pd1239

NASA Image and Video Library

2007-05-17

KENNEDY SPACE CENTER, FLA. -- In the Astrotech Space Operations facility, Orbital Science technicians install a computer chip on the Dawn spacecraft. The silicon chip holds the names of more than 360,000 space enthusiasts worldwide who signed up to participate in a virtual voyage to the asteroid belt and is about the size of an American five-cent coin. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/Jim Grossmann

KSC-07pd0853

NASA Image and Video Library

2007-04-10

KENNEDY SPACE CENTER, FLA. -- At Astrotech, an external cover is removed from around the shipping container holding the Dawn spacecraft. The container will then be moved into the high bay of the Payload Processing Facility and the spacecraft removed. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/Jim Grossmann

KSC-07pd0862

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In clean room C of Astrotech's Payload Processing Facility, a worker wearing a "bunny suit," or clean-room attire, begins removing the protective cover surrounding the Dawn spacecraft. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

KSC-07pd0863

NASA Image and Video Library

2007-04-11

KENNEDY SPACE CENTER, FLA. -- In clean room C of Astrotech's Payload Processing Facility, a worker wearing a "bunny suit," or clean-room attire, looks over the Dawn spacecraft after removing the protective cover, at bottom right. In the clean room, the spacecraft will undergo further processing. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn mission is managed by JPL, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate in Washington, D.C. Photo credit: NASA/George Shelton

Dawn XMO2 Image 29

NASA Image and Video Library

2017-01-11

Ikapati Crater on Ceres is seen at top right in this image from NASA's Dawn spacecraft. Ikapati has a complex of central peaks and roughly parallel fractures on its floor. The crater, named for a Philippine goddess of cultivated lands, measures 31 miles (50 kilometers) in diameter. Dawn took this image on Oct. 24, 2016, during its second extended-mission science orbit (XMO2), from a distance of about 920 miles (1,480 kilometers) above the surface of Ceres. The image resolution is about 460 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA21249

KSC-07pd1238

NASA Image and Video Library

2007-05-17

KENNEDY SPACE CENTER, FLA. -- In the Astrotech Space Operations facility, a computer chip awaits installation on the Dawn spacecraft. The silicon chip holds the names of more than 360,000 space enthusiasts worldwide who signed up to participate in a virtual voyage to the asteroid belt and is about the size of an American five-cent coin. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. Dawn is scheduled to launch June 30 from Launch Complex 17-B. Photo credit: NASA/Jim Grossmann

Chemical Mixing Model and K-Th-Ti Systematics and HED Meteorites for the Dawn Mission

NASA Technical Reports Server (NTRS)

Usui, T.; McSween, H. Y., Jr.; Mittlefehldt, D. W.; Prettyman, T. H.

2009-01-01

The Dawn mission will explore 4 Vesta, a large differentiated asteroid believed to be the parent body of the howardite, eucrite and diogenite (HED) meteorite suite. The Dawn spacecraft carries a gamma-ray and neutron detector (GRaND), which will measure the abundances of selected elements on the surface of Vesta. This study provides ways to leverage the large geochemical database on HED meteorites as a tool for interpreting chemical analyses by GRaND of mapped units on the surface of Vesta.

KSC-07pd2400

NASA Image and Video Library

2007-09-01

KENNEDY SPACE CENTER, FLA. -- This logo represents the mission of the Dawn spacecraft. During its nearly decade-long mission, Dawn will study the asteroid Vesta and dwarf planet Ceres, celestial bodies believed to have accreted early in the history of the solar system. The mission hopes to unlock some of the mysteries of planetary formation, including the building blocks and the processes leading to their state today. The Dawn mission is managed by the Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, Calif., for NASA's Science Mission Directorate in Washington, D.C.

Determination of the pKa of the N-terminal amino group of ubiquitin by NMR

PubMed Central

Oregioni, Alain; Stieglitz, Benjamin; Kelly, Geoffrey; Rittinger, Katrin; Frenkiel, Tom

2017-01-01

Ubiquitination regulates nearly every aspect of cellular life. It is catalysed by a cascade of three enzymes and results in the attachment of the C-terminal carboxylate of ubiquitin to a lysine side chain in the protein substrate. Chain extension occurs via addition of subsequent ubiquitin molecules to either one of the seven lysine residues of ubiquitin, or via its N-terminal α-amino group to build linear ubiquitin chains. The pKa of lysine side chains is around 10.5 and hence E3 ligases require a mechanism to deprotonate the amino group at physiological pH to produce an effective nucleophile. In contrast, the pKa of N-terminal α-amino groups of proteins can vary significantly, with reported values between 6.8 and 9.1, raising the possibility that linear chain synthesis may not require a general base. In this study we use NMR spectroscopy to determine the pKa for the N-terminal α-amino group of methionine1 of ubiquitin for the first time. We show that it is 9.14, one of the highest pKa values ever reported for this amino group, providing a rational for the observed need for a general base in the E3 ligase HOIP, which synthesizes linear ubiquitin chains. PMID:28252051

Electric terminal performance and characterization of solid oxide fuel cells and systems

NASA Astrophysics Data System (ADS)

Lindahl, Peter Allan

Solid Oxide Fuel Cells (SOFCs) are electrochemical devices which can effect efficient, clean, and quiet conversion of chemical to electrical energy. In contrast to conventional electricity generation systems which feature multiple discrete energy conversion processes, SOFCs are direct energy conversion devices. That is, they feature a fully integrated chemical to electrical energy conversion process where the electric load demanded of the cell intrinsically drives the electrochemical reactions and associated processes internal to the cell. As a result, the cell's electric terminals provide a path for interaction between load side electric demand and the conversion side processes. The implication of this is twofold. First, the magnitude and dynamic characteristics of the electric load demanded of the cell can directly impact the long-term efficacy of the cell's chemical to electrical energy conversion. Second, the electric terminal response to dynamic loads can be exploited for monitoring the cell's conversion side processes and used in diagnostic analysis and degradation-mitigating control schemes. This dissertation presents a multi-tier investigation into this electric terminal based performance characterization of SOFCs through the development of novel test systems, analysis techniques and control schemes. First, a reference-based simulation system is introduced. This system scales up the electric terminal performance of a prototype SOFC system, e.g. a single fuel cell, to that of a full power-level stack. This allows realistic stack/load interaction studies while maintaining explicit ability for post-test analysis of the prototype system. Next, a time-domain least squares fitting method for electrochemical impedance spectroscopy (EIS) is developed for reduced-time monitoring of the electrochemical and physicochemical mechanics of the fuel cell through its electric terminals. The utility of the reference-based simulator and the EIS technique are demonstrated through their combined use in the performance testing of a hybrid-source power management (HSPM) system designed to allow in-situ EIS monitoring of a stack under dynamic loading conditions. The results from the latter study suggest that an HSPM controller allows an opportunity for in-situ electric terminal monitoring and control-based mitigation of SOFC degradation. As such, an exploration of control-based SOFC degradation mitigation is presented and ideas for further work are suggested.

Geochemistry at 4 Vesta: Observations Using Fast Neutrons

NASA Technical Reports Server (NTRS)

Lawrence, David J.; Prettyman, Thomas H.; Feldman, William C.; Bazell, David; Mittlefehldt, David W.; Peplowski, Patrick N.; Reedy, Robert C.

2012-01-01

Dawn is currently in orbit around the asteroid 4 Vesta, and one of the major objectives of the mission is to probe the relationship of Vesta to the Howardite, Eucrite, and Diogenite (HED) meteorites. As Vesta is an example of a differentiated planetary embryo, Dawn will also provide fundamental information about planetary evolution in the early solar system [1]. To help accomplish this overall goal, the Dawn spacecraft carries the Gamma-Ray and Neutron Detector (GRaND). GRaND uses planetary gamma-ray and neutron spectroscopy to measure the surface elemental composition of Vesta and will provide information that is unique and complementary to that provided by the other Dawn instruments and investigations. Gamma-ray and neutron spectroscopy is a standard technique for measuring planetary compositions [2], having successfully made measurements at near-Earth asteroids, the Moon, Mars, Mercury and now Vesta. GRaND has made the first measurements of the neutron spectrum from any asteroid (previous asteroid measurements were only made with gamma-rays). Dawn has been collecting data at Vesta since July 2011. The prime data collection period for GRaND is the Low-Altitude Mapping Orbit (LAMO), which started on 12 December 2011 and will last through spring 2012. During LAMO, the Dawn spacecraft orbits at an average altitude of 210 km above the surface of Vesta, which allows good neutron and gamma-ray signals to be detected from Vesta. A description of the overall goals of GRaND and a summary of the initial findings are given elsewhere [3,4]. The subject of this study is to present the information that will be returned from GRaND using fast neutron measurements. Here, we discuss what fast neutrons can reveal about Vesta s surface composition, how such data can address Dawn science goals, and describe fast neutron measurements made in the early portion of the Vesta LAMO phase.

Plasma atrial natriuretic peptide and N-terminal pro B-type natriuretic peptide concentrations in dogs with right-sided congestive heart failure

PubMed Central

KANNO, Nobuyuki; HORI, Yasutomo; HIDAKA, Yuichi; CHIKAZAWA, Seishiro; KANAI, Kazutaka; HOSHI, Fumio; ITOH, Naoyuki

2015-01-01

The clinical utility of plasma natriuretic peptide concentrations in dogs with right-sided congestive heart failure (CHF) remains unclear. We investigated whether plasma levels of atrial natriuretic peptide (ANP) and N-terminal pro B-type natriuretic peptide (NT-proBNP) are useful for assessing the congestive signs of right-sided heart failure in dogs. This retrospective study enrolled 16 healthy dogs and 51 untreated dogs with presence (n=28) or absence (n=23) of right-sided CHF. Medical records of physical examinations, thoracic radiography and echocardiography were reviewed. The plasma concentration of canine ANP was measured with a chemiluminescent enzyme immunoassay. Plasma NT-proBNP concentrations were determined using an enzyme immunoassay. Plasma ANP and NT-proBNP concentrations in dogs with right-sided CHF were significantly higher than in healthy controls and those without right-sided CHF. The plasma NT-proBNP concentration >3,003 pmol/l used to identify right-sided CHF had a sensitivity of 88.5% and specificity of 90.3%. An area under the ROC curve (AUC) was 0.93. The AUC for NT-proBNP was significantly higher than the AUCs for the cardiothoracic ratio, vertebral heart score, ratio of right ventricular end-diastolic internal diameter to body surface area, tricuspid late diastolic flow and ratio of the velocities of tricuspid early to late diastolic flow. These results suggest that plasma ANP and NT-proBNP concentrations increase markedly in dogs with right-sided CHF. Particularly, NT-proBNP is simple and helpful biomarkers to assess the right-sided CHF. PMID:26607133

Dawn HAMO Image 23

NASA Image and Video Library

2015-09-24

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 27, 2015.

Dawn HAMO Image 20

NASA Image and Video Library

2015-09-21

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 26, 2015.

Dawn LAMO Image 106

NASA Image and Video Library

2016-06-09

This image from NASA Dawn spacecraft shows a portion of Ceres known as Erntedank Planum, a broad plateau 345 miles 555 kilometers wide. The terrain seen here lies just to the southeast of Occator Crater, home of Ceres brightest region.

Dawn HAMO Image 82

NASA Image and Video Library

2015-12-22

Part of the southern hemisphere on dwarf planet Ceres is seen in this image taken by NASA Dawn spacecraft. Hamori crater, named after a Japanese god and protector of tree leaves, is the large crater near the center of the image.

Color Map of Ceres Elliptical Projection

NASA Image and Video Library

2016-03-22

This global map elliptical map from NASA Dawn spacecraft shows the surface of Ceres in enhanced color, encompassing infrared wavelengths beyond human visual range. Some areas near the poles are black where Dawn color imaging coverage is incomplete.

Dawn LAMO Image 89

NASA Image and Video Library

2016-05-16

This image captured by NASA Dawn spacecraft features the shadowy rim of an unnamed crater on Ceres. The crater on the left appears relatively old, as its flanks are rugged and the crater density inside it is more or less uniform.

KSC-07pd1389

NASA Image and Video Library

2007-06-07

KENNEDY SPACE CENTER, FLA. -- At Astrotech's Hazardous Processing Facility, technicians look at the connections for loading the Dawn spacecraft with xenon gas for the ion propulsion system. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jim Grossmann

KSC-07pd1390

NASA Image and Video Library

2007-06-07

KENNEDY SPACE CENTER, FLA. -- At Astrotech's Hazardous Processing Facility, a technician checks the connections for loading the Dawn spacecraft with xenon gas for the ion propulsion system. Dawn's mission is to explore two of the asteroid belt's most intriguing and dissimilar occupants: asteroid Vesta and the dwarf planet Ceres. The Dawn spacecraft uses ion propulsion to get the additional velocity needed to reach Vesta once it leaves the Delta rocket. It also uses ion propulsion to spiral to lower altitudes on Vesta, to leave Vesta and cruise to Ceres and to spiral to a low-altitude orbit at Ceres. Ion propulsion makes efficient use of the onboard fuel by accelerating it to a velocity 10 times that of chemical rockets. Dawn is scheduled to launch July 7aboard a Delta II rocket from Launch Complex 17-B at Cape Canaveral Air Force Station. Photo credit: NASA/Jim Grossmann

High-resolution Ceres Low Altitude Mapping Orbit Atlas derived from Dawn Framing Camera images

NASA Astrophysics Data System (ADS)

Roatsch, Th.; Kersten, E.; Matz, K.-D.; Preusker, F.; Scholten, F.; Jaumann, R.; Raymond, C. A.; Russell, C. T.

2017-06-01

The Dawn spacecraft Framing Camera (FC) acquired over 31,300 clear filter images of Ceres with a resolution of about 35 m/pxl during the eleven cycles in the Low Altitude Mapping Orbit (LAMO) phase between December 16 2015 and August 8 2016. We ortho-rectified the images from the first four cycles and produced a global, high-resolution, uncontrolled photomosaic of Ceres. This global mosaic is the basis for a high-resolution Ceres atlas that consists of 62 tiles mapped at a scale of 1:250,000. The nomenclature used in this atlas was proposed by the Dawn team and was approved by the International Astronomical Union (IAU). The full atlas is available to the public through the Dawn Geographical Information System (GIS) web page [http://dawngis.dlr.de/atlas] and will become available through the NASA Planetary Data System (PDS) (http://pdssbn.astro.umd.edu/).

Some Effects of Procedural Variations on Choice Responding in Concurrent Chains

ERIC Educational Resources Information Center

Moore, J.

2009-01-01

The present research used pigeons in a three-key operant chamber and varied procedural features pertaining to both initial and terminal links of concurrent chains. The initial links randomly alternated on the side keys during a session, while the terminal links always appeared on the center key. Both equal and unequal initial-link schedules were…

Leaf Starch Turnover Occurs in Long Days and in Falling Light at the End of the Day.

PubMed

Fernandez, Olivier; Ishihara, Hirofumi; George, Gavin M; Mengin, Virginie; Flis, Anna; Sumner, Dean; Arrivault, Stéphanie; Feil, Regina; Lunn, John E; Zeeman, Samuel C; Smith, Alison M; Stitt, Mark

2017-08-01

We investigated whether starch degradation occurs at the same time as starch synthesis in Arabidopsis ( Arabidopsis thaliana ) leaves in the light. Starch accumulated in a linear fashion for about 12 h after dawn, then accumulation slowed and content plateaued. Following decreases in light intensity, the rate of accumulation of starch declined in proportion to the decline in photosynthesis if the decrease occurred <10 h after dawn, but accumulation ceased or loss of starch occurred if the same decrease in light intensity was imposed more than 10 h after dawn. These changes in starch accumulation patterns after prolonged periods in the light occurred at both high and low starch contents and were not related to time-dependent changes in either the rate of photosynthesis or the partitioning of assimilate between starch and Suc, as assessed from metabolite measurements and 14 CO 2 pulse experiments. Instead, measurements of incorporation of 13 C from 13 CO 2 into starch and of levels of the starch degradation product maltose showed that substantial starch degradation occurred simultaneously with synthesis at time points >14 h after dawn and in response to decreases in light intensity that occurred >10 h after dawn. Starch measurements in circadian clock mutants suggested that the clock influences the timing of onset of degradation. We conclude that the propensity for leaf starch to be degraded increases with time after dawn. The importance of this phenomenon for efficient use of carbon for growth in long days and for prevention of starvation during twilight is discussed. © 2017 American Society of Plant Biologists. All Rights Reserved.

The Enabling Use of Ion Propulsion on Dawn

NASA Astrophysics Data System (ADS)

Rayman, M.; Russell, C. T.; Raymond, C. A.; Mase, R. M.

2011-12-01

Dawn's mission to orbit both Vesta and Ceres is enabled by its use of ion propulsion. Even orbiting Vesta alone with conventional propulsion would have been unaffordable within the constraints of the Discovery Program, and orbiting both would have been impossible. In fact, no other spacecraft has been targeted to orbit two solar system destinations, which is only one of the many firsts that Dawn will achieve. The successful testing of ion propulsion on Deep Space 1 paved the way for Dawn not only to use the hardware with confidence but also to learn how to design the flight system and design the mission to take advantage of its capabilities. In addition to allowing Dawn to reach these two important targets, ion propulsion allows the spacecraft to accomplish significant changes in its orbit. Therefore, science observations of Vesta are planned from four different orbits, at varying altitudes and solar geometry. The use of ion propulsion results in a significant mission design effort since the trajectory is constantly being refined. This also creates a flexible mission architecture, which allows for optimization of the mission as conditions change. Solar electric ion propulsion is especially well suited to missions to the Main Asteroid Belt since solar energy is still a viable power source, whereas the size of the solar array needed beyond 3.5 AU is a potential limitation. Dawn has already surpassed the record for greatest propulsive velocity, but its greatest achievements will no doubt be the incredible bounty of science data enabled by this innovative flight system.

Leaf Starch Turnover Occurs in Long Days and in Falling Light at the End of the Day1[OPEN

PubMed Central

Mengin, Virginie; Arrivault, Stéphanie

2017-01-01

We investigated whether starch degradation occurs at the same time as starch synthesis in Arabidopsis (Arabidopsis thaliana) leaves in the light. Starch accumulated in a linear fashion for about 12 h after dawn, then accumulation slowed and content plateaued. Following decreases in light intensity, the rate of accumulation of starch declined in proportion to the decline in photosynthesis if the decrease occurred <10 h after dawn, but accumulation ceased or loss of starch occurred if the same decrease in light intensity was imposed more than 10 h after dawn. These changes in starch accumulation patterns after prolonged periods in the light occurred at both high and low starch contents and were not related to time-dependent changes in either the rate of photosynthesis or the partitioning of assimilate between starch and Suc, as assessed from metabolite measurements and 14CO2 pulse experiments. Instead, measurements of incorporation of 13C from 13CO2 into starch and of levels of the starch degradation product maltose showed that substantial starch degradation occurred simultaneously with synthesis at time points >14 h after dawn and in response to decreases in light intensity that occurred >10 h after dawn. Starch measurements in circadian clock mutants suggested that the clock influences the timing of onset of degradation. We conclude that the propensity for leaf starch to be degraded increases with time after dawn. The importance of this phenomenon for efficient use of carbon for growth in long days and for prevention of starvation during twilight is discussed. PMID:28663333

Dielectric properties of Asteroid Vesta's surface as constrained by Dawn VIR observations

NASA Astrophysics Data System (ADS)

Palmer, Elizabeth M.; Heggy, Essam; Capria, Maria T.; Tosi, Federico

2015-12-01

Earth and orbital-based radar observations of asteroids provide a unique opportunity to characterize surface roughness and the dielectric properties of their surfaces, as well as potentially explore some of their shallow subsurface physical properties. If the dielectric and topographic properties of asteroid's surfaces are defined, one can constrain their surface textural characteristics as well as potential subsurface volatile enrichment using the observed radar backscatter. To achieve this objective, we establish the first dielectric model of asteroid Vesta for the case of a dry, volatile-poor regolith-employing an analogy to the dielectric properties of lunar soil, and adjusted for the surface densities and temperatures deduced from Dawn's Visible and InfraRed mapping spectrometer (VIR). Our model suggests that the real part of the dielectric constant at the surface of Vesta is relatively constant, ranging from 2.3 to 2.5 from the night- to day-side of Vesta, while the loss tangent shows slight variation as a function of diurnal temperature, ranging from 6 × 10-3 to 8 × 10-3. We estimate the surface porosity to be ∼55% in the upper meter of the regolith, as derived from VIR observations. This is ∼12% higher than previous estimation of porosity derived from previous Earth-based X- and S-band radar observation. We suggest that the radar backscattering properties of asteroid Vesta will be mainly driven by the changes in surface roughness rather than potential dielectric variations in the upper regolith in the X- and S-band.

Introducing CoDa (Cosmic Dawn): Radiation-Hydrodynamics of Galaxy Formation in the Early Universe

NASA Astrophysics Data System (ADS)

Ocvirk, Pierre; Gillet, Nicolas; Shapiro, Paul; Aubert, Dominique; Iliev, Ilian; Romain, Teyssier; Yepes, Gustavo; Choi, Jun-hwan; Sullivan, David; Knebe, Alexander; Gottloeber, Stefan; D'Aloisio, Anson; Park, Hyunbae; Hoffman, Yehuda

2015-08-01

CoDa (Cosmic Dawn) is the largest fully coupled radiation hydrodynamics simulation of the reionization of the local Universe to date. It was performed using RAMSES-CUDATON running on 8192 nodes (i.e. 8192 GPUs) on the titan supercomputer at Oak Ridge National Laboratory to simulate a 64 h-1Mpc side box down to z=4.23. In this simulation, reionization proceeds self-consistently, driven by stellar radiation. We compare the simulation's reionization history, ionizing flux density, the cosmic star formation history and the CMB Thompson scattering optical depth with their observational values. Luminosity functions are also in rather good agreement with high redshift observations, although very bright objects (MAB1600 < -21) are overabundant in CoDa. We investigate the evolution of the intergalactic medium, and find that gas filaments present a sheathed structure, with a hot envelope surrounding a cooler core. They are however not able to self-shield, while regions denser than 10^-4.5 H atoms per comoving h^-3cm^3 are. Haloes below M ˜ 3.10^9 M⊙ are severely affected by the expanding, rising UV background: their ISM is quickly photo-heated to temperatures above our star formation threshold and therefore stop forming stars after local reionization has occured. Overall, the haloes between 10^(10-11) M⊙ dominate the star formation budget of the box for most of the Epoch of Reionization. Several additional studies will follow, looking for instance at environmental effects on galaxy properties, and the regimes of accretion.

Comparing Vesta Topography

NASA Image and Video Library

2013-09-27

These two images compare topographic maps of the giant asteroid Vesta as discerned by NASA Hubble Space Telescope top and as seen by NASA Dawn spacecraft bottom. Hubble has been in an orbit around Earth, while Dawn orbited Vesta from 2011 to 2012.

Dawn HAMO Image 34

NASA Image and Video Library

2015-10-09

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on September 15, 2015, and has a resolution of 450 feet 140 meters per pixel.

Dawn HAMO Image 27

NASA Image and Video Library

2015-09-30

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on August 22, 2015, and has a resolution of 450 feet 140 meters per pixel.

Dawn View from OpNav9

NASA Image and Video Library

2015-05-28

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 23, 2015, from a distance of 3,169 miles 5,100 kilometers. Resolution in the image is about 1,565 feet 477 meters per pixel.

Level-2 Milestone 3504: Scalable Applications Preparations and Outreach for the Sequoia ID (Dawn)

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

Futral, W. Scott; Gyllenhaal, John C.; Hedges, Richard M.

2010-07-02

This report documents LLNL SAP project activities in anticipation of the ASC Sequoia system, ASC L2 milestone 3504: Scalable Applications Preparations and Outreach for the Sequoia ID (Dawn), due June 30, 2010.

Dawn Mission to Vesta and Ceres Lithograph

NASA Image and Video Library

2007-01-01

This artist's lithograph features general information, significant dates, and interesting facts on the backabout asteroid Vesta and dwarf planet Ceres and is part of the Mission Art series from NASA's Dawn mission. http://photojournal.jpl.nasa.gov/catalog/PIA19370

[Continuous subcutaneous morphine to patients with terminal cancer. Analgesia at home].

PubMed

Laursen, J O

1994-04-04

Since 1992 it has been possible for cancer patients in the county of Southern Jutland to receive terminal care in their own homes. An essential part of this management is effective pain relief; more than 60% of cancer patients have chronic pain. In cases where oral medication or epidural administration of morphine is insufficient or complicated by side-effects continuous subcutaneous morphine administration may be suitable. The patient may be treated in this latter manner for long periods of time. A case story is described where a cancer patient was treated with continuous subcutaneous morphine in his home for more than 257 days without complications or major side-effects.

Plasma observations during the Mars atmospheric “plume” event of March–April 2012

PubMed Central

Andrews, D. J.; Barabash, S.; Edberg, N. J. T.; Gurnett, D. A.; Hall, B. E. S.; Holmström, M.; Lester, M.; Morgan, D. D.; Opgenoorth, H. J.; Ramstad, R.; Sanchez-Cano, B.; Way, M.; Witasse, O.

2018-01-01

We present initial analysis and conclusions from plasma observations made during the reported “Mars plume event” of March - April 2012. During this period, multiple independent amateur observers detected a localized, high-altitude “plume” over the Martian dawn terminator [Sanchez-Lavega et al., Nature, 2015, doi:10.1038/nature14162], the cause of which remains to be explained. The estimated brightness of the plume exceeds that expected for auroral emissions, and its projected altitude greatly exceeds that at which clouds are expected to form. We report on in-situ measurements of ionospheric plasma density and solar wind parameters throughout this interval made by Mars Express, obtained over the same surface region, but at the opposing terminator. Measurements in the ionosphere at the corresponding location frequently show a disturbed structure, though this is not atypical for such regions with intense crustal magnetic fields. We tentatively conclude that the formation and/or transport of this plume to the altitudes where it was observed could be due in part to the result of a large interplanetary coronal mass ejection (ICME) encountering the Martian system. Interestingly, we note that the only similar plume detection in May 1997 may also have been associated with a large ICME impact at Mars. PMID:29552437

Plasma observations during the Mars atmospheric "plume" event of March-April 2012.

PubMed

Andrews, D J; Barabash, S; Edberg, N J T; Gurnett, D A; Hall, B E S; Holmström, M; Lester, M; Morgan, D D; Opgenoorth, H J; Ramstad, R; Sanchez-Cano, B; Way, M; Witasse, O

2016-04-01

We present initial analysis and conclusions from plasma observations made during the reported "Mars plume event" of March - April 2012. During this period, multiple independent amateur observers detected a localized, high-altitude "plume" over the Martian dawn terminator [Sanchez-Lavega et al., Nature, 2015, doi:10.1038/nature14162], the cause of which remains to be explained. The estimated brightness of the plume exceeds that expected for auroral emissions, and its projected altitude greatly exceeds that at which clouds are expected to form. We report on in-situ measurements of ionospheric plasma density and solar wind parameters throughout this interval made by Mars Express, obtained over the same surface region, but at the opposing terminator. Measurements in the ionosphere at the corresponding location frequently show a disturbed structure, though this is not atypical for such regions with intense crustal magnetic fields. We tentatively conclude that the formation and/or transport of this plume to the altitudes where it was observed could be due in part to the result of a large interplanetary coronal mass ejection (ICME) encountering the Martian system. Interestingly, we note that the only similar plume detection in May 1997 may also have been associated with a large ICME impact at Mars.

Dawn HAMO Image 42

NASA Image and Video Library

2015-10-21

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres at mid-latitudes, from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 21, 2015, and has a resolution of 450 feet 140 meters per pixel.

Dawn Survey Orbit Image 40

NASA Image and Video Library

2015-08-04

This image, taken by NASA Dawn spacecraft on June 24, 2015, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers with a resolution of 1,400 feet 410 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19613

Dawn LAMO Image 38

NASA Image and Video Library

2016-03-02

NASA Dawn spacecraft obtained this view of Azacca Crater on Ceres. The rim of this crater has terraces descending from its rim down to its floor. The crater floor is relatively free of large impact scars and is named for the Haitian god of agriculture

A Last Look Back at Vesta

NASA Image and Video Library

2012-09-05

This image is from the last sequence of images NASA Dawn spacecraft obtained of the giant asteroid Vesta, looking down at Vesta north pole as it was departing. Dawn escaped from Vesta orbit on Sept. 4, 2012 PDT Sept. 5, 2012 CET.

Dawn LAMO Image 90

NASA Image and Video Library

2016-05-17

This image from NASA Dawn spacecraft shows the western rim of Azacca Crater on Ceres. A smaller impact feature sits on its flank. Of particular interest in this scene is the great number of small, bright spots, in the southern part of the image.

Parallel computing of a climate model on the dawn 1000 by domain decomposition method

NASA Astrophysics Data System (ADS)

Bi, Xunqiang

1997-12-01

In this paper the parallel computing of a grid-point nine-level atmospheric general circulation model on the Dawn 1000 is introduced. The model was developed by the Institute of Atmospheric Physics (IAP), Chinese Academy of Sciences (CAS). The Dawn 1000 is a MIMD massive parallel computer made by National Research Center for Intelligent Computer (NCIC), CAS. A two-dimensional domain decomposition method is adopted to perform the parallel computing. The potential ways to increase the speed-up ratio and exploit more resources of future massively parallel supercomputation are also discussed.

Dawn XMO2 Image 3

NASA Image and Video Library

2016-11-09

Relatively young craters, with sharp crater rims and streaks of bright material, are the focus of this view of Ceres from NASA's Dawn spacecraft. The large, ancient and quite degraded crater Fluusa is seen at top center. The younger craters are Kupalo, at lower right, and Juling, to its left. Dawn took this image on Oct. 17, 2016, from its second extended-mission science orbit (XMO2), at a distance of about 920 miles (1,480 kilometers) above the surface. The image resolution is about 460 feet (140 meters) per pxel. http://photojournal.jpl.nasa.gov/catalog/PIA21223

Dawn Orbit Determination Team: Trajectory Modeling and Reconstruction Processes at Vesta

NASA Technical Reports Server (NTRS)

Abrahamson, Matthew J.; Ardito, Alessandro; Han, Dongsuk; Haw, Robert; Kennedy, Brian; Mastrodemos, Nick; Nandi, Sumita; Park, Ryan; Rush, Brian; Vaughan, Andrew

2013-01-01

The Dawn spacecraft spent over a year in orbit around Vesta from July 2011 through August 2012. In order to maintain the designated science reference orbits and enable the transfers between those orbits, precise and timely orbit determination was required. Challenges included low-thrust ion propulsion modeling, estimation of relatively unknown Vesta gravity and rotation models, track-ing data limitations, incorporation of real-time telemetry into dynamics model updates, and rapid maneuver design cycles during transfers. This paper discusses the dynamics models, filter configuration, and data processing implemented to deliver a rapid orbit determination capability to the Dawn project.

Capillary zone electrophoresis determination of aniline and pyridine in sewage samples using transient isotachophoresis with a system-induced terminator.

PubMed

Hattori, Takanari; Okamura, Hideo; Asaoka, Satoshi; Fukushi, Keiichi

2017-08-18

Transient isotachophoresis (tITP) with a system-induced terminator (SIT) was developed for capillary zone electrophoresis (CZE) determination of aniline (An + ) and pyridine (Py + ) in sewage samples. After sample injection, a water vial was set at the sample-inlet side. Then voltage was applied to generate a system-induced terminator (H + ). Experiments and simulations revealed a concentration effect by tITP with an SIT: background electrolyte (BGE) - 100mM acetic acid (AcOH) and 50mM NaOH (pH 4.6); detection wavelength - 200nm for An + and 254nm for Py + ; vacuum injection period - 15s (190nL); SIT generation - 10kV applied for 80s with the sample inlet side anode; separation voltage - 20kV with the sample inlet side anode. The limits of detection (LODs, S/N=3) of An + and Py + respectively reached 10 and 42μg/L, with good repeatability (peak area RSDs≤6.9%) and calibration graph linearity (R 2 =0.9997). The proposed method was applied for determination of An + and Py + in sewage samples. Recoveries of An + (0.50mg/L) and Py + (2.0mg/L) in spiked sewage samples were 94-104%. Copyright © 2017 Elsevier B.V. All rights reserved.

Novel synthesis of cyclic amide-linked analogues of angiotensins II and III.

PubMed

Matsoukas, J M; Hondrelis, J; Agelis, G; Barlos, K; Gatos, D; Ganter, R; Moore, D; Moore, G J

1994-09-02

Cyclic amide-linked angiotension II (ANGII) analogues have been synthesized by novel strategies, in an attempt to test the ring clustering and the charge relay bioactive conformation recently suggested. These analogues were synthesized by connecting side chain amino and carboxyl groups at positions 1 and 8, 2 and 8, 3 and 8, and 3 and 5, N-terminal amino and C-terminal carboxyl groups at positions 1 and 8, 2 and 8, and 4 and 8, and side chain amino to C-terminal carboxyl group at positions 1 and 8. All these analogues were biologically inactive, except for cyclic [Sar1, Asp3, Lys5]ANGII (analogue 10) which had high contractile activity in the rat uterus assay (30% of ANGII) and [Lys1, Tyr(Me)4, Glu8]ANGII (analogue 7) which had weak antagonist activity (PA2 approximately 6). Precyclic linear peptides synthesized using 2-chlorotrityl chloride resin and N alpha-Fmoc-amino acids with suitable side chain protection were obtained in high yield and purity and were readily cyclized with benzotriazol-1-yloxytris(dimethylamino)-phosphonium hexafluorophosphate as coupling reagent. Molecular modeling suggests that the ring structure of the potent analogue can be accommodated in the charge relay conformation proposed for ANGII.

Organization of projections from the spinal trigeminal subnucleus oralis to the spinal cord in the rat: a neuroanatomical substrate for reciprocal orofacial-cervical interactions.

PubMed

Devoize, Laurent; Doméjean, Sophie; Melin, Céline; Raboisson, Patrick; Artola, Alain; Dallel, Radhouane

2010-07-09

The organization of efferent projections from the spinal trigeminal nucleus oralis (Sp5O) to the spinal cord in the rat was studied using the anterograde tracer Phaseolus vulgaris leucoagglutinin. Sp5O projections to the spinal cord are restricted to the cervical cord. No labeled terminal can be detected in the thoracic and lumbar cord. The organization of these projections happens to critically depend on the dorso-ventral location of the injection site. On the one hand, the dorsal part of the Sp5O projects to the medial part of the dorsal horn (laminae III-V) at the C1 level, on the ipsilateral side, and to the ventral horn, on both sides but mainly on the ipsilateral one. Ipsilateral labeled terminals are distributed throughout laminae VII to IX but tend to cluster around the dorso-medial motor nuclei, especially at C3-C5 levels. Within the contralateral ventral horn, label terminals are found particularly in the region of the ventro-medial motor nucleus. This projection extends as far caudally as C3 or C4 level. On the other hand, the ventral part of the Sp5O projects to the lateral part of the dorsal horn (laminae III-V) at the C1 level, on the ipsilateral side, and to the ventral horn, on both sides but mainly on the contralateral one. Contralateral labeled terminals are distributed within the region of the dorso- and ventro-medial motor nuclei at C1-C4 levels whereas they are restricted to the dorso-medial motor nucleus at C5-C8 levels. These findings suggest that Sp5O is involved in the coordination of neck movements and in the modulation of incoming sensory information at the cervical spinal cord. Copyright (c) 2010 Elsevier B.V. All rights reserved.

Dawn HAMO Image 40

NASA Image and Video Library

2015-10-19

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 20, 2015, and has a resolution of 450 feet 140 meters per pixel.

Dawn HAMO Image 41

NASA Image and Video Library

2015-10-20

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 21, 2015, and has a resolution of 450 feet 140 meters per pixel.

Earth Observations taken by the Expedition 27 Crew

NASA Image and Video Library

2011-04-12

ISS027-E-012224 (12 April 2011) --- Sunset over western South America is featured in this image photographed by an Expedition 27 crew member on the International Space Station. Crew members onboard the space station see, on average, sixteen sunrises and sunsets during a 24-hour orbital period. Each changeover between day and night on the ground is marked by the terminator, or line separating the sunlit side of Earth from the side in darkness. While the terminator is conceptualized as a hard boundary?and is frequently presented as such in graphics and visualizations?in reality the boundary between light and dark is diffuse due to scattering of light by Earth?s atmosphere. This zone of diffuse lighting is experienced as dusk or twilight on the ground ? while the sun is no longer visible, some illumination is still present due to light scattering over the local horizon. The terminator is visible in this photograph trending across the image from lower left to upper right. This panoramic view across central South America, looking towards the northeast, was acquired at approximately 7:37 p.m. local time. Layers of Earth?s atmosphere, colored bright white to deep blue, are visible extending across the horizon (or limb). The highest cloud tops have a reddish glow from the direct light of the setting sun while lower clouds are in twilight. The Salar de Coipasa, a large salt lake in Bolivia, is dimly visible on the night side of the terminator. The salar provides a geographic reference point that allows the location and viewing orientation of the image to be determined.

20. View from northeast to southwest side of scanner building ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

20. View from northeast to southwest side of scanner building 104 showing two waveguide termination faces (fiberglass light bands on left of photograph). - Clear Air Force Station, Ballistic Missile Early Warning System Site II, One mile west of mile marker 293.5 on Parks Highway, 5 miles southwest of Anderson, Anderson, Denali Borough, AK

Comparing Vesta's Surface Roughness to the Moon Using Bistatic Radar Observations by the Dawn Mission

NASA Astrophysics Data System (ADS)

Palmer, E. M.; Heggy, E.; Kofman, W. W.; Moghaddam, M.

2015-12-01

The first orbital bistatic radar (BSR) observations of a small body have been conducted opportunistically by NASA's Dawn spacecraft at Asteroid Vesta using the telecommunications antenna aboard Dawn to transmit and the Deep Space Network 70-meter antennas on Earth to receive. Dawn's high-gain communications antenna continuously transmitted right-hand circularly polarized radio waves (4-cm wavelength), and due to the opportunistic nature of the experiment, remained in a fixed orientation pointed toward Earth throughout each BSR observation. As a consequence, Dawn's transmitted radio waves scattered from Vesta's surface just before and after each occultation of the Dawn spacecraft behind Vesta, resulting in surface echoes at highly oblique incidence angles of greater than 85 degrees, and a small Doppler shift of ~2 Hz between the carrier signal and surface echoes from Vesta. We analyze the power and Doppler spreading of Vesta's surface echoes to assess surface roughness, and find that Vesta's area-normalized radar cross section ranges from -8 to -17 dB, which is notably much stronger than backscatter radar cross section values reported for the Moon's limbs (-20 to -35 dB). However, our measurements correspond to the forward scattering regime--such that at high incidence, radar waves are expected to scatter more weakly from a rough surface in the backscatter direction than that which is scattered forward. Using scattering models of rough surfaces observed at high incidence, we report on the relative roughness of Vesta's surface as compared to the Moon and icy Galilean satellites. Through this, we assess the dominant processes that have influenced Vesta's surface roughness at centimeter and decimeter scales, which are in turn applicable to assisting future landing, sampling and orbital missions of other small bodies.

Ceres Evolution: From Thermodynamic Modeling and Now Dawn Observation

NASA Astrophysics Data System (ADS)

McCord, T. B.; Combe, J. P.; Castillo, J. C.; Raymond, C. A.; De Sanctis, M. C.; Jaumann, R.; Ammannito, E.; Russell, C. T.

2015-12-01

Thermodynamic modeling indicated that Ceres has experienced planetary processes, including extensive melting of its ~25% water and differentiation, (McCord and Sotin, JGR, 2005; Castillo and McCord, Icarus, 2009). Early telescopic studies showed Ceres' surface to be spectrally similar to carboneous-chondrite-like material, i.e., aqueously altered silicates darkened by carbon, with a water-OH-related absorption near 3.06 µm. Later observations improved the spectra and suggested more specific interpretations: Structural water in clay minerals, phyllosilicates, perhaps ammoniated, iron-rich clays, carbonates, brucite, all implying extensive aqueous alteration, perhaps in the presence of CO2. Telescopic observations and thermodynamic models predicted Dawn would find a very different body compared to Vesta (e.g. McCord et al., SSR, 2011), as current Dawn observations are confirming. Ceres' original water ice should have melted early in its evolution, with the resulting differentiation and mineralization strongly affecting Ceres' composition, size and shape over time. The ocean should have become very salty and perhaps may still be liquid in places. The surface composition from telescopes seems to reflect this complex history. The mineralization with repeated mixing of the crust with the early liquid interior and with in-fall from space would create a complex surface that will present an interpretation challenge for Dawn. The Dawn spacecraft is currently collecting observations of Ceres' landforms, elemental and mineralogical/molecular composition and gravity field from orbit. Early results suggest a heavily cratered but distorted and lumpy body with features and composition consistent with internal activity, perhaps recent or current, associated with water and perhaps other volatiles. We will present and interpret the latest Dawn Ceres findings and how they affect our earlier understanding of Ceres evolution from modeling and telescope observations.

[Continuous subcutaneous morphine--treatment of pain in patients with terminal cancer].

PubMed

Nielsen, F B; Clemensen, S E; Olesen, A S; Hole, P

1990-06-11

Nine patients with terminal cancer were treated for pain with continuous subcutaneous injection of morphine via a portable battery-driven injection pump. Treatment was instituted on account of failure of other forms of treatment with oral or epidural morphine derivatives or on account of severe nausea and vomiting which necessitated parenteral administration. Treatment proved reasonably effective and no side effects of significance occurred. Two of the patients could be treated in their homes. The method is thus considered as suitable for treatment of pain in patients with terminal cancer.

Dawn Survey Orbit Image 32

NASA Image and Video Library

2015-07-22

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19601

Dawn Survey Orbit Image 23

NASA Image and Video Library

2015-07-09

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 22, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19591

Dawn HAMO Image 16

NASA Image and Video Library

2015-09-15

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19894

Dawn Survey Orbit Image 5

NASA Image and Video Library

2015-06-16

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 6, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19573

Dawn HAMO Image 19

NASA Image and Video Library

2015-09-18

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 26, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19897

Dawn Survey Orbit Image 31

NASA Image and Video Library

2015-07-21

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19600

Dawn OpNav9 Image 5

NASA Image and Video Library

2015-06-12

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 22, 2015, from a distance of 3,200 miles 5,100 kilometers with a resolution of 1,600 feet 480 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19567

Dawn Survey Orbit Image 26

NASA Image and Video Library

2015-07-14

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19594

Dawn Survey Orbit Image 15

NASA Image and Video Library

2015-06-26

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 10, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19583

Dawn Survey Orbit Image 4

NASA Image and Video Library

2015-06-15

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 6, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19572

Dawn OpNav9 Image 4

NASA Image and Video Library

2015-06-11

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 22, 2015, from a distance of 3,200 miles 5,100 kilometers with a resolution of 1,600 feet 480 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19566

Dawn OpNav9 Image 3

NASA Image and Video Library

2015-06-10

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 22, 2015, from a distance of 3,200 miles 5,100 kilometers with a resolution of 1,600 feet 480 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19565

Dawn HAMO Image 17

NASA Image and Video Library

2015-09-16

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19895

Dawn Survey Orbit Image 8

NASA Image and Video Library

2015-06-19

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 6, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19576

Dawn HAMO Image 15

NASA Image and Video Library

2015-09-14

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19893

Dawn OpNav9 Image 1

NASA Image and Video Library

2015-06-08

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 22, 2015, from a distance of 3,200 miles 5,100 kilometers with a resolution of 1,600 feet 480 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19563

Dawn HAMO Image 21

NASA Image and Video Library

2015-09-22

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 27, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19899

Dawn HAMO Image 14

NASA Image and Video Library

2015-09-11

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19892

Dawn Survey Orbit Image 22

NASA Image and Video Library

2015-07-08

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 18, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19590

Dawn HAMO Image 18

NASA Image and Video Library

2015-09-17

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 26, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19896

Dawn Survey Orbit Image 30

NASA Image and Video Library

2015-07-20

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19599

Dawn Survey Orbit Image 28

NASA Image and Video Library

2015-07-16

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19596

Dawn Survey Orbit Image 12

NASA Image and Video Library

2015-06-23

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 7, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19580

Dawn OpNav9 Image 2

NASA Image and Video Library

2015-06-09

This image of Ceres is part of a sequence taken by NASA Dawn spacecraft on May 22, 2015, from a distance of 3,200 miles 5,100 kilometers with a resolution of 1,600 feet 480 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19564

Dawn Survey Orbit Image 27

NASA Image and Video Library

2015-07-15

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19595

Dawn HAMO Image 22

NASA Image and Video Library

2015-09-23

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 27, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19900

Dawn Survey Orbit Image 7

NASA Image and Video Library

2015-06-18

This image, taken by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 9, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19575

Dawn First Glimpse of Vesta -- Processed

NASA Image and Video Library

2011-05-11

This image, processed to show the true size of the giant asteroid Vesta, shows Vesta in front of a spectacular background of stars. It was obtained by the framing camera aboard NASA Dawn spacecraft on May 3, 2011, from a distance of about 750,000 miles.

Singing in the moonlight: dawn song performance of a diurnal bird varies with lunar phase

PubMed Central

York, Jennifer E.; Young, Andrew J.; Radford, Andrew N.

2014-01-01

It is well established that the lunar cycle can affect the behaviour of nocturnal animals, but its potential to have a similar influence on diurnal species has received less research attention. Here, we demonstrate that the dawn song of a cooperative songbird, the white-browed sparrow weaver (Plocepasser mahali), varies with moon phase. When the moon was above the horizon at dawn, males began singing on average 10 min earlier, if there was a full moon compared with a new moon, resulting in a 67% mean increase in performance period and greater total song output. The lack of a difference between full and new moon dawns when the moon was below the horizon suggests that the observed effects were driven by light intensity, rather than driven by other factors associated with moon phase. Effects of the lunar cycle on twilight signalling behaviour have implications for both pure and applied animal communication research. PMID:24429683

The role of PDF neurons in setting the preferred temperature before dawn in Drosophila.

PubMed

Tang, Xin; Roessingh, Sanne; Hayley, Sean E; Chu, Michelle L; Tanaka, Nobuaki K; Wolfgang, Werner; Song, Seongho; Stanewsky, Ralf; Hamada, Fumika N

2017-05-02

Animals have sophisticated homeostatic controls. While mammalian body temperature fluctuates throughout the day, small ectotherms, such as Drosophila achieve a body temperature rhythm (BTR) through their preference of environmental temperature. Here, we demonstrate that pigment dispersing factor (PDF) neurons play an important role in setting preferred temperature before dawn. We show that small lateral ventral neurons (sLNvs), a subset of PDF neurons, activate the dorsal neurons 2 (DN2s), the main circadian clock cells that regulate temperature preference rhythm (TPR). The number of temporal contacts between sLNvs and DN2s peak before dawn. Our data suggest that the thermosensory anterior cells (ACs) likely contact sLNvs via serotonin signaling. Together, the ACs-sLNs-DN2s neural circuit regulates the proper setting of temperature preference before dawn. Given that sLNvs are important for sleep and that BTR and sleep have a close temporal relationship, our data highlight a possible neuronal interaction between body temperature and sleep regulation.

KSC-07pd1515

NASA Image and Video Library

2007-06-15

KENNEDY SPACE CENTER, FLA. -- On Launch Pad 17-B at Cape Canaveral Air Force Station, workers maneuver the second stage of the Delta II launch vehicle onto the first stage for mating. The Delta II-Heavy, manufactured by the United Launch Alliance, is scheduled to launch the Dawn spacecraft on its 4-year flight to the asteroid belt. The Delta II-Heavy is the strongest rocket in the Delta II class. It will use three stages and nine solid-fueled booster rockets to propel Dawn on its way. A 9.5-foot payload fairing will protect the spacecraft from the heat and stresses of launch. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Dawn is scheduled to launch July 7. Photo credit: NASA/Jack Pfaller

Dawn Auroral Breakup at Saturn Initiated by Auroral Arcs: UVIS/Cassini Beginning of Grand Finale Phase

NASA Astrophysics Data System (ADS)

Radioti, A.; Grodent, D.; Yao, Z. H.; Gérard, J.-C.; Badman, S. V.; Pryor, W.; Bonfond, B.

2017-12-01

We present Cassini auroral observations obtained on 11 November 2016 with the Ultraviolet Imaging Spectrograph at the beginning of the F-ring orbits and the Grand Finale phase of the mission. The spacecraft made a close approach to Saturn's southern pole and offered a remarkable view of the dayside and nightside aurora. With this sequence we identify, for the first time, the presence of dusk/midnight arcs, which are azimuthally spread from high to low latitudes, suggesting that their source region extends from the outer to middle/inner magnetosphere. The observed arcs could be auroral manifestations of plasma flows propagating toward the planet from the magnetotail, similar to terrestrial "auroral streamers." During the sequence the dawn auroral region brightens and expands poleward. We suggest that the dawn auroral breakup results from a combination of plasma instability and global-scale magnetic field reconfiguration, which is initiated by plasma flows propagating toward the planet. Alternatively, the dawn auroral enhancement could be triggered by tail magnetic reconnection.

Dawn Orbit Determination Team: Trajectory and Gravity Prediction Performance During Vesta Science Phases

NASA Technical Reports Server (NTRS)

Kennedy, Brian; Abrahamson, Matt; Ardito, Alessandro; Han, Dongsuk; Haw, Robert; Mastrodemos, Nicholas; Nandi, Sumita; Park, Ryan; Rush, Brian; Vaughan, Andrew

2013-01-01

The Dawn spacecraft was launched on September 27th, 2007. Its mission is to consecutively rendezvous with and observe the two largest bodies in the asteroid belt, Vesta and Ceres. It has already completed over a year's worth of direct observations of Vesta (spanning from early 2011 through late 2012) and is currently on a cruise trajectory to Ceres, where it will begin scientific observations in mid-2015. Achieving this data collection required careful planning and execution from all spacecraft teams. Dawn's Orbit Determination (OD) team was tasked with accurately predicting the trajectory of the Dawn spacecraft during the Vesta science phases, and also determining the parameters of Vesta to support future science orbit design. The future orbits included the upcoming science phase orbits as well as the transfer orbits between science phases. In all, five science phases were executed at Vesta, and this paper will describe some of the OD team contributions to the planning and execution of those phases.

C-terminal amino acid residue loss for deprotonated peptide ions containing glutamic acid, aspartic acid, or serine residues at the C-terminus.

PubMed

Li, Zhong; Yalcin, Talat; Cassady, Carolyn J

2006-07-01

Deprotonated peptides containing C-terminal glutamic acid, aspartic acid, or serine residues were studied by sustained off-resonance irradiation collision-induced dissociation (SORI-CID) in a Fourier transform ion cyclotron resonance (FT-ICR) mass spectrometer with ion production by electrospray ionization (ESI). Additional studies were performed by post source decay (PSD) in a matrix-assisted laser desorption ionization/time-of-flight (MALDI/TOF) mass spectrometer. This work included both model peptides synthesized in our laboratory and bioactive peptides with more complex sequences. During SORI-CID and PSD, [M - H]- and [M - 2H]2- underwent an unusual cleavage corresponding to the elimination of the C-terminal residue. Two mechanisms are proposed to occur. They involve nucleophilic attack on the carbonyl carbon of the adjacent residue by either the carboxylate group of the C-terminus or the side chain carboxylate group of C-terminal glutamic acid and aspartic acid residues. To confirm the proposed mechanisms, AAAAAD was labelled by 18O specifically on the side chain of the aspartic acid residue. For peptides that contain multiple C-terminal glutamic acid residues, each of these residues can be sequentially eliminated from the deprotonated ions; a driving force may be the formation of a very stable pyroglutamatic acid neutral. For peptides with multiple aspartic acid residues at the C-terminus, aspartic acid residue loss is not sequential. For peptides with multiple serine residues at the C-terminus, C-terminal residue loss is sequential; however, abundant loss of other neutral molecules also occurs. In addition, the presence of basic residues (arginine or lysine) in the sequence has no effect on C-terminal residue elimination in the negative ion mode.

KSC-07pd2062

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — Sitting on a transporter, the Dawn spacecraft arrives at the Astrotech payload processing facility. Dawn was returned from Launch Pad 17-B at Cape Canaveral Air Force Station to Astrotech to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/Charisse Nahser

KSC-07pd2063

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — The Dawn spacecraft is moved inside the Astrotech payload processing facility. Dawn was returned from Launch Pad 17-B at Cape Canaveral Air Force Station to Astrotech to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/Charisse Nahser

KSC-07pd1658

NASA Image and Video Library

2007-06-27

KENNEDY SPACE CENTER, FLA. -- At Launch Pad 17-B, at Cape Canaveral Air Force Station, workers prepare NASA's Dawn spacecraft mated to the Delta II upper stage booster, for hoisting up into the mobile service tower. Dawn will be mated with the Delta II launch vehicle. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA's first purely scientific mission powered by three solar electric ion propulsion engines. Photo credit: NASA/Troy Cryder.

Dawn XMO2 Image 28

NASA Image and Video Library

2017-01-03

Meanderi Crater on Ceres is seen at lower right in this image from NASA's Dawn spacecraft. Meanderi -- named for the Ngaing goddess (New Guinea) of taro, sugar cane and other foods -- hosts several medium-sized craters within its walls. Meanderi measures 64 miles (103 kilometers) in diameter. The crater is centered at 41 degrees south, 194 degrees east. Dawn took this image on Oct. 26, 2016, during its second extended-mission science orbit (XMO2), from a distance of about 920 miles (1,480 kilometers) above the surface of Ceres. The image resolution is about 460 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA21248

Electrically operated magnetic switch designed to display reduced leakage inductance

DOEpatents

Cook, Edward G.

1994-01-01

An electrically operated magnetic switch is disclosed herein for use in opening and closing a circuit between two terminals depending upon the voltage across these terminals. The switch so disclosed is comprised of a ferrite core in the shape of a toroid having opposing ends and opposite inner and outer sides and an arrangement of electrically conductive components defining at least one current flow path which makes a number of turns around the core. This arrangement of components includes a first plurality of electrically conducive rigid rods parallel with and located outside the outer side of the core and a second plurality of electrically conductive rigid rods parallel with and located inside the inner side of the core. The arrangement also includes means for electrically connecting these rods together so that the define the current flow path. In one embodiment, this latter means uses rigid cross-tab means. In another, preferred embodiment, printed circuits on rigid dielectric substrates located on opposite ends of the core are utilized to interconnect the rods together.

Growth and characterization of epitaxially stabilized ceria(001) nanostructures on Ru(0001)

DOE PAGES

Flege, Jan Ingo; Hocker, Jan; Kaemena, Bjorn; ...

2016-05-03

We have studied (001) surface terminated cerium oxide nanoparticles grown on a ruthenium substrate using physical vapor deposition. Their morphology, shape, crystal structure, and chemical state are determined by low-energy electron microscopy and micro-diffraction, scanning probe microscopy, and synchrotron-based X-ray absorption spectroscopy. Square islands are identified as CeO 2 nanocrystals exhibiting a (001) oriented top facet of varying size; they have a height of about 7 to 10 nm and a side length between about 50 and 500 nm, and are terminated with a p(2 × 2) surface reconstruction. Micro-illumination electron diffraction reveals the existence of a coincidence lattice atmore » the interface to the ruthenium substrate. The orientation of the side facets of the rod-like particles is identified as (111); the square particles are most likely of cuboidal shape, exhibiting (100) oriented side facets. Lastly, the square and needle-like islands are predominantly found at step bunches and may be grown exclusively at temperatures exceeding 1000 °C.« less

Dawn HAMO Image 32

NASA Image and Video Library

2015-10-07

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on September 9, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19910

Dawn HAMO Image 31

NASA Image and Video Library

2015-10-06

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on September 9, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19909

Dawn HAMO Image 33

NASA Image and Video Library

2015-10-08

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on September 14, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19971

Dawn HAMO Image 30

NASA Image and Video Library

2015-10-05

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on September 9, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19908

Dawn HAMO Image 36

NASA Image and Video Library

2015-10-13

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on September 20, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19978

Dawn HAMO Image 37

NASA Image and Video Library

2015-10-14

This image, taken by NASA Dawn spacecraft on Sept. 20, 2015, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19979

Dawn HAMO Image 35

NASA Image and Video Library

2015-10-12

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on August 23, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19972

Dawn HAMO Image 29

NASA Image and Video Library

2015-10-02

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on September 9, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19907

Dawn HAMO Image 9

NASA Image and Video Library

2015-09-03

This image, taken by NASA Dawn spacecraft, shows a portion of Ceres at mid-latitudes from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19885

Dawn HAMO Image 28

NASA Image and Video Library

2015-10-01

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on August 24, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19906

Dawn HAMO Image 25

NASA Image and Video Library

2015-09-28

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on August 21, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19903

Dawn HAMO Image 26

NASA Image and Video Library

2015-09-29

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on August 21, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19904

Dawn HAMO Image 24

NASA Image and Video Library

2015-09-25

This image, taken by NASA's Dawn spacecraft, shows the surface of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image was taken on August 21, 2015, and has a resolution of 450 feet (140 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19902

SARAS 2: a spectral radiometer for probing cosmic dawn and the epoch of reionization through detection of the global 21-cm signal

NASA Astrophysics Data System (ADS)

Singh, Saurabh; Subrahmanyan, Ravi; Shankar, N. Udaya; Rao, Mayuri Sathyanarayana; Girish, B. S.; Raghunathan, A.; Somashekar, R.; Srivani, K. S.

2018-04-01

The global 21-cm signal from Cosmic Dawn (CD) and the Epoch of Reionization (EoR), at redshifts z ˜ 6-30, probes the nature of first sources of radiation as well as physics of the Inter-Galactic Medium (IGM). Given that the signal is predicted to be extremely weak, of wide fractional bandwidth, and lies in a frequency range that is dominated by Galactic and Extragalactic foregrounds as well as Radio Frequency Interference, detection of the signal is a daunting task. Critical to the experiment is the manner in which the sky signal is represented through the instrument. It is of utmost importance to design a system whose spectral bandpass and additive spurious signals can be well calibrated and any calibration residual does not mimic the signal. Shaped Antenna measurement of the background RAdio Spectrum (SARAS) is an ongoing experiment that aims to detect the global 21-cm signal. Here we present the design philosophy of the SARAS 2 system and discuss its performance and limitations based on laboratory and field measurements. Laboratory tests with the antenna replaced with a variety of terminations, including a network model for the antenna impedance, show that the gain calibration and modeling of internal additive signals leave no residuals with Fourier amplitudes exceeding 2 mK, or residual Gaussians of 25 MHz width with amplitudes exceeding 2 mK. Thus, even accounting for reflection and radiation efficiency losses in the antenna, the SARAS 2 system is capable of detection of complex 21-cm profiles at the level predicted by currently favoured models for thermal baryon evolution.

Moon Search Algorithms for NASA's Dawn Mission to Asteroid Vesta

NASA Technical Reports Server (NTRS)

Memarsadeghi, Nargess; Mcfadden, Lucy A.; Skillman, David R.; McLean, Brian; Mutchler, Max; Carsenty, Uri; Palmer, Eric E.

2012-01-01

A moon or natural satellite is a celestial body that orbits a planetary body such as a planet, dwarf planet, or an asteroid. Scientists seek understanding the origin and evolution of our solar system by studying moons of these bodies. Additionally, searches for satellites of planetary bodies can be important to protect the safety of a spacecraft as it approaches or orbits a planetary body. If a satellite of a celestial body is found, the mass of that body can also be calculated once its orbit is determined. Ensuring the Dawn spacecraft's safety on its mission to the asteroid Vesta primarily motivated the work of Dawn's Satellite Working Group (SWG) in summer of 2011. Dawn mission scientists and engineers utilized various computational tools and techniques for Vesta's satellite search. The objectives of this paper are to 1) introduce the natural satellite search problem, 2) present the computational challenges, approaches, and tools used when addressing this problem, and 3) describe applications of various image processing and computational algorithms for performing satellite searches to the electronic imaging and computer science community. Furthermore, we hope that this communication would enable Dawn mission scientists to improve their satellite search algorithms and tools and be better prepared for performing the same investigation in 2015, when the spacecraft is scheduled to approach and orbit the dwarf planet Ceres.

Using Dawn to Observe SEP Events Past 2 AU

NASA Astrophysics Data System (ADS)

Villarreal, Michaela; Russell, Christopher T.; Prettyman, Thomas H.

2017-10-01

The launch of the STEREO spacecraft provided much insight into the longitudinal and radial distribution of solar energetic particles (SEPs) relative to their origin site. However, almost all of the observations of SEP events have been made exclusively near 1 AU. The Dawn mission, which orbited around Vesta before arriving at Ceres, provides an opportunity to analyze these events at much further distances. Although Dawn's Gamma Ray and Neutron Detector (GRaND) is not optimized for SEP characterization, it is sensitive to protons greater than 4 MeV, making it capable of detecting a solar energetic particle event in its vicinity. Solar energetic particles in this area of the solar system are important as they are believed to cause sputtering at bodies such as Ceres and comets (Villarreal et al., 2017; Wurz et al., 2015). In this study, we use Dawn’s GRaND data from 2011-2015 when Dawn was at distances between 2-3 AU. We compare the SEP events seen by Dawn with particle measurements at 1 AU using STEREO, Wind, and ACE to understand how the SEP events evolved past 1 AU.References: Villarreal, M. N., et al. (2017), The dependence of the Cerean exosphere on solar energetic particle events, Astrophys. J. Lett., 838, L8.Wurz, P. et al. (2015), Solar wind sputtering of dust on the surface of 67P/Churyumov-Gerasimenko, A&A, 583, A22.

4 Vesta in Color: High Resolution Mapping from Dawn Framing Camera Images

NASA Technical Reports Server (NTRS)

Reddy, V.; LeCorre, L.; Nathues, A.; Sierks, H.; Christensen, U.; Hoffmann, M.; Schroeder, S. E.; Vincent, J. B.; McSween, H. Y.; Denevi, B. W.;

Dawn-dusk asymmetries in rotating magnetospheres: Lessons from modeling Saturn

NASA Astrophysics Data System (ADS)

Jia, Xianzhe; Kivelson, Margaret G.

2016-02-01

Spacecraft measurements reveal perplexing dawn-dusk asymmetries of field and plasma properties in the magnetospheres of Saturn and Jupiter. Here we describe a previously unrecognized source of dawn-dusk asymmetry in a rapidly rotating magnetosphere. We analyze two magnetohydrodynamic simulations, focusing on how flows along and across the field vary with local time in Saturn's dayside magnetosphere. As plasma rotates from dawn to noon on a dipolarizing flux tube, it flows away from the equator along the flux tube at roughly half of the sound speed (Cs), the maximum speed at which a bulk plasma can flow along a flux tube into a lower pressure region. As plasma rotates from noon to dusk on a stretching flux tube, the field-aligned component of its centripetal acceleration decreases and it flows back toward the equator at speeds typically smaller than 1/2 Cs. Correspondingly, the plasma sheet remains far thicker and the field less stretched in the afternoon than in the morning. Different radial force balance in the morning and afternoon sectors produce asymmetry in the plasma sheet thickness and a net dusk-to-dawn flow inside of L = 15 or equivalently, a large-scale electric field (E) oriented from postnoon to premidnight, as reported from observations. Morning-afternoon asymmetry analogous to that found at Saturn has been observed at Jupiter, and a noon-midnight component of E cannot be ruled out.

Reevaluating Surface Composition of Asteroid (4) Vesta by Comparing HED Spectral Data with Dawn Framing Camera (FC) Observations

NASA Astrophysics Data System (ADS)

Giebner, T.; Jaumann, R.; Schröder, S.

2016-08-01

This master's thesis project tries to reevaluate previous findings on asteroid (4) Vesta's surface composition by using DAWN FC Filter image ratios in a new way in order to identify HED (howardite, eucrite, diogenite) lithologies on the surface.

Dawn HAMO Image 44

NASA Image and Video Library

2015-10-23

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 21, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19986

Dawn HAMO Image 10

NASA Image and Video Library

2015-09-04

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19886

Dawn Survey Orbit Image 53

NASA Image and Video Library

2015-08-24

This image, taken by NASA's Dawn spacecraft, shows the bright spots of Occator crater on Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19630

Dawn HAMO Image 52

NASA Image and Video Library

2015-11-04

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres at mid-latitudes from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 29, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19994

Dawn HAMO Image 8

NASA Image and Video Library

2015-09-02

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19884

Dawn HAMO Image 12

NASA Image and Video Library

2015-09-10

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19888

Dawn HAMO Image 48

NASA Image and Video Library

2015-10-29

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 22, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19990

Dawn Survey Orbit Image 34

NASA Image and Video Library

2015-07-24

This image, taken on June 25, 2015 by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers, with a resolution of 1,400 feet 410 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19603

Dawn HAMO Image 6

NASA Image and Video Library

2015-08-31

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19882

Dawn HAMO Image 7

NASA Image and Video Library

2015-09-01

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19883

Dawn HAMO Image 45

NASA Image and Video Library

2015-10-26

This image, taken by NASA Dawn spacecraft, shows the surface of dwarf planet Ceres at mid-latitudes from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 21, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19987

Dawn HAMO Image 5

NASA Image and Video Library

2015-08-28

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19881

Dawn HAMO Image 4

NASA Image and Video Library

2015-08-27

This image, taken by NASA's Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles (1,470 kilometers). The image, with a resolution of 450 feet (140 meters) per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19635

Dawn HAMO Image 43

NASA Image and Video Library

2015-10-22

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 21, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19985

Dawn Survey Orbit Image 35

NASA Image and Video Library

2015-07-27

This image, taken by NASA Dawn spacecraft, shows the brightest spots on dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers. The image, with a resolution of 1,400 feet 410 meters per pixel, was taken on June 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19604

Dawn HAMO Image 38

NASA Image and Video Library

2015-10-15

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 20, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19980

Dawn Survey Orbit Image 13

NASA Image and Video Library

2015-06-24

The north pole of Ceres can be seen in this image taken on June 9, 2015 by NASA Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers with a resolution of 1,400 feet 410 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19581

Dawn HAMO Image 11

NASA Image and Video Library

2015-09-08

This image, taken by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image, with a resolution of 450 feet 140 meters per pixel, was taken on August 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19887

Dawn HAMO Image 49

NASA Image and Video Library

2015-10-30

This image, taken by NASA Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 915 miles 1,470 kilometers. The image was taken on Sept. 22, 2015, and has a resolution of 450 feet 140 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19991

Dawn Survey Orbit Image 33

NASA Image and Video Library

2015-07-23

This image, taken on June 25, 2015 by NASA Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles 4,400 kilometers, with a resolution of 1,400 feet 410 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19602

Dawn Survey Orbit Image 45

NASA Image and Video Library

2015-08-11

This image, taken June 6, 2015 by NASA Dawn spacecraft, shows Haulani crater on Ceres from an altitude of 2,700 miles 4,400 kilometers with a resolution of 1,400 feet 410 meters per pixel. North on Ceres is toward upper right. http://photojournal.jpl.nasa.gov/catalog/PIA19621

Modeling and Simulation of an Unmanned Ground Vehicle Power System

DTIC Science & Technology

2014-08-07

Modeling and Simulation of an Unmanned Ground Vehicle Power System John Broderick Jack Hartner Dawn Tilbury Ella Atkins Sponsored by U.S...5a. CONTRACT NUMBER 5b. GRANT NUMBER 5c. PROGRAM ELEMENT NUMBER 6. AUTHOR(S) John Broderick ; Jack Hartner; Dawn Tilbury; Ella Atkins 5d. PROJECT

Travels With Mullen

Science.gov Websites

Department of Defense Submit Search Operation New Dawn September 2010 More Stories Mullen Gets Afghanistan mission officially transfer to the civilian-led Operation New Dawn, Navy Adm. Mike Mullen, chairman of the Operation Atlantic Resolve Sexual Assault Prevention Asia-Pacific Rebalance Cyber Strategy News Today in DOD

Club Drugs. The DAWN Report.

ERIC Educational Resources Information Center

Substance Abuse and Mental Health Services Administration (DHHS/PHS), Rockville, MD. Office of Applied Studies.

This report was prepared in response to requests from the media, law enforcement, and community leaders for information about club drugs. By being able to utilize statistics from hospital emergency departments and by compiling statistics on drug-related deaths, the Drug Abuse Warning Network (DAWN) is able to alert parents, educators, and others…

Juling Crater's Floor

NASA Image and Video Library

2018-03-14

This view from NASA's Dawn mission shows the floor of Ceres' Juling Crater. The crater floor shows evidence of the flow of ice and rock, similar to rock glaciers in Earth's polar regions. Dawn acquired the picture with its framing camera on Aug. 30, 2016. https://photojournal.jpl.nasa.gov/catalog/PIA21920

Dawn: Testing Paradigms by Exploring Dichotomies

NASA Astrophysics Data System (ADS)

Russell, C. T.; Schmidt, B. E.; Wise, J.; Ristvey, J.; Raymond, C. A.

2010-12-01

NASA’s Dawn mission represents a series of “firsts” for major NASA missions. Dawn is the first major NASA science mission to use ion propulsion engines, allowing Dawn to be the first mission to orbit one target and then leave its gravity well to explore a second destination. Dawn is the first science mission to the main asteroid belt, reaching protoplanet Vesta in summer 2011, and will be the first mission to reach a “dwarf planet” when it arrives at Ceres in 2015. By targeting both Vesta and Ceres, Dawn explores two intriguing dichotomies in the solar system, that of the dry rocky planets and the wet icy bodies (Fire and Ice) and the dichotomy between planets and asteroids. Is there a clear dividing line here? Vesta, the second most massive asteroid, is a protoplanet: a round, mostly intact asteroid that bears more resemblance to a planet than to smaller asteroids. Vesta is also the likely parent body of the HED meteorites that richly populate Earth’s meteorite collections. It is possible to hold a piece of Vesta in your hands. From the HED meteorites, scientists have learned the Vesta is one of few differentiated asteroids. And from its spectrum, rich in basaltic minerals, it is known to be much like a mini-version of Earth’s Moon and Mercury. Vesta’s surface once was home to floods of lava not unlike those found still today on the Earth. Vesta is very similar to a terrestrial planet. Ceres is the giant of the asteroid belt with a hydrostatic shape that earns it a dwarf planet classification. Like its larger cousins, Ceres’ round shape suggests that the body may be differentiated, but due to its low density, Ceres’ interior is more like an icy moon of Jupiter. Beneath a relatively thin clay veneer probably lies an ice-rich mantle and rocky core, and even possibly a liquid ocean. With such enticing questions posed for Vesta and Ceres, Dawn will enable scientists and the public alike to explore how planets were born, how fire and ice have shaped the solar system, and have a chance to push the boundaries of our own classification system. Dawn’s set of instrumentation, with cameras, a visible and infrared spectrometer, a gamma ray and neutron detector and radio science, will produce a wealth of information about two previously unexplored, diverse and yet somehow familiar worlds. Communication of the lessons learned by Dawn from the scientists to the public has and will occur over a range of interfaces, including a series of online activities such as Find a Meteorite, Clickworkers and a simulation of an ion engine. Other activities include Dawn “Science of the Day” archives, fun family activities and games as well as classroom materials and outreach events. Since the two bodies are the brightest sources in the main belt, an integral part of Dawn’s journey has been the integration of amateur and “backyard” astronomers. All these activities allow us to share the science with the public. Dawn arrives at Vesta in the middle of the Year of the Solar System in July 2011 and will depart for Ceres as the YSS ends.

"How I do it"--radical right colectomy with side-to-side stapled ileo-colonic anastomosis.

PubMed

Hübner, M; Larson, D W; Wolff, B G

2012-08-01

Standardization of surgical technique helps to reproduce excellent clinical outcomes, especially in teaching institutions. We aim to describe in detail our established approach for oncological right colectomy. The right colon is mobilized in a five-step latero-inferior approach starting off with the terminal ileum, visualizing the duodenum and the head of pancreas. The ascending colon is dissected from the retroperitoneum, and takedown of the hepatic flexure is completed coming retrograde from the transverse colon. Transection of the remaining retroperitoneal attachments completes exposure of the duodenum and mobilization of the right colon. Ileocolic vessels are dissected out and divided close to their origin, and the mesocolon is divided. We then establish intestinal continuity by use of a side-to-side stapled technique. The arms of a linear cutting stapler are inserted via transverse incisions at the anti-mesenteric sides of the terminal ileum and the transverse colon (tenia) and fired. The enterotomy site is closed by removal of the specimen using a second transverse firing of the linear cutting stapler. An important final step is the reinforcement of the anastomotic ends and the crossing of the staple lines; an omental patch and closure of the mesenteric window are optional. The suggested standardized five-step lateral-to-medial dissection of the right colon and the three-step side-to-side stapled technique for ileo-colonic anastomosis are easy to learn and to reproduce. Careful adherence to pivotal technical details will help to obtain an optimal oncological outcome and a consistently low leak rate around 2%.

Impact of the storm-time plasma sheet ion composition on the ring current energy density

NASA Astrophysics Data System (ADS)

Mouikis, C.; Kistler, L. M.; Petrinec, S. M.; Fuselier, S. A.; Cohen, I.

2017-12-01

The adiabatic inward transport of the night-side near-earth ( 6 Re) hot plasma sheet is the dominant contributor to the ring current pressure during storm times. During storm times, the plasma sheet composition in the 6 - 12 Re tail region changes due to O+ entry from the lobes (from the cusp) and the direct feeding from the night side auroral region. In addition, at substorm onset the plasma sheet O+ ions can be preferentially accelerated. We use MMS and observations during two magnetic storms, 5/8/2016 and 7/16/2017, to monitor the composition changes and energization in the 6 - 12 Re plasma sheet region. For both storms the MMS apogee was in the tail. In addition, we use subsequent Van Allen Probe observations (with apogee in the dawn and dusk respectively) to test if the 6-12 Re plasma sheet, observed by MMS, is a sufficient source of the O+ in the ring current. For this we will compare the phase space density (PSD) of the plasma sheet source population and the PSD of the inner magnetosphere at constant magnetic moment values as used in Kistler et al., [2016].

Preliminary infrared radiometry of the night side of mercury from mariner 10.

PubMed

Chase, S C; Miner, E D; Morrison, D; Münch, G; Neugebauer, G; Schroeder, M

1974-07-12

The infrared radiometer on Mariner 10 measured the thermal emission from the planet with a spatial resolution element as small as 40 kilometers in a broad wavelength band centered at 45 micrometers. The minimum brightness temperature (near local midnight) in these near-equatorial scans was 100 degrees K. Along the track observed, the temperature declined steadily from local sunset to near midnight, behaving as would be expected for a homogeneous, porous material with a thermal inertia of 0.0017 cal cm(-2) sec(-(1/2)) degrees K(-1), a value only slightly larger than that of the moon. From near midnight to dawn, however, the temperature fluctuated over a range of about 10 degrees K, implying the presence of regions having thermal inertia as high as 0.003 cal cm(-2) sec-(1/2) degrees K(-1).

KSC-2009-2725

NASA Image and Video Library

2009-04-17

CAPE CANAVERAL, Fla. – Just before dawn, space shuttle Endeavour is bathed in xenon lights after being secured on Launch Pad 39B at NASA's Kennedy Space Center in Florida. First motion on rollout from the Vehicle Assembly Building was at 11:57 p.m. EDT April 16. On either side of the pad are two of the new lightning towers erected for NASA's Constellation Program, which will use the pad for Ares rocket launches. Endeavour will be prepared on the pad for liftoff in the unlikely event that a rescue mission is necessary following space shuttle Atlantis' launch on the STS-125 mission to service NASA's Hubble Space Telescope. After Atlantis is cleared to land, Endeavour will move to Launch Pad 39A for its upcoming STS-127 mission to the International Space Station, targeted to launch June 13. Photo credit: NASA/Dimitri Gerondidakis

Electron transfer dissociation of synthetic and natural peptides containing lanthionine/methyllanthionine bridges.

PubMed

Dolle, Ashwini B; Jagadeesh, Narasimhappagari; Bhaumik, Suman; Prakash, Sunita; Biswal, Himansu S; Gowd, Konkallu Hanumae

2018-06-15

The modes of cleavage of lanthionine/methyllanthionine bridges under electron transfer dissociation (ETD) were investigated using synthetic and natural lantipeptides. Knowledge of the mass spectrometric fragmentation of lanthionine/methyllanthionine bridges may assist in the development of analytical methods for the rapid discovery of new lantibiotics. The present study strengthens the advantage of ETD in the characterization of posttranslational modifications of peptides and proteins. Synthetic and natural lantipeptides were obtained by desulfurization of peptide disulfides and cyanogen bromide digestion of the lantibiotic nisin, respectively. These peptides were subjected to electrospray ionization collision-induced dissociation tandem mass spectrometry (CID-MS/MS) and ETD-MS/MS using an HCT ultra ETDII ion trap mass spectrometer. MS 3 CID was performed on the desired product ions to prove cleavage of the lanthionine/methyllanthionine bridge during ETD-MS/MS. ETD has advantages over CID in the cleavage of the side chain of lanthionine/methyllanthionine bridges. The cleavage of the N-Cα backbone peptide bond followed by C-terminal side chain of the lanthionine bridge results in formation of c •+ and z + ions. Cleavage at the preceding peptide bond to the C-terminal side chain of lanthionine/methyllanthionine bridges yields specific fragments with the cysteine/methylcysteine thiyl radical and dehydroalanine. ETD successfully cleaves the lanthionine/methyllanthionine bridges of synthetic and natural lantipeptides. Diagnostic fragment ions of ETD cleavage of lanthionine/methyllanthionine bridges are the N-terminal cysteine/methylcysteine thiyl radical and C-terminal dehydroalanine. Detection of the cysteine/methylcysteine thiyl radical and dehydroalanine in combined ETD-CID-MS may be used for the rapid identification of lantipeptide natural products. Copyright © 2018 John Wiley & Sons, Ltd.

A Description of Local Time Asymmetries in the Kronian Current Sheet

NASA Astrophysics Data System (ADS)

Nickerson, J. S.; Hansen, K. C.; Gombosi, T. I.

2012-12-01

Cassini observations imply that Saturn's magnetospheric current sheet is displaced northward above the rotational equator [C.S. Arridge et al., Warping of Saturn's magnetospheric and magnetotail current sheets, Journal of Geophysical Research, Vol. 113, August 2008]. Arridge et al. show that this hinging of the current sheet above the equator occurs over the noon, midnight, and dawn local time sectors. They present an azimuthally independent model to describe this paraboloid-like geometry. We have used our global MHD model, BATS-R-US/SWMF, to study Saturn's magnetospheric current sheet under various solar wind dynamic pressure and solar zenith angle conditions. We show that under reasonable conditions the current sheet does take on the basic shape of the Arridge model in the noon, midnight, and dawn sectors. However, the hinging distance parameter used in the Arridge model is not a constant and does in fact vary in Saturn local time. We recommend that the Arridge model should be adjusted to account for this azimuthal dependence. Arridge et al. does not discuss the shape of the current sheet in the dusk sector due to an absence of data but does presume that the current sheet will assume the same geometry in this region. On the contrary, our model shows that this is not the case. On the dusk side the current sheet hinges (aggressively) southward and cannot be accounted for by the Arridge model. We will present results from our simulations showing the deviation from axisymmetry and the general behavior of the current sheet under different conditions.

KSC-07pd2061

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — On Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is safely secured on a transporter for its trip to Astrotech. Dawn is being returned to the Astrotech payload processing facility to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/George Shelton

KSC-07pd2058

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — On Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lowered from the mobile service tower to the ground. Dawn is being returned to the Astrotech payload processing facility to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/George Shelton

KSC-07pd2059

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — On Pad 17-B at Cape Canaveral Air Force Station, the Dawn spacecraft is lowered from the mobile service tower to the ground. Dawn is being returned to the Astrotech payload processing facility to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/George Shelton

Efficient peptide ligation between allyl-protected Asp and Cys followed by palladium-mediated deprotection.

PubMed

Kamo, Naoki; Hayashi, Gosuke; Okamoto, Akimitsu

2018-04-24

An efficient method for peptide ligation between C-terminal Asp(OAllyl) and N-terminal Cys has been developed. Peptide ligation and removal of the allyl group at the Asp carboxylate side chain proceeded in one pot by adding a small amount of Pd/TPPTS complex. Based on this efficient synthetic method, PEP-19 (61 amino acids), which is highly expressed in Purkinje cells, was synthesized.

SPERTI Terminal Building (PER604) is under construction in foreground, with ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

SPERT-I Terminal Building (PER-604) is under construction in foreground, with vertical metal siding partially affixed to gable end of building. Utility lines are laid in shallow trench to Reactor Pit and Instrument Cell Buildings also under construction in distance. Photographer: R.G. Larsen. Date: April 22, 1955. INEEL negative no. 55-1001 - Idaho National Engineering Laboratory, SPERT-I & Power Burst Facility Area, Scoville, Butte County, ID

Interim Service ISDN Satellite (ISIS) hardware experiment development for advanced ISDN satellite designs and experiments

NASA Technical Reports Server (NTRS)

Pepin, Gerard R.

1992-01-01

The Interim Service Integrated Service Digital Network (ISDN) Satellite (ISIS) Hardware Experiment Development for Advanced Satellite Designs describes the development of the ISDN Satellite Terminal Adapter (ISTA) capable of translating ISDN protocol traffic into Time Division Multiple Access (TDMA) signals for use by a communications satellite. The ISTA connects the Type 1 Network Termination (NT1) via the U-interface on the line termination side of the CPE to the RS-499 interface for satellite uplink. The same ISTA converts in the opposite direction the RS-499 to U-interface data with a simple switch setting.

Interim Service ISDN Satellite (ISIS) hardware experiment design for advanced ISDN satellite design and experiments

NASA Technical Reports Server (NTRS)

Pepin, Gerard R.

1992-01-01

The Interim Service Integrated Services Digital Network (ISDN) Satellite (ISIS) Hardware Experiment Design for Advanced Satellite Designs describes the design of the ISDN Satellite Terminal Adapter (ISTA) capable of translating ISDN protocol traffic into time division multiple access (TDMA) signals for use by a communications satellite. The ISTA connects the Type 1 Network Termination (NT1) via the U-interface on the line termination side of the CPE to the V.35 interface for satellite uplink. The same ISTA converts in the opposite direction the V.35 to U-interface data with a simple switch setting.

Dawn Survey Orbit Image 20

NASA Image and Video Library

2015-07-06

This image, taken by NASA's Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 22, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19588

Dawn Survey Orbit Image 29

NASA Image and Video Library

2015-07-17

This image, taken by NASA's Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 25, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19597

Dawn Survey Orbit Image 17

NASA Image and Video Library

2015-06-30

This image, taken by NASA's Dawn spacecraft, shows a portion of the southern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 16, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19585

Dawn Survey Orbit Image 25

NASA Image and Video Library

2015-07-13

This image, taken by NASA's Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 24, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19593

Dawn Survey Orbit Image 24

NASA Image and Video Library

2015-07-10

This image, taken by NASA's Dawn spacecraft, shows a portion of the northern hemisphere of dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 21, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA19592

Dawn Survey Orbit Image 46

NASA Image and Video Library

2015-08-12

This image, taken on June 6, 2015 by NASA Dawn spacecraft, shows a mountain on Ceres at center-left that is 4 miles 6 kilometers high, from an altitude of 2,700 miles 4,400 kilometers with a resolution of 1,400 feet 410 meters per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA19622

76 FR 35259 - In the Matter of Dawn Technologies, Inc., Distinctive Devices, Inc., Haber, Inc., and...

Federal Register 2010, 2011, 2012, 2013, 2014

2011-06-16

... SECURITIES AND EXCHANGE COMMISSION [File No. 500-1] In the Matter of Dawn Technologies, Inc., Distinctive Devices, Inc., Haber, Inc., and Independence Brewing Co.; Order of Suspension of Trading June 14... a lack of current and accurate information concerning the securities of Independence Brewing Co...

DAWN Handbook: Teaching Students with Disabilities--Guidelines for Academic Staff

ERIC Educational Resources Information Center

Kennedy, Stephen; Treanor, Declan; O'Grady, Mary

2008-01-01

This guide was developed by DAWN (Disability Advisors Working Network) in consultation with AHEAD (Association for Higher Education Access and Disability), Asperger Syndrome Association of Ireland, Brainwave, DeafHear, Dyslexia Association of Ireland and the National Council for the Blind. This is an introductory guide and should be used as a…

Wejkwapniaq (Coming of the Dawn).

ERIC Educational Resources Information Center

Christmas, Peter

Just as the Micmac word "wejkwapniaq" may be interpreted in several ways, the title of this compilation of fact, folklore, and history of the Micmac people can be interpreted to mean "The Dawn of Nova Scotia History" or "The Coming of New and Bad Things for the Micmac". This teacher's guide provides information on the…

DAWN Mission Bus and Waveguide Venting Analysis Review

NASA Technical Reports Server (NTRS)

Cragg, Clinton H.; Kichak, Robert A.; Sutter, James K.; Holder, Donald; Jeng, Frank; Ruitberg, Arthur; Sank, Victor

2007-01-01

A concern was raised regarding the time after launch when the DAWN Mission Communications Subsystem, which contains a 100 Watt X-Band Traveling Wave Tube Amplifier (TWTA) with a high voltage ((approximately 7 Kilo Volt (KV)) Electronic Power Converter (EPC), will be powered on for the first post-launch downlink. This activation is planned to be approximately one hour after launch. Orbital Sciences (the DAWN Mission spacecraft contractor) typically requires a 24-hour wait period prior to high voltage initiation for Earth-orbiting Science and GEO spacecraft. The concern relates to the issue of corona and/or radio frequency (RF) breakdown of the TWTA ((high voltage direct current (DC) and RF)), and of the microwave components (high voltage RF) in the presence of partial atmospheric pressures or outgassing constituents. In particular, generally the diplexer and circulator are susceptible to RF breakdown in the corona region due to the presence of small physical gaps (( 2.5 millimeter (mm)) between conductors that carry an RF voltage. The NESC concurred the DAWN Mission communication system is safe for activation.

Dawn Arrives at Vesta: The Smallest Terrestrial Planet

NASA Astrophysics Data System (ADS)

Russell, C. T.; Raymond, C. A.; Coradini, A.; Nathues, A.; De Sanctis, M. C.; Prettyman, T. H.; Jaumann, R.; McSween, H. Y.; McCord, T. B.; Keller, H. U.; Rayman, M.

2011-12-01

The Dawn Mission is a revolutionary concept in planetary exploration. Within the cost cap of a low-cost Discovery mission, a spacecraft has been flown to the main asteroid belt and been put into orbit around its second most massive body, 4 Vesta. Vesta was clearly beginning its march to planet-hood when its accretion stopped, most probably by the formation of Jupiter. Dawn's exploration is enabled by an ion propulsion system that will not only allow Dawn to descend to 200 km altitude, but to leave Vesta, travel to and orbit 1 Ceres in 2015 and map this largest main belt asteroid, a dwarf planet. The initial images of the surface of Vesta have been astounding. They reveal the diverse geochemical processes driven by the internal heat of this 530 km diameter body and titanic forces that have battered Vesta for over 4.65 billion years. A large southern impact structure, troughs ringing the equator, striped craters, dark albedo features contrasting with very high albedo features and a richly colored surface distinguish this most unusual small world.

The role of PDF neurons in setting the preferred temperature before dawn in Drosophila

PubMed Central

Tang, Xin; Roessingh, Sanne; Hayley, Sean E; Chu, Michelle L; Tanaka, Nobuaki K; Wolfgang, Werner; Song, Seongho; Stanewsky, Ralf; Hamada, Fumika N

2017-01-01

Animals have sophisticated homeostatic controls. While mammalian body temperature fluctuates throughout the day, small ectotherms, such as Drosophila achieve a body temperature rhythm (BTR) through their preference of environmental temperature. Here, we demonstrate that pigment dispersing factor (PDF) neurons play an important role in setting preferred temperature before dawn. We show that small lateral ventral neurons (sLNvs), a subset of PDF neurons, activate the dorsal neurons 2 (DN2s), the main circadian clock cells that regulate temperature preference rhythm (TPR). The number of temporal contacts between sLNvs and DN2s peak before dawn. Our data suggest that the thermosensory anterior cells (ACs) likely contact sLNvs via serotonin signaling. Together, the ACs-sLNs-DN2s neural circuit regulates the proper setting of temperature preference before dawn. Given that sLNvs are important for sleep and that BTR and sleep have a close temporal relationship, our data highlight a possible neuronal interaction between body temperature and sleep regulation. DOI: http://dx.doi.org/10.7554/eLife.23206.001 PMID:28463109

Studying Cosmic Dawn with WFIRST

NASA Astrophysics Data System (ADS)

Rhoads, James; Malhotra, Sangeeta; Jansen, Rolf A.; Windhorst, Rogier; Tilvi, Vithal; Finkelstein, Steven; Wold, Isak; Papovich, Casey; Fan, Xiaohui; Mellema, Garrelt; Zackrisson, Erik; Jensen, Hannes; T

2018-01-01

Our understanding of Cosmic Dawn can be revolutionized using WFIRST's combination of wide-field, sensitive, high resolution near-infrared imaging and spectroscopy. Guest investigator studies of WFIRST's high latitude imaging survey and supernova search fields will yield orders of magnitude increases in our samples of Lyman break galaxies from z=7 to z>12. The high latitude spectrsocopic survey will enable an unprecedented search for z>7 quasars. Guest observer deep fields can extend these studies to flux levels of Hubble's deepest fields, over regions measured in square degrees. The resulting census of luminous objects in the Cosmic Dawn will provide key insights into the sources of the ultraviolet photons that powered reionization. Moreover, because WFIRST has a wide field (slitless) spectroscopic capability, it can be used to search for Lyman alpha emitting galaxies over the full history of reionization. By comparing the Lyman alpha galaxy statistics to those of continuum sources, we can directly probe the transparency of the intergalactic gas and chart reionization history.Our team is planning for both Guest Investigator and Guest Observer applications of WFIRST to studying Cosmic Dawn, and welcomes dialog with other interested members of the community.

Ceres During Opposition Surge.

NASA Image and Video Library

2017-05-16

NASA's Dawn spacecraft successfully observed Ceres at opposition on April 29, 2017, taking images from a position exactly between the sun and Ceres' surface. Mission specialists had carefully maneuvered Dawn into a special orbit so that the spacecraft could view Occator Crater, which contains the brightest area of Ceres, from this new perspective. A movie shows these opposition images, with contrast enhanced to highlight brightness differences. The bright spots of Occator stand out particularly well on an otherwise relatively bland surface. Dawn took these images from an altitude of about 12,000 miles (20,000 kilometers). Based on data from ground-based telescopes and spacecraft that have previously viewed planetary bodies at opposition, scientists predicted that Ceres would appear brighter from this opposition configuration. This increase in brightness, or "surge," relates the size of the grains of material on the surface, as well as how porous those materials are. The science motivation for performing these observations is further explained in the March 2017 issue of the Dawn Journal blog. A movie can be viewed at https://photojournal.jpl.nasa.gov/catalog/PIA21405

Association of infantile bruxism and the terminal relationships of the primary second molars.

PubMed

Junqueira, Tatiana Helena; Nahás-Scocate, Ana Carla Raphaelli; Valle-Corotti, Karyna Martins do; Conti, Ana Claudia de Castro Ferreira; Trevisan, Shirley

2013-01-01

The aim of this study was to analyze the association between infantile bruxism and the terminal relationships of the primary second molars. A total of 937 pre-school children (both genders), aged from 2 to 6 years, from municipal schools in São Paulo were evaluated. In this study, a questionnaire considering the bruxism habit and the presence of headaches and/or restless sleep was answered by the parents/guardians. A clinical exam of occlusion in the anteroposterior direction (vertical plane - VP, mesial step - MS and distal step - DS) was performed by the examiners in the school environment. Student's t test, Fisher's test and a logistic regression test were applied for the statistical analysis at a significance level of 5%. The prevalence of the bruxism habit was 29.3% among the total sample. Because there was no significant difference between the sides evaluated, the left side was taken as the standard. Among those children with bruxism, 25.7% presented a mesial step terminal relationship at the primary second molars, 29.1% had DS, and 30.2% had VP. Regarding the association of the parafunctional habit with the type of terminal relationship, no significant results were found. Children who slept restlessly or suffered from headaches were verified to show a higher chance of expressing the habit (OR = 2.4 and 1.6, respectively). The prevalence of bruxism in the studied sample was 29.3%, and its association with the primary second molars' terminal relationship was not statistically significant.

Crystal structure of Cex1p reveals the mechanism of tRNA trafficking between nucleus and cytoplasm.

PubMed

Nozawa, Kayo; Ishitani, Ryuichiro; Yoshihisa, Tohru; Sato, Mamoru; Arisaka, Fumio; Kanamaru, Shuji; Dohmae, Naoshi; Mangroo, Dev; Senger, Bruno; Becker, Hubert D; Nureki, Osamu

2013-04-01

In all eukaryotes, transcribed precursor tRNAs are maturated by processing and modification processes in nucleus and are transported to the cytoplasm. The cytoplasmic export protein (Cex1p) captures mature tRNAs from the nuclear export receptor (Los1p) on the cytoplasmic side of the nuclear pore complex, and it delivers them to eukaryotic elongation factor 1α. This conserved Cex1p function is essential for the quality control of mature tRNAs to ensure accurate translation. However, the structural basis of how Cex1p recognizes tRNAs and shuttles them to the translational apparatus remains unclear. Here, we solved the 2.2 Å resolution crystal structure of Saccharomyces cerevisiae Cex1p with C-terminal 197 disordered residues truncated. Cex1p adopts an elongated architecture, consisting of N-terminal kinase-like and a C-terminal α-helical HEAT repeat domains. Structure-based biochemical analyses suggested that Cex1p binds tRNAs on its inner side, using the positively charged HEAT repeat surface and the C-terminal disordered region. The N-terminal kinase-like domain acts as a scaffold to interact with the Ran-exportin (Los1p·Gsp1p) machinery. These results provide the structural basis of Los1p·Gsp1p·Cex1p·tRNA complex formation, thus clarifying the dynamic mechanism of tRNA shuttling from exportin to the translational apparatus.

Spherical harmonic representation of the main geomagnetic field for world charting and investigations of some fundamental problems of physics and geophysics

NASA Technical Reports Server (NTRS)

Barraclough, D. R.; Hide, R.; Leaton, B. R.; Lowes, F. J.; Malin, S. R. C.; Wilson, R. L. (Principal Investigator)

1982-01-01

Progress in the harmonic analysis of MAGSAT data is reported. Single-day data sets were subdivided into information on the sunrise side of the Earth and information on the sunset side of the Earth. Data for the main and external fields each demonstrate a clear and consistent systematic difference between the sets of data which was determined to be, due to ionospheric currents which differ from the sunset to the sunrise terminator. A toroidal field was analyzed for and determined to be an apparent toroidal field resulting from electric currents concentrated in the two terminators. Progressive elimination of auroral zone data demonstrates that the information presented does not arise from complications due to Birkeland currents.

Enhanced Early View of Ceres from Dawn

NASA Image and Video Library

2014-12-05

As the Dawn spacecraft flies through space toward the dwarf planet Ceres, the unexplored world appears to its camera as a bright light in the distance, full of possibility for scientific discovery. This view was acquired as part of a final calibration of the science camera before Dawn's arrival at Ceres. To accomplish this, the camera needed to take pictures of a target that appears just a few pixels across. On Dec. 1, 2014, Ceres was about nine pixels in diameter, nearly perfect for this calibration. The images provide data on very subtle optical properties of the camera that scientists will use when they analyze and interpret the details of some of the pictures returned from orbit. Ceres is the bright spot in the center of the image. Because the dwarf planet is much brighter than the stars in the background, the camera team selected a long exposure time to make the stars visible. The long exposure made Ceres appear overexposed, and exaggerated its size; this was corrected by superimposing a shorter exposure of the dwarf planet in the center of the image. A cropped, magnified view of Ceres appears in the inset image at lower left. The image was taken on Dec. 1, 2014 with the Dawn spacecraft's framing camera, using a clear spectral filter. Dawn was about 740,000 miles (1.2 million kilometers) from Ceres at the time. Ceres is 590 miles (950 kilometers) across and was discovered in 1801. http://photojournal.jpl.nasa.gov/catalog/PIA19050

Evidence for ground-ice occurrence on asteroid Vesta using Dawn bistatic radar observations

NASA Astrophysics Data System (ADS)

Palmer, E. M.; Heggy, E.; Kofman, W. W.

2017-12-01

From 2011 to 2012, the Dawn spacecraft orbited asteroid Vesta, the first of its two targets in the asteroid belt, and conducted the first bistatic radar (BSR) experiment at a small-body, during which Dawn's high-gain communications antenna is used to transmit radar waves that scatter from Vesta's surface toward Earth at high incidence angles just before and after occultation of the spacecraft behind the asteroid. Among the 14 observed mid-latitude forward-scatter reflections, the radar cross section ranges from 84 ± 8 km2 (near Saturnalia Fossae) to 3,588 ± 200 km2 (northwest of Caparronia crater), implying substantial spatial variation in centimeter- to decimeter-scale surface roughness. The compared distributions of surface roughness and subsurface hydrogen concentration [H]—measured using data from Dawn's BSR experiment and Gamma Ray and Neutron Spectrometer (GRaND), respectively—reveal the occurrence of heightened subsurface [H] with smoother terrains that cover tens of square kilometers. Furthermore, unlike on the Moon, we observe no correlation between surface roughness and surface ages on Vesta—whether the latter is derived from lunar or asteroid-flux chronology [Williams et al., 2014]—suggesting that cratering processes alone are insufficient to explain Vesta's surface texture at centimeter-to-decimeter scales. Dawn's BSR observations support the hypothesis of transient melting, runoff and recrystallization of potential ground-ice deposits, which are postulated to flow along fractures after an impact, and provide a mechanism for the smoothing of otherwise rough, fragmented impact ejecta. Potential ground-ice presence within Vesta's subsurface was first proposed by Scully et al. [2014], who identified geomorphological evidence for transient water flow along several of Vesta's crater walls using Dawn Framing Camera images. While airless, differentiated bodies such as Vesta and the Moon are thought to have depleted their initial volatile content during the process of differentiation, evidence to the contrary is continuing to change our understanding of the distribution and preservation of volatiles during planetary formation in the early solar system.

Ceres' Evolution Before and After Dawn: Where are We Now?

NASA Astrophysics Data System (ADS)

McCord, T. B.; Castillo, J. C.

2016-12-01

Observations of Ceres before Dawn indicated that it contains 25 wt% water, and thermodynamic modeling indicated Ceres probably had experienced the same process of differentiation due to melting of the original ice after accretion as experienced by large icy moons. Consistent with that was a surface of altered mineralogy like clays suggesting aqueous alteration of the original chondritic silicates. Dawn has revealed some concentration of mass toward the center, specific aqueously altered mineralogies, a stiff surface with weaker material beneath, and extrusions and protrusions suggesting recent subsurface activity, including exposures of water ice that must be very recent. This wealth of new information from Dawn enables selection of more specific evolution models that best match the vastly improved Dawn observations. In this new study we propose one possibility is that Ceres accreted as an ice and silicate mixture after short-lived radionuclides in CAIs had significantly decayed, i.e. nearer 5 my after CAIs, and thus differentiated less completely than for hotter models. On the other hand, the presence of heavily aqueously altered mineralogies, including probably salts, suggests extensive mixing of water and silicates, which might normally be associated with more complete differentiation. Geologically recent activity, perhaps even to the present time, seems evident from several young landforms, including protrusions consistent with diapirism and recent exposures of water ice. This suggests recent flexing of the subsurface and rising of less dense interior material, including salts and ice. The presence of ammoniated minerals and what appear to be salt deposits suggest a major lowering of subsurface water ice melting temperature, enhancing the duration of water-silicate contact, and perhaps accelerating the mineralization processes and slowing or halting differentiation of water and silicates. Thus, Ceres is becoming known as the first body outward from the Sun that has had its evolution controlled by water-driven processes. Investigations of its interior and geology enable by Dawn's observations will in turn help to better understand other ice-rich bodies.

Ceres' evolution before and after Dawn: Where are we now?

NASA Astrophysics Data System (ADS)

McCord, Thomas B.; Castillo-Rogez, Julie C.

2016-10-01

Observations of Ceres before Dawn indicated that it contains ~25 wt% water, and thermodynamic modeling indicated Ceres probably had experienced the same process of differentiation due to melting of the original ice after accretion as experienced by large icy moons. Consistent with that was a surface of altered mineralogy like clays suggesting aqueous alteration of the original chondritic silicates. Dawn has revealed some concentration of mass toward the center, specific aqueously altered mineralogies, a stiff surface with weaker material beneath, and extrusions and protrusions suggesting recent subsurface activity, including exposures of water ice that must be very recent. This wealth of new information from Dawn enables selection of more specific evolution models that best match the vastly improved Dawn observations. In this new study we propose one possibility is that Ceres accreted as an ice and silicate mixture after short-lived radionuclides in CAIs had significantly decayed, i.e. nearer 5 my after CAIs, and thus differentiated less completely than for hotter models. On the other hand, the presence of heavily aqueously altered mineralogies, including probably salts, suggests extensive mixing of water and silicates, which might normally be associated with more complete differentiation. Geologically recent activity, perhaps even to the present time, seems evident from several young landforms, including protrusions consistent with diapirism and recent exposures of water ice. This suggests recent flexing of the subsurface and rising of less dense interior material, including salts and ice. The presence of ammoniated minerals and what appear to be salt deposits suggest a major lowering of subsurface water ice melting temperature, enhancing the duration of water-silicate contact, and perhaps accelerating the mineralization processes and slowing or halting differentiation of water and silicates. Thus, Ceres is becoming known as the first body outward from the Sun that has had its evolution controlled by water-driven processes. Investigations of its interior and geology enable by Dawn's observations will in turn help to better understand other ice-rich bodies.

Migrating the Dawn Data Archive to the PDS4 Standard

NASA Astrophysics Data System (ADS)

Joy, S. P.; Mafi, J. N.; King, T. A.; Raymond, C. A.; Russell, C. T.

2017-12-01

The Dawn mission was proposed prior to the development of the PDS4 standard and all of its data are archived at the PDS Small Bodies Node (SBN) using the older PDS3 standard. Plans to migrate the existing PDS archives to PDS4 have been discussed within PDS for some time, and have been reemphasized in the PDS Roadmap Study for 2017 - 2026 (https://pds.nasa.gov/roadmap/PlanetaryDataSystemRMS17-26_20jun17.pdf). Updating the Dawn metadata to PDS4 would enable users of those data to take advantage of new capabilities offered by PDS4, and insure the full compatibility of past archives with current and future PDS4 tools and services. The Dawn data themselves will not require any reformatting during the migration to PDS4. The data and documentation will need to be reorganized and the metadata enhanced to fill in the gaps in the PDS3 metadata. The planned migration to PDS4 would be primarily carried out at the Dawn Science Center (DSC) at UCLA but the activity will require close coordination with the PDS-SBN. The PDS4 standard allows individual nodes to customize the metadata through the use of optional parameters and local data dictionaries to satisfy discipline and mission specific search and retrieval requirements and support node tools and services. The DSC shares much of its staff with the Planetary Plasma Interactions (PPI) Node of the PDS. This sharing of personnel means that the DSC staff are well versed in the PDS4 standard, have actively participated in the development of this standard, and are fully trained in the use of PPI tools for PDS4 metadata migration and/or generation. The combination of PDS4 training and detailed understanding of the Dawn mission, instruments, and datasets makes the DSC the most cost-effective organization to migrate these data to PDS4.

A Fault Location Algorithm for Two-End Series-Compensated Double-Circuit Transmission Lines Using the Distributed Parameter Line Model

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

Kang, Ning; Gombos, Gergely; Mousavi, Mirrasoul J.

A new fault location algorithm for two-end series-compensated double-circuit transmission lines utilizing unsynchronized two-terminal current phasors and local voltage phasors is presented in this paper. The distributed parameter line model is adopted to take into account the shunt capacitance of the lines. The mutual coupling between the parallel lines in the zero-sequence network is also considered. The boundary conditions under different fault types are used to derive the fault location formulation. The developed algorithm directly uses the local voltage phasors on the line side of series compensation (SC) and metal oxide varistor (MOV). However, when potential transformers are not installedmore » on the line side of SC and MOVs for the local terminal, these measurements can be calculated from the local terminal bus voltage and currents by estimating the voltages across the SC and MOVs. MATLAB SimPowerSystems is used to generate cases under diverse fault conditions to evaluating accuracy. The simulation results show that the proposed algorithm is qualified for practical implementation.« less

Interfacial preparation and optical transmission surface plasmon resonance of Janus metamaterials membrane

NASA Astrophysics Data System (ADS)

Du, Yixuan; Zhang, Xiaowei; Li, Yunbo

2018-01-01

Janus metamaterials membrane had been fabricated using self-assembly strategy at the oil/water interface with thiol-terminated polymers. Janus metamaterials membrane exhibits a characteristic surface plasmon absorption band, in which the peak position is sensitive to the addition of polymer. The optical transmission surface plasmon resonance (T-SPR) peak has a blue shift at the visible region with addition of thiol-terminated polystyrene (PS-SH). With thiol-terminated poly (ethylene glycol) (PEG-SH) attachment onto the surface side of gold nanoparticles (AuNPs), the T-SPR band has a successive blue shift. One surprising thing is that it has a flat terrace on T-SPR band from 580 to 740 nm. In addition, The T-SPR of Janus metamaterials membrane dramatically changed with the addition PS-SH when the PEG-SH was capped on the opposite side. The morphologies of AuNPs membrane and Janus metamaterials membrane support the above mentioned result of SPR. In virtue of tunable SPR band, the Janus metamaterials membrane has great potential application in science-based design of optical sensing sensors and surface-enhanced optic sensitive detection.

Understanding Volatile Occurrence on Vesta Using Bistatic Radar and GRaND Observations by the Dawn Mission

NASA Astrophysics Data System (ADS)

Palmer, E. M.; Heggy, E.; Kofman, W. W.

2016-12-01

The first orbital bistatic radar experiment was conducted by Dawn at Asteroid Vesta, where Dawn's HGA was used to transmit X-band radio waves and Earth's Deep Space Network (DSN) 70-meter antennas were used to receive. Due to the opportunistic nature of the experiment, the HGA remained in a fixed orientation toward the Earth such that surface radar reflections occurred at grazing incidence angles of 89° just before and after Dawn's occultation behind Vesta. Among the 16 observed echo sites, we find that σ0ranges from -12 dB to -20 dB and has corresponding RMS slopes ranging from 1°- 8°. To assess potential volatile presence, we compare the distribution of RMS slopes to subsurface hydrogen concentrations observed by Dawn's Gamma Ray and Neutron Detector (GRaND) to 1 m depth. While Vesta's surface is thought to have been largely depleted of volatiles during its differentiation, observations by Dawn'sGRaND and VIR instruments suggest the potential introduction of hydrated material through meteoritic impacts. We identify seven sites of potential volatile occurrence—where low roughness (<5°) is observed to be coupled with high content of hydrated materials (0.025 - 0.04 wt%). Such sites support the possibility of volatile presence, as the regolith should otherwise be particularly rough in the absence of smoothening processes such as the melting, run-off and recrystallization of water ice after an impact. The sites correspond to occultation entry orbit numbers 635, 644 and 719—which overlap Divalia Fossae, Marcia crater ejecta and Octavia crater, respectively—and exit orbit numbers 377, 406, 407 and 720—overlapping northern cratered trough terrain, dark material near Aruntia crater and the cratered highlands. Toward comparing volatile occurrence on other small bodies, Dawn'sBSR experiment at Asteroid Ceres raises new questions. How does the range of decimeter-scale RMS slopes compare with Vesta's surface? How well does the distribution of RMS slopes correlate with GRaND's map of subsurface hydrogen concentration? In addition to optimizing future missions' landing and surface trafficability, characterizing small body surface roughness using BSR will enable further investigation into the relationship between volatile presence and decimeter-scale surface roughness.

High resolution Ceres HAMO atlas derived from Dawn FC images

NASA Astrophysics Data System (ADS)

Roatsch, Thomas; Kersten, Elke; Matz, Klaus-Dieter; Preusker, Frank; Scholten, Frank; Jaumann, Ralf; Raymond, Carol A.; Russell, Chris T.

2016-04-01

Introduction: NASA's Dawn spacecraft entered the orbit of dwarf planet Ceres in March 2015, and will characterize the geology, elemental and mineralogical composition, topography, shape, and internal structure of Ceres. One of the major goals of the mission is a global mapping of Ceres. Data: The Dawn mission was mapping Ceres in HAMO (High Altitude Mapping Orbit, 1475 km altitude) between August and October 2015. The framing camera took about 2,600 clear filter images with a resolution of about 140 m/pixel during these cycles. The images were taken with different viewing angles and different illumination conditions. We selected images from one cycle (cycle #1) for the mosaicking process to have similar viewing and illumination conditions. Very minor gaps in the coverage were filled with a few images from cycle #2. Data Processing: The first step of the processing chain towards the cartographic products is to ortho-rectify the images to the proper scale and map projec-tion type. This process requires detailed information of the Dawn orbit and attitude data and of the topography of the targets. Both, improved orientation and a high-resolution shape model, are provided by stereo processing (bundle block adjustment) of the HAMO stereo image dataset [3]. Ceres's HAMO shape model was used for the calculation of the ray intersection points while the map projection itself was done onto the reference sphere of Ceres with a radius of 470 km. The final step is the controlled mosaicking) of all images to a global mosaic of Ceres, the so-called basemap. Ceres map tiles: The Ceres atlas was produced in a scale of 1:750,000 and consists of 15 tiles that conform to the quadrangle scheme proposed by Greeley and Batson [4]. A map scale of 1:750,000 guarantees a mapping at the highest available Dawn resolution in HAMO. The individual tiles were extracted from the global mosaic and reprojected. Nomenclature: The Dawn team proposed 81 names for geological features. By international agreement, craters must be named after gods and goddesses of agriculture and vegetation from world mythology, whereas other geological features must be named after agricultural festivals of the world. The nomenclature proposed by the Dawn team was approved by the IAU [http://planetarynames.wr.usgs.gov/] and is shown in Fig. 1. The entire Ceres HAMO atlas will be available to the public through the Dawn GIS web page [http://dawngis.dlr.de/atlas]. References: [1] Russell, C.T. and Raymond, C.A., Space Sci. Rev., 163, DOI 10.1007/s11214-011-9836-2; [2] Sierks, et al., 2011, Space Sci. Rev., 163, DOI 10.1007/s11214-011-9745-4; [3] Preusker, F. et al., this session; [4] Greeley, R. and Batson, G., 1990, Planetary Mapping, Cambridge University Press.

The C-terminal domain of the betaine carrier BetP of Corynebacterium glutamicum is directly involved in sensing K+ as an osmotic stimulus.

PubMed

Schiller, Dirk; Rübenhagen, René; Krämer, Reinhard; Morbach, Susanne

2004-05-18

The glycine betaine carrier BetP of Corynebacterium glutamicum was recently shown to function both as an osmosensor and as an osmoregulator in proteoliposomes by sensing changes in the internal K(+) concentration as a measure of hyperosmotic stress. In vivo analysis of mutants carrying deletions at the C-terminal extension of BetP indicated that this domain participates in osmostress-dependent activity regulation. To address the question, whether a putative K(+) sensor is located within the C-terminal domain, several mutants with truncations in this domain were purified and reconstituted in proteoliposomes of Escherichia coli phospholipids, since this in vitro system allowed variation of the K(+) concentration at the lumenal side. Truncation of 12 amino acids led to a partly deregulated BetP in terms of osmoregulation; however, K(+) sensitivity was not impaired in this mutant. The deletion of 25 amino acid residues at the C-terminal end of BetP led to both deregulation of the carrier activity, i.e., high activity independent of external osmolality, and loss of K(+)-dependent transport stimulation, indicating that this region of the C-terminal domain is necessary for K(+) sensing and/or K(+)-dependent carrier activation. Immunological and proteolysis analyses showed that BetP and its recombinant forms were reconstituted in a right-side-out orientation, i.e., the C-terminal domain faces the lumen of the proteoliposomes and is thus able to detect the K(+) signal at the inside. This is the first experimental demonstration of a direct connection between an osmotic stimulus, i.e., the change in internal K(+), and a putative sensor domain.

Topology of subunits of the mammalian cytochrome c oxidase: Relationship to the assembly of the enzyme complex

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

Yu-Zhong Zhang; Ewart, G.; Capaldi, R.A.

The arrangement of three subunits of beef heart cytochrome c oxidase, subunits Va, VIa, and VIII, has been explored by chemical labeling and protease digestion studies. Subunit Va is an extrinsic protein located on the C side of the mitochondrial inner membrane. This subunit was found to label with N-(4-azido-2-nitrophenyl)-2-aminoethane({sup 35}S)sulfonate and sodium methyl 4-({sup 3}H)formylphenyl phosphate in reconstituted vesicles in which 90% of cytochrome c oxidase complexes were oriented with the C domain outermost. Subunit VIa was cleaved by trypsin both in these reconstituted vesicles and in submitochondrial particles, indicating a transmembrane orientation. The epitope for a monoclonal antibodymore » (mAb) to subunit VIa was lost or destroyed when cleavage occurred in reconstituted vesicles. This epitope was localized to the C-terminal part of the subunit by antibody binding to a fusion protein consisting of glutathione S-transferase (G-ST) and the C-terminal amino acids 55-85 of subunit VIa. No antibody binding was obtained with a fusion protein containing G-ST and the N-terminal amino acids 1-55. The mAb reaction orients subunit VIa with its C-terminus in the C-domain. Subunit VIII was cleaved by trypsin in submitochondrial particles but not in reconstituted vesicles. N-Terminal sequencing of the subunit VIII cleavage produce from submitochondrial particles gave the same sequence as the untreated subunit, i.e., ITA, indicating that it is the C-terminus which is cleaved from the M side. Subunits Va and VIII each contain N-terminal extensions or leader sequences in the precursor polypeptides; subunit VIa is made without an N-terminal extension.« less

Chapter 12: Daily Patterns of Marbled Murrelet Activity at Inland Sites

Treesearch

Nancy L. Naslund; Brian P. O’Donnell

1995-01-01

Patterns in the daily activity of Marbled Murrelets (Brachyramphus marmoratus) at inland sites has been studied throughout their range from California to Alaska. Murrelets are most active at inland sites around dawn, and to a lesser degree, at dusk. Throughout their range, peak levels of activity (detections) occur in the hour around dawn, but...

Dawn Survey Orbit Image 21

NASA Image and Video Library

2015-07-07

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 17, 2015. A bright area called "Spot 1" can be seen in this image. http://photojournal.jpl.nasa.gov/catalog/PIA19589

Dawn Survey Orbit Image 14

NASA Image and Video Library

2015-06-25

This image, taken by NASA's Dawn spacecraft, shows dwarf planet Ceres from an altitude of 2,700 miles (4,400 kilometers). The image, with a resolution of 1,400 feet (410 meters) per pixel, was taken on June 9, 2015. The bright feature in the upper-left is also seen in PIA19581. http://photojournal.jpl.nasa.gov/catalog/PIA19582

Sherry Red Owl, Stands at Dawn Woman

ERIC Educational Resources Information Center

Crazy Bull, Cheryl

2014-01-01

This article introduces Sherry Red Owl, also known as "Stands at Dawn Woman," because she greets each day as a new opportunity and has spent her life working at new things. She worked at Sinte Gleska University (SGU) during its founding years, taught at an elementary school when few Native teachers were employed in the school systems,…

77 FR 8943 - Culturally Significant Objects Imported for Exhibition Determinations: “The Dawn of Egyptian Art”

Federal Register 2010, 2011, 2012, 2013, 2014

2012-02-15

... Determinations: ``The Dawn of Egyptian Art'' SUMMARY: Notice is hereby given of the following determinations... Egyptian Art,'' imported from abroad for temporary exhibition within the United States, are of cultural... of Art, New York, NY from on or about April 2, 2012, until on or about August 5, 2012, and at...

The Dawn Gravity Investigation at Vesta and Ceres

NASA Technical Reports Server (NTRS)

Konopliv, A. S.; Asmar, S.W.; Bills, B. G.; Mastrodemos, N.; Park, R. S.; Raymond, C. A.; Smith, D. E.; Zuber, M. T.

2011-01-01

The objective of the Dawn gravity investigation is to use high precision X-band Doppler tracking and landmark tracking from optical images to measure the gravity fields of Vesta and Ceres to a half-wavelength surface resolution better than 90-km and 300-km, respectively. Depending on the Doppler tracking assumptions, the gravity field will be determined to somewhere between harmonic degrees 15 and 25 for Vesta and about degree 10 for Ceres. The gravity fields together with shape models determined from Dawn's framing camera constrain models of the interior from the core to the crust. The gravity field is determined jointly with the spin pole location. The second degree harmonics together with assumptions on obliquity or hydrostatic equilibrium may determine the moments of inertia.

KSC-07pd2066

NASA Image and Video Library

2007-07-22

KENNEDY SPACE CENTER, FLA. — At the Astrotech payload processing facility, workers guide the movement of the upper canister being lifted from the Dawn spacecraft, seen encased in a protective cover. Dawn was returned from Launch Pad 17-B at Cape Canaveral Air Force Station to Astrotech to await a new launch date. The launch opportunity extends from Sept. 7 to Oct. 15. Dawn is the ninth mission in NASA's Discovery Program. The spacecraft will be the first to orbit two planetary bodies, asteroid Vesta and dwarf planet Ceres, during a single mission. Vesta and Ceres lie in the asteroid belt between Mars and Jupiter. It is also NASA’s first purely scientific mission powered by three solar electric ion propulsion engines. NASA/Charisse Nahser

KSC-07pd1591

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians begin placing the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

KSC-07pd1592

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians begin securing the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

KSC-07pd1593

NASA Image and Video Library

2007-06-19

KENNEDY SPACE CENTER, FLA. -- At Astrotech, technicians are securing the sun shade over the high gain antenna on the Dawn spacecraft. Made of germanium kapton, the shade, which is RF transparent, is placed over the sensitive antenna to reflect and emit harmful solar radiation to prevent the antenna from being excessively heated. Dawn is scheduled to launch July 7 from Pad 17-B on Cape Canaveral Air Force Station. Dawn's goal is to characterize the conditions and processes of the solar system's earliest epoch by investigating in detail the largest protoplanets that have remained intact since their formations: asteroid Vesta and the dwarf planet Ceres. They reside in the extensive zone between Mars and Jupiter together with many other smaller bodies, called the asteroid belt. Photo credit: NASA/George Shelton

Origin of Dark Material on VESTA from DAWN FC Data: Remnant Carbonaceous Chondrite Impators

NASA Technical Reports Server (NTRS)

Reddy, V.; LeCorre, L.; Nathues, A.; Mittlefehldt, David W.; Cloutis, E. A.; OBrien, D. P.; Durda, D. D.; Bottke, W. F.; Buczkowski, D.; Scully, J. E. C.;

Clues to Ceres' Internal Structure

NASA Image and Video Library

2017-10-26

This frame from an animation shows Ceres as seen by NASA's Dawn spacecraft from its high-altitude mapping orbit at 913 miles (1,470 kilometers) above the surface. The colorful map overlaid at right shows variations in Ceres' gravity field measured by Dawn, and gives scientists hints about the dwarf planet's internal structure. Red colors indicate more positive values, corresponding to a stronger gravitational pull than expected, compared to scientists' pre-Dawn model of Ceres' internal structure; blue colors indicate more negative values, corresponding to a weaker gravitational pull. The animation was created by projecting a map of Ceres onto a rotating sphere. The image scale is about 450 feet (140 meters) per pixel. The animations are available at https://photojournal.jpl.nasa.gov/catalog/PIA22083

Ionospheric control of the dawn-dusk asymmetry of the Mars magnetotail current sheet

NASA Astrophysics Data System (ADS)

Liemohn, Michael W.; Xu, Shaosui; Dong, Chuanfei; Bougher, Stephen W.; Johnson, Blake C.; Ilie, Raluca; De Zeeuw, Darren L.

2017-06-01

This study investigates the role of solar EUV intensity at controlling the location of the Mars magnetotail current sheet and the structure of the lobes. Four simulation results are examined from a multifluid magnetohydrodynamic model. The solar wind and interplanetary magnetic field (IMF) conditions are held constant, and the Mars crustal field sources are omitted from the simulation configuration. This isolates the influence of solar EUV. It is found that solar maximum conditions, regardless of season, result in a Venus-like tail configuration with the current sheet shifted to the -Y (dawnside) direction. Solar minimum conditions result in a flipped tail configuration with the current sheet shifted to the +Y (duskside) direction. The lobes follow this pattern, with the current sheet shifting away from the larger lobe with the higher magnetic field magnitude. The physical process responsible for this solar EUV control of the magnetotail is the magnetization of the dayside ionosphere. During solar maximum, the ionosphere is relatively strong and the draped IMF field lines quickly slip past Mars. At solar minimum, the weaker ionosphere allows the draped IMF to move closer to the planet. These lower altitudes of the closest approach of the field line to Mars greatly hinder the day-to-night flow of magnetic flux. This results in a buildup of magnetic flux in the dawnside lobe as the S-shaped topology on that side of the magnetosheath extends farther downtail. The study demonstrates that the Mars dayside ionosphere exerts significant control over the nightside induced magnetosphere of that planet.