Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p23c1729g&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P23C-1729
Mathematics
Logic
[5410] Planetary Sciences: Solid Surface Planets / Composition, [5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties
Scientific paper
The NASA Galileo spacecraft observed asteroid 951 Gaspra on October 29, 1991 with the Near Infrared Mapping Spectrometer (NIMS) at wavelengths ranging from 0.7 - 5.2 micrometers [Carlson et al., 1992]. Work is being conducted to produce a radiance calibrated spectral image of a 17 channel, 1.3 km per pixel NIMS observation of 951 Gaspra for the NASA Planetary Data System (PDS). Analysis [Granahan, 2011] of this S asteroid data has yielded a detection of a 2.7 micrometer absorption feature in all of the observed surface pixels of this data set. Also measured [Granahan, 2011] were groups of spectra that possessed different band centers near 1.0 micrometers and band depths at 2.0 micrometers due to the minerals olivine and pyroxene. The 2.7 micrometer absorption feature has its strongest absorption within Yeates Regio. Yeates Regio is one of 951 Gaspra's basins [Veverka et al., 1994]. The absorption is weakest in the vicinity of the asteroid's ridges. A material that has an absorption at 2.7 micrometers is structural hydroxyl (OH). The carbonaceous chondrite meteorite Murchison contains structural hydroxyl that creates such a spectral feature [Rivkin et al., 2002]. It has also been observed in the spectra of montmorrilonite [McAdam and Hibbitts, 2011]. Updated measurements of olivine and pyroxene spectral bands were also conducted for this radiance data of 951 Gaspra. Two groups of spectra were observed to be differentiated by spectral band centers measured at 0.99 and 1.05 micrometers with corresponding differences of band depth around 2.0 micrometers. The 0.99 micrometer group of spectra possesses the larger 2.0 micrometer band depth. These families of spectra correspond to those of SI (1.05 micrometer group) and SIII (0.99 micrometer group) classes [Gaffey et al., 1993] of the S asteroids. They are distinct from ordinary chondrite meteorites and imply the occurrence of differentiation on 951 Gaspra. This 17 channel radiance spectral image is being packaged as a FITS (Flexible Image Transport System) format [Pence et al., 2010] with a detached PDS label file for storage in the Small Bodies Node of the NASA PDS system. The file can be read into software packages that include the routines in "The IDL Astronomy User's Library" of NASA Goddard Space Flight Center and the U.S. Geological Survey's Integrated Software for Imagers and Spectrometers (ISIS) 3 system. Carlson, R. W., et al.,(1992),Bulletin of the American Astronomical Society, 24, 932. Gaffey, M. J., et al., (1993) Icarus, 106, 573-602. Granahan, J. C. (2011) Icarus, 213, 265-272. McAdam, M. M., and C. A. Hibbitts (2011) 42nd Lunar and Planetary Science Conference, #1026. Pence, W. D., et al., (2010) Astronomy and Astrophysics, 524(A42), 1-40. Rivkin, A. S., et al., (2002) Asteroids III, pp. 235-253, University of Arizona Press, Tucson. Veverka, J., et al., (1994) Icarus, 107, 2-17.
No associations
LandOfFree
A 2.7 Micrometer Feature and Other Spectral Signatures of Asteroid 951 Gaspra does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with A 2.7 Micrometer Feature and Other Spectral Signatures of Asteroid 951 Gaspra, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A 2.7 Micrometer Feature and Other Spectral Signatures of Asteroid 951 Gaspra will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-869865