Near-Infrared Spectroscopy and Imaging of the 2009 Jupiter impact debris field: Constraints on particle composition, size and vertical distribution

Details Near-Infrared Spectroscopy and Imaging of the 2009 Jupiter impact debris field: Constraints on particle composition, size and vertical distribution Near-Infrared Spectroscopy and Imaging of the 2009 Jupiter impact debris field: Constraints on particle composition, size and vertical distribution

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p31a1228y&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P31A-1228

Physics

[0300] Atmospheric Composition And Structure, [6220] Planetary Sciences: Solar System Objects / Jupiter

Scientific paper

We present results of near-infrared imaging and spectroscopy of the 2009 Jupiter impact site and its associated debris field during the time period from 20 July 2009 (approximately 20 hours after impact) to 31 August 2009 (nearly six weeks post-impact). Our data were acquired with NASA/InfraRed Telescope Facility (IRTF) facility instruments, SpeX, 1- to 5-micron spectrometer and its guide camera, and NSFCam2, 1- to 5-micron multi-spectral camera. On 20 July, the impact site appeared as a localized region, close to and brighter than Jupiter's south polar haze. The impact site then expanded longitudinally in both directions. Nearly five weeks later, the debris field continues to spread, characterized by a few localized structures or cores near the original impact longitude, surrounded by material which is extended by about 7 degrees in latitude and 80 degrees in longitude. Early multi-spectral images and spectra of the debris identify ammonia as a constituent. Spectra and images of the debris material in subsequent weeks, redistributed by the zonal and meridional wind field of Jupiter, indicates the debris continues to be very prominent at 2 microns; comparable in reflectivity to the south polar haze and high in the atmosphere, implying small particles. The cores of the debris field were the only components of the neutral atmosphere detectable in the strong methane-absorbing 3.2- to 3.4-micron region as late as 6 August, but they were no longer detectable as of 18 August. In the 2-micron region, the debris reflectivity also diminished with time, mostly likely as a result of downward sedimentation. Our results will be compared to the those from SL9 fragment impacts and the "undisturbed" Jovian atmosphere, constraining the vertical distribution of the perturbation, composition and particle sizes of the debris.

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