SQCX X-ray Observations Of The Deep Impact Spacecraft Close Encounters With Comets 9P/Tempel 1 And 103P/Hartley 2

Details SQCX X-ray Observations Of The Deep Impact Spacecraft Close Encounters With Comets 9P/Tempel 1 And 103P/Hartley 2 SQCX X-ray Observations Of The Deep Impact Spacecraft Close Encounters With Comets 9P/Tempel 1 And 103P/Hartley 2

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1714l&link_type=abstract

American Astronomical Society, HEAD meeting #11, #17.14; Bulletin of the American Astronomical Society, Vol. 41, p.685

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We present results from the extensive Chandra, SWIFT, Spitzer, and groundbased observing campaigns studying Comet 9P/Tempel 1 in support of NASA's Deep Impact (DI) mission as an indication of the results expected for the next DI flyby of comet 103P/Hartley 2 at 0.1 AU geocentric distance in November 2010. 9P/Tempel 1 was observed for 300 ksec between 30th June and 24th July 2005, and continuously for 60 ksec on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin, cold wind comet 2P/Encke system (Lisse et al. 2005) was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in x-ray flux due to the Deep Impact excavation was small, 20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5 x 106 kg ( 10 hrs of normal coma outflow). Over time, other temporally variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Good agreement between the Chandra and SWIFT x-ray photometry was found. Two flares, much stronger than the man-made increase due to Deep Impact, were found in the observed x-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed Spitzer gas production rates and ACE solar wind ion fluxes with a SWCX mechanism for the emission was found to be consistent with the temporal- and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma.

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