Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign

Details Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007icar..190..391l&link_type=abstract

Icarus, Volume 190, Issue 2, p. 391-405.

Astronomy and Astrophysics

Astrophysics

5

Scientific paper

We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ˜295 ks between 30th June and 24th July 2005, and continuously for ˜64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329 1347] 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 event was small, ˜20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×10 kg (˜10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, 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 gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, 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, with intermittent impulsive events due to solar flares and coronal mass ejections.

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