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On May 23, 2006 we used the ACIS-S instrument on the Chandra X-rayObservatory (CXO) to study the X-ray emission from the B fragment of comet73P/2006 (Schwassmann-Wachmann 3) (73P/B). We obtained a total of 20 ks of CXOobservation time of Fragment B, and also investigated contemporaneous ACE andSOHO solar wind physical data. The CXO data allow us to spatially resolve thedetailed structure of the interaction zone between the solar wind and thefragment's coma at a resolution of ~ 1,000 km, and to observe the X-rayemission due to multiple comet--like bodies. We detect a change in the spectralsignature with the ratio of the CV/OVII line increasing with increasingcollisional opacity as predicted by Bodewits \e (2007). The line fluxes arisefrom a combination of solar wind speed, the species that populate the wind andthe gas density of the comet. We are able to understand some of the observedX-ray morphology in terms of non-gravitational forces that act upon an activelyoutgassing comet's debris field. We have used the results of the Chandraobservations on the highly fragmented 73P/B debris field to re-analyze andinterpret the mysterious emission seen from comet C/1999 S4 (LINEAR) on August1st, 2000, after the comet had completely disrupted. We find the physicalsituations to be similar in both cases, with extended X-ray emission due tomultiple, small outgassing bodies in the field of view. Nevertheless, the twocomets interacted with completely different solar winds, resulting indistinctly different spectra.

Chandra's Close Encounter with the Disintegrating Comets 73P/2006 (Schwassmann--Wachmann--3) Fragment B and C/1999 S4 (LINEAR)