[Previous] | [Session 122] | [Next]
J.C. Raymond, A. Baldi, G. Fabbiano, A. Zezas (CfA), F. Schweizer (STScI), T.J. Ponman, A.M. Read (U. Birmingham), A.R. King (U. Leicester)
We use the parameters of the diffuse X-ray emitting gas in the Antennae derived from Chandra observations by Baldi et al. to examine the heating and cooling rates of the plasma. We consider radiative cooling, thermal conduction and adiabatic expansion, and we compare with published values of magnetic field strength and H I column density. We find that the observed elemental composition enhancements are consistent with the enrichment expected for Type II supernovae that heat the gas. We also find that static models that emphasize the role of thermal conduction cannot be scaled to the conditions in the Antennae. This work was supported by NASA contract NAS8-39073 (CXC) to the Smithsonian Institution.
[Previous] | [Session 122] | [Next]
Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.