Hot Gas Evolution in Nearly Normal Elliptical Galaxies

The dynamic evolution of the hot gaseous component of nearly normal elliptical galaxies is considered, reviewing the results of recent numerical simulations modeling data from X-ray observations. The governing equations employed are introduced; two model galaxies are simulated at two different supernova rates; and further computations are performed to estimate the effects of a dark halo, thermal conductivity, and chemical abundances on the gas flow. The results are presented in graphs and characterized in detail. It is shown that a significant amount of dark matter is required to explain the observed soft X-ray emission.