Mass Loss from Stars Into Cooling Flow Ellipticals

Details Mass Loss from Stars Into Cooling Flow Ellipticals Mass Loss from Stars Into Cooling Flow Ellipticals

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21344308b&link_type=abstract

American Astronomical Society, AAS Meeting #213, #443.08; Bulletin of the American Astronomical Society, Vol. 41, p.325

Astronomy and Astrophysics

Astronomy

Scientific paper

Early-type galaxies possess a dilute hot gas (2-10E6 K) that is probably the thermalized ejecta of the mass loss from evolving stars. To study the processes by which the mass loss from orbiting stars interacts with the hot ambient gas, we use numerical hydrodynamic simulations. For the cases of red giant mass loss, a bow shock develops upstream and most of the ejecta is pushed into a wake that interacts with the hot ambient medium through shocks and fluid instabilities. Most of the ejecta is heated to nearly the ambient temperature, with about 20% remaining cool. For the planetary nebula case, radiative losses are more effective and a significantly larger fraction of the ejecta remains cool when it exits the grid. This cool gas may be responsible for some of the optical and ultraviolet emission lines seen in early-type galaxies.

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