Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9718s&link_type=abstract
American Astronomical Society, AAS Meeting #211, #97.18; Bulletin of the American Astronomical Society, Vol. 39, p.906
Astronomy and Astrophysics
Astronomy
Scientific paper
Galaxy merger simulations have modeled the behavior of gas within a galactic disk, yet the dynamics of hot gas within a spiral galaxy halo has been neglected. We report the preliminary results of high resolution numerical simulations of dark matter halo mergers containing hot halo gas -- a component predicted to surround spiral galaxies and recently confirmed by X-ray detection in an isolated massive spiral galaxy (Pedersen et al., 2006). Our simulations have important implications for galaxy evolution, and may help explain the formation and enrichment of the Warm-Hot Intergalactic Medium. It is known that the majority of the baryons in the present-day Universe resides in a warm-hot intergalactic medium; however, the physical processes that cause them to escape from galaxies are not well understood. Usually, super-winds from massive stars and supernovae feedback are invoked to explain the gas loss but the derived star formation rates are not consistent with the data. Our preliminary results suggest that the bulk orbital kinetic energy from the merger gets converted into the kinetic energy of the gas; since the halo gas already has a high thermal pressure, this energy input easily liberates the gas. We find that the more gas is liberated from less massive galaxies.
Holley-Bockelmann Kelly
Sinha Manodeep
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