Other
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111102b&link_type=abstract
American Astronomical Society, AAS Meeting #211, #111.02; Bulletin of the American Astronomical Society, Vol. 39, p.940
Other
Scientific paper
The gas accretion histories for simulated disk galaxies spanning two orders of magnitude in mass (3.4x1010 to 3.3x1012 M&sun;) are investigated. We confirm previous findings that the standard model, in which gas is shock heated to the virial temperature of the galaxy when accreted, requires significant modification. In our simulations, no gas entering galaxies with masses below 1011 M&sun; is shock heated at the virial radius, while a mixture of shocked and unshocked gas enters the galaxy above this mass. For galaxies more massive than the Milky Way, a strong shock develops, making it difficult for shocked gas to cool onto the disk. We examine the fraction of stellar disk mass that forms from (a) smoothly accreted, shock heated gas, (b) smoothly accreted, unshocked gas (e.g., in filaments), and (c) "clumpy” accretion of gas from satellite galaxies. We find that for the whole range of masses, smoothly accreted gas (whether shocked or unshocked, but never in another galaxy) dominates. Higher mass galaxies merge with other galaxy halos that have a higher baryon-to-dark matter ratio, while low mass galaxies accrete "darker” halos with a lower baryon-to-dark matter ratio. This leads to a trend in which the fraction of gas accreted ("clumpy") from other galaxies increases with mass.
Brook Chris
Brooks Alyson
Governato Fabio
Quinn Terry
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