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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-2608
DTSTART:20120223T213000Z
DTEND:20120223T230000Z
DTSTAMP:20260416T110549Z
LAST-MODIFIED:20120213T174700Z
LOCATION:4421 Sterling Hall
SUMMARY:Star Formation\, gas loss\, and the molecular gas in simulatio
 ns of evolving galaxies\, Astronomy Colloquium\, Charlotte Christensen
 \, University of Arizona
DESCRIPTION:The physics of the interstellar media (ISM) affects both t
 he location of star formation and the efficiency of supernova feedback
  by changing the properties of the star forming gas. In most previous 
 galaxy formation simulations\, though\, the cold\, molecular phase of 
 the ISM has been neglected. In this talk\, I present a method for inte
 grating the non-equilibrium molecular hydrogen (H2) abundance througho
 ut a simulation\, including such processes as dissociation by Lyman-We
 rner radiation\, shielding of molecular gas\, and H2-based star format
 ion. I apply this model to high-resolution cosmological simulations of
  galaxies ranging from 10^9 to 10^12 solar masses and compare it to si
 mulations with different ISM models. I find that the inclusion of H2 r
 esults in galaxies with clumpier ISMs and more dispersed star formatio
 n. The increased clumpiness of the gas leads to greater efficiency of 
 supernova at removing of low-angular momentum material from the galaxy
 . The result is spiral galaxies with smaller bulges and more realistic
  rotation curve. I discuss how the these interaction between the ISM s
 tructure\, star formation\, and supernova feedback result in changes t
 o the mass distribution and compare the formation histories of galaxie
 s of different masses.
URL:https://www.physics.wisc.edu/events/?id=2608
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