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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20141029T123000
DTEND;TZID=Atlantic/Canary:20141029T133000
UID:iactalks-687
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/687
CREATED:2014-10-29T12:30:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY: Simulations of Galaxy Formation: Feedback and the early formation 
 of compact spheroids by disc instabilities.
DESCRIPTION: Simulations of Galaxy Formation: Feedback and the early format
 ion of compact spheroids by disc instabilities.\nDr. Daniel Ceverino\n\nAn
 y successful model of galaxy formation needs to explain the low rate  of s
 tar formation in the small progenitors of today’s galaxies. This  in
 efficiency is necessary for reproducing the low stellar-to-virial mass  fr
 actions. A possible driver of this low efficiency is the radiation  pressu
 re exerted by ionizing photons from massive stars. The effect of  radiatio
 n pressure in cosmological, zoom-in galaxy formation simulations  is model
 led as a non-thermal pressure that acts only in dense and  optically thick
  star-forming regions.  The main effect of radiation  pressure is to regul
 ate and limit the high values of gas density and the  amount of gas availa
 ble for star formation. By using these simulations,  I will address the ea
 rly formation of compact spheroids by violent disc  instabilities (VDI). D
 ue to the inefficiency of star formation, this  process is gas rich, so th
 e dissipation naturally leads to compact  spheroids. These VDI-driven sphe
 roids, much like merger-driven  spheroids, have steep surface density prof
 iles, consistent with a  classical, de-Vaucouleurs profile at all times.
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