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SUMMARY:How galaxies form stars - Andrey Kravtsov (U Chicago)
DTSTART:20181004T150000Z
DTEND:20181004T160000Z
UID:TALK111697@talks.cam.ac.uk
CONTACT:28811
DESCRIPTION:Formation of stars in galaxies is a complex multi-scale proces
 s. One of the big puzzles about star formation was that observations show 
 that galaxies convert their gas (molecular and atomic) into stars on a tim
 e scale of ~5-10 Gyrs\, which is much longer than time scales of any relev
 ant processes in the ISM and is also considerably longer than the correspo
 nding conversion time scale in star-forming molecular clouds.\n\nIn additi
 on\, observations over the past decade showed that star formation rate in 
 observed regular (non-star burst) galaxies scales almost linearly with *mo
 lecular* gas mass\, with the coefficient of proportionality\, the depletio
 n time = M_H2/SFR of about 2 Gyrs with a relatively small scatter\, even t
 hough scatter is large on the scale of star forming clouds.\n\nMany galaxy
  formation simulations could reproduce the observed value of depletion tim
 e\, but the physics controlling it\, its dependence on assumptions made ab
 out star formation\, and the slope of the relation was not understood. I w
 ill present results of a suite of simulations that we used to explore this
  behavior systematically and a simple physical model that explains the phy
 sics behind both the observed long gas depletion times in galaxies and the
  linear relation between molecular gas mass and star formation rate.\n
LOCATION:Sackler Lecture Theatre\, IoA (tea at 3:30 pm)
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