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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20131126T123000
DTEND;TZID=Atlantic/Canary:20131126T133000
UID:iactalks-565
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/565
CREATED:2013-11-26T12:30:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Dusty supernovae running the thermodynamics of the matter reinserte
 d by young stellar clusters 
DESCRIPTION:Dusty supernovae running the thermodynamics of the matter reins
 erted by young stellar clusters \nDr. Guillermo Tenorio Tagle\n\nFollowing
  the observational and theoretical evidence that points at core  collapse 
 supernovae as major producers of dust, we calculate the  hydrodynamics of 
 the matter reinserted within young and massive super  stellar clusters und
 er the assumption of gas and dust radiative cooling.  The large supernova 
 rate expected in massive clusters allows for a  continuous replenishment o
 f dust immersed in the high temperature  thermalized reinserted matter and
  warrants a stationary presence of dust  within the cluster volume during 
 the type II supernova era (~ 3 Myr -  40 Myr). Such a balance determines t
 he range of dust to gas mass ratio  and this the dust cooling law. We then
  search for the critical line in  the cluster mechanical luminosity (or cl
 uster mass) vs cluster size,  that separates quasi- adiabatic and strongly
  radiative cluster wind  solutions from the bimodal cases. In the latter, 
 strong radiative  cooling reduces considerably the cluster wind mechanical
  energy output  and affects particularly the cluster central regions, lead
 ing to  frequent thermal instabilities that diminish the pressure and inhi
 bit  the exit of the reinserted matter. Instead matter accumulates there a
 nd  is expected to eventually lead to gravitational instabilities and to  
 further stellar formation with the matter reinserted by former massive  st
 ars. The main outcome of the calculations is that the critical line is  al
 most two orders of magnitude or more, depending on the assumed value  of V
 \infty, lower than when only gas radiative cooling is applied. And  thus, 
 massive clusters (M_sc > 10^5 Msun) are predicted to enter the  bimodal
  regime.
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