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SUMMARY:Supernova Dust - Mike Barlow\, University College London
DTSTART:20171026T150000Z
DTEND:20171026T160000Z
UID:TALK93565@talks.cam.ac.uk
CONTACT:Simon Hodgkin
DESCRIPTION:Until the advent in the late 1990’s of sensitive submillimet
 re arrays such as SCUBA\, it was generally believed that the main sources 
 of the interstellar dust found in galaxies were dusty outflows from evolve
 d AGB stars and M supergiants\, although a dust contribution from supernov
 ae had long been predicted on theoretical grounds. The detection at submil
 limetre wavelengths of very large dust masses in some high redshift galaxi
 es emitting less than a billion years after the Big Bang led to a more ser
 ious consideration of core-collapse supernovae (CCSNe) from massive stars 
 as major dust contributors. But it was not until the Herschel mission and 
 subsequent high angular resolution ALMA observations that direct evidence 
 was obtained for the presence of significantly large masses of newly forme
 d dust in some young CCSN remnants. The presence of dust in CCSN ejecta ca
 n also be diagnosed and quantified from red-blue asymmetries in their late
 -time optical emission line profiles. I will describe the current results 
 from these methods for estimating the masses of dust that have formed in s
 upernova ejecta\, and their implications.
LOCATION:Sackler Lecture Theatre\, IoA (tea at 3:30 pm)
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