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PRODID:-//Heidelberg University//HePhySTO//EN
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DTEND:20260526T153000Z
UID:b1b4ba8bb08acbf586ea3cea68f190c1@physik.uni-heidelberg.de
DTSTAMP:20260411T171216Z
LOCATION:
DESCRIPTION:Active galactic nuclei are mostly powered by inflow through acc
 retion disks onto central supermassive black holes.  Beyond a few times the
 ir Schwarzschild  radius\, gravitational instability in these disks leads t
 o self-regulated formation and evolution of massive stars which chemically 
 enrich their neighborhood along with stellar-mass black holes.  These compa
 ct remnants are captured by coexisting massive main sequence stars\, form c
 lose binaries\, readily merge\, and excite intense gravitational waves with
  potentially observable electromagnetic signatures.  The massive stars' mig
 ration\, with or without black hole cores\, efficiently transporting mass r
 egardless of the Eddington limit and promoting the rapid growth of supermas
 sive black holes in the early Universe.  Analogous physical processes are a
 lso relevant in the context of planet formation in protostellar disks.  The
 y account for the persistent super-solar metallicity\, especially in Nitrog
 en and iron\, inferred from broad emission lines of  high and low redshift 
 AGNs. To arrange a visit with the speaker during the visit\, please contact
  their host: Haochang Jiang <h-jiang@mpia.de>\n\nImported from https://www.
 physik.uni-heidelberg.de/hephysto/ (no warranty for accuracy).
URL;VALUE=URI:https://www.physik.uni-heidelberg.de/hephysto/index.php?s=tal
 k&id=12467
SUMMARY:Heidelberg Joint Astronomical Colloquium: Douglas Lin - Stellar evo
 lution & black hole coagulation in AGNs: an analogue of planet formation
DTSTART:20260526T143000Z
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