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SUMMARY:On the evolution of the disk and corona in accreting black hole bi
 naries - Javier Garcia\, Caltech
DTSTART:20190710T121500Z
DTEND:20190710T124500Z
UID:TALK127333@talks.cam.ac.uk
CONTACT:Dr George Lansbury
DESCRIPTION:During an outburst\, accreting black hole binaries (BHB) cycle
  between quiescence to their Eddington luminosity exhibiting a rich phenom
 enology that includes thermal and non-thermal X-ray emission\, ionized ref
 lection\, relativistic jets\, quasi-periodic oscillations\, and disk winds
 . The current paradigm dictates that the accretion disk is highly truncate
 d during the jet-dominated hard state\, while in the soft state the jet is
  quenched and the inner-disk is stable at the inner-most circular orbit (I
 SCO) radius. I will present recent spectroscopy analysis that contradicts 
 this picture. We have found evidence for strong X-ray reflection originate
 d very close to the black hole\, suggesting that the disk has reached the 
 ISCO radius at the early phases of the outburst\, while the non-thermal co
 ronal emission shows clear signs of evolution in both its electron tempera
 ture and optical depth. The implications of these observational findings a
 re discussed in the context of state transitions of several BHBs.
LOCATION:Sackler Lecture Theatre\, IoA
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