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SUMMARY:Extracting physical parameters of SMBH accretion by modeling the X
 _ray spectra of TDE.
DTSTART;VALUE=DATE-TIME:20230629T103000Z
DTEND;VALUE=DATE-TIME:20230629T104500Z
DTSTAMP;VALUE=DATE-TIME:20260610T063429Z
UID:indico-contribution-826@cern.ch
DESCRIPTION:Speakers: Richard Saxton (Telespazio for ESA\, ESAC\, Madrid\,
  Spain)\nThe disruption and subsequent accretion of a star by a super-mass
 ive black hole (SMBH) provides an excellent laboratory to study a broad ra
 nge of accretion conditions over timescales as short as months or a few ye
 ars. We show how a physical model of a relativistic thin accretion disc\, 
 applied to the X-ray spectra of a sample of 19 tidal disruption events (TD
 E) in the high-accretion thermal phase\, can yield the black hole mass and
  inner radius of the disc. From this study we offer a possible solution fo
 r the problem of low apparent total mass accretion in TDE systems and perf
 orm a sanity check on the hypothesis that the peak optical/UV emission in 
 TDEs is due to the reprocessing of X-ray radiation. \n\nWhen the accretion
  rate in a TDE drops well below the Eddington limit\, the spectrum is comm
 only observed to develop a hard X-ray tail\, believed to be due to the Com
 pton up-scattering of disc photons by a warm electron cloud. We show that 
 \nthis component develops very rapidly in at least one source and use this
  to constrain the mechanism responsible for the creation of the Comptonisa
 tion zone.\nFinally we present new data on a further interesting extra-gal
 actic\, hard X-ray transient\, providing strong support that it was also c
 aused by a TDE.\n\nhttps://indico.unina.it/event/61/contributions/826/
LOCATION:Centro Congressi Federico II Aula Magna
URL:https://indico.unina.it/event/61/contributions/826/
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