The evolution of the optically thick accretion disk in nova muscae

Ranjeev Misra, Fulvio Melia

Research output: Contribution to journalArticle

3 Citations (Scopus)

Abstract

We here model the soft X-ray flux from the black hole X-ray nova, GS 1124-68 (Nova Muscae, GRS 1124-68) as emission from an optically thick accretion disk with Comptonization. Our results suggest that the disk's inner edge has a radius the dependence of which on the accretion rate is a power law, and that the slope of this function changes between the different spectral states. This disk configuration retains a hot inner region, which can account for the hard X-rays, although its structure appears to be different during the soft and ultra-soft states.

Original languageEnglish (US)
Pages (from-to)848-854
Number of pages7
JournalAstrophysical Journal
Volume484
Issue number2
DOIs
StatePublished - 1997
Externally publishedYes

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accretion disks
accretion
x rays
power law
slopes
radii
configurations
rate

Keywords

  • Accretion, accretion disks
  • Black hole physics
  • Novae, cataclysmic variables radiation mechanisms: Thermal
  • X-rays: Stars

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

The evolution of the optically thick accretion disk in nova muscae. / Misra, Ranjeev; Melia, Fulvio.

In: Astrophysical Journal, Vol. 484, No. 2, 1997, p. 848-854.

Research output: Contribution to journalArticle

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