The evolution of the optically thick accretion disk in nova muscae

Ranjeev Misra; Fulvio Melia

doi:10.1086/304384

The evolution of the optically thick accretion disk in nova muscae

Ranjeev Misra, Fulvio Melia

Research output: Contribution to journal › Article › peer-review

3 Scopus citations

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 language	English (US)
Pages (from-to)	848-854
Number of pages	7
Journal	Astrophysical Journal
Volume	484
Issue number	2
DOIs	https://doi.org/10.1086/304384
State	Published - 1997
Externally published	Yes

Keywords

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

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/304384

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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.",

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author = "Ranjeev Misra and Fulvio Melia",

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AU - Melia, Fulvio

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N2 - 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.

AB - 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.

KW - Accretion, accretion disks

KW - Black hole physics

KW - Novae, cataclysmic variables radiation mechanisms: Thermal

KW - X-rays: Stars

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JF - Astrophysical Journal

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The evolution of the optically thick accretion disk in nova muscae

Abstract

Keywords

ASJC Scopus subject areas

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