Optically Thick Outflows of Supercritical Accretion Discs: Radiative Diffusion Approach

Abstract

Highly supercritical accretion discs are probable sources of dense optically thick axisymmetric winds. We introduce a new approach based on diffusion approximation radiative transfer in a funnel geometry and obtain an analytical solution for the energy density distribution inside the wind assuming that all the mass, momentum and energy are injected well inside the spherization radius. This allows to derive the spectrum of emergent emission for various inclination angles. We show that self-irradiation effects play an important role altering the temperature of the outcoming radiation by about 20% and the apparent X-ray luminosity by a factor of 2-3. The model has been successfully applied to two ULXs. The basic properties of the high ionization HII-regions found around some ULXs are also easily reproduced in our assumptions.

32 pages, 9 figures, 1 table; accepted to PASJ

References in corpus (10)

• Super-critically accreting stellar-mass black holes as ultraluminous X-ray sources
• XMM-Newton observations of the brightest Ultraluminous X-ray sources
• X-ray observations of ultraluminous X-ray sources
• A 62 Day X-Ray Periodicity and an X-Ray Flare from the Ultraluminous X-Ray Source in M82
• On the weakness of disc models in bright ULXs
• Spectroscopy of Optical Counterparts of Ultraluminous X-ray Sources
• Spectroscopic binaries with components of similar mass
• Do Ultraluminous X-ray Sources Really Contain Intermediate-mass Black Holes?
• Optical Spectroscopy of the ULX-Associated Nebula MF16
• Spectral energy distribution of super-Eddington flows

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• Spitzer Observations of MF 16 Nebula and the associated Ultraluminous X-ray Source
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