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Title: COMPTONIZED PHOTON SPECTRA OF SUPERCRITICAL BLACK HOLE ACCRETION FLOWS WITH APPLICATION TO ULTRALUMINOUS X-RAY SOURCES

Abstract

Radiation spectra of supercritical black hole accretion flows are computed using a Monte Carlo method by post-processing the results of axisymmetric radiation hydrodynamic simulations. We take into account thermal/bulk Comptonization, free-free absorption, and photon trapping. We found that a shock-heated region ({approx}10{sup 8} K) appears at the funnel wall near the black hole where the supersonic inflow is reflected by the centrifugal barrier of the potential. Both thermal and bulk Comptonization significantly harden photon spectra although most of the photons upscattered above 40 keV are swallowed by the black hole due to the photon trapping. When the accretion rate onto the black hole is M-dot Almost-Equal-To 200L{sub E}/c{sup 2}, where L{sub E} is the Eddington luminosity, the spectrum has a power-law component which extends up to {approx}10 keV by upscattering of photons in the shock-heated region. In higher mass accretion rates, the spectra roll over around 5 keV due to downscattering of the photons by cool electrons in the dense outflow surrounding the jet. Our results are consistent with the spectral features of ultraluminous X-ray sources, which typically show either a hard power-law component extending up to 10 keV or a rollover around 5 keV. We found that the spectrummore » of NGC 1313 X-2 is quite similar to the spectrum numerically obtained for high accretion rate (M-dot {approx} 1000L{sub E}/c{sup 2}) source observed with low viewing angle (i = 10 Degree-Sign -20 Degree-Sign ). Our numerical results also demonstrate that the face-on luminosity of supercritically accreting stellar mass black holes (10 M{sub Sun }) can significantly exceed 10{sup 40} erg s{sup -1}.« less

Authors:
;  [1];  [2]; ; ;  [3]
  1. Department of Physics, Graduate School of Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522 (Japan)
  2. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka-shi, Tokyo 181-8588 (Japan)
  3. Department of Astronomy, Kyoto University, Kitashirakawa, Sakyo-ku, Kyoto 606-8502 (Japan)
Publication Date:
OSTI Identifier:
22037111
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 752; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; ACCRETION DISKS; ASTRONOMY; ASTROPHYSICS; AXIAL SYMMETRY; BLACK HOLES; CARBON MONOXIDE; COMPUTERIZED SIMULATION; COSMIC ELECTRONS; COSMIC PHOTONS; EMISSION SPECTRA; HYDRODYNAMICS; JETS; KEV RANGE; LUMINOSITY; MASS; MONTE CARLO METHOD; RADIANT HEAT TRANSFER; TRAPPING

Citation Formats

Kawashima, T., Matsumoto, R., Ohsuga, K., Mineshige, S., Yoshida, T., and Heinzeller, D., E-mail: kawashima-t@astro.s.chiba-u.ac.jp. COMPTONIZED PHOTON SPECTRA OF SUPERCRITICAL BLACK HOLE ACCRETION FLOWS WITH APPLICATION TO ULTRALUMINOUS X-RAY SOURCES. United States: N. p., 2012. Web. doi:10.1088/0004-637X/752/1/18.
Kawashima, T., Matsumoto, R., Ohsuga, K., Mineshige, S., Yoshida, T., & Heinzeller, D., E-mail: kawashima-t@astro.s.chiba-u.ac.jp. COMPTONIZED PHOTON SPECTRA OF SUPERCRITICAL BLACK HOLE ACCRETION FLOWS WITH APPLICATION TO ULTRALUMINOUS X-RAY SOURCES. United States. doi:10.1088/0004-637X/752/1/18.
Kawashima, T., Matsumoto, R., Ohsuga, K., Mineshige, S., Yoshida, T., and Heinzeller, D., E-mail: kawashima-t@astro.s.chiba-u.ac.jp. Sun . "COMPTONIZED PHOTON SPECTRA OF SUPERCRITICAL BLACK HOLE ACCRETION FLOWS WITH APPLICATION TO ULTRALUMINOUS X-RAY SOURCES". United States. doi:10.1088/0004-637X/752/1/18.
@article{osti_22037111,
title = {COMPTONIZED PHOTON SPECTRA OF SUPERCRITICAL BLACK HOLE ACCRETION FLOWS WITH APPLICATION TO ULTRALUMINOUS X-RAY SOURCES},
author = {Kawashima, T. and Matsumoto, R. and Ohsuga, K. and Mineshige, S. and Yoshida, T. and Heinzeller, D., E-mail: kawashima-t@astro.s.chiba-u.ac.jp},
abstractNote = {Radiation spectra of supercritical black hole accretion flows are computed using a Monte Carlo method by post-processing the results of axisymmetric radiation hydrodynamic simulations. We take into account thermal/bulk Comptonization, free-free absorption, and photon trapping. We found that a shock-heated region ({approx}10{sup 8} K) appears at the funnel wall near the black hole where the supersonic inflow is reflected by the centrifugal barrier of the potential. Both thermal and bulk Comptonization significantly harden photon spectra although most of the photons upscattered above 40 keV are swallowed by the black hole due to the photon trapping. When the accretion rate onto the black hole is M-dot Almost-Equal-To 200L{sub E}/c{sup 2}, where L{sub E} is the Eddington luminosity, the spectrum has a power-law component which extends up to {approx}10 keV by upscattering of photons in the shock-heated region. In higher mass accretion rates, the spectra roll over around 5 keV due to downscattering of the photons by cool electrons in the dense outflow surrounding the jet. Our results are consistent with the spectral features of ultraluminous X-ray sources, which typically show either a hard power-law component extending up to 10 keV or a rollover around 5 keV. We found that the spectrum of NGC 1313 X-2 is quite similar to the spectrum numerically obtained for high accretion rate (M-dot {approx} 1000L{sub E}/c{sup 2}) source observed with low viewing angle (i = 10 Degree-Sign -20 Degree-Sign ). Our numerical results also demonstrate that the face-on luminosity of supercritically accreting stellar mass black holes (10 M{sub Sun }) can significantly exceed 10{sup 40} erg s{sup -1}.},
doi = {10.1088/0004-637X/752/1/18},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 752,
place = {United States},
year = {2012},
month = {6}
}