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Near-critical spherical accretion by neutron stars - General relativistic treatmentTime-independent spherical accretion by a neutron star is studied using general relativistic radiation hydrodynamics. Numerical integrations of the flow equations are presented. These show that when the luminosity is sufficiently close to (but below) the Eddington limit, the flow velocity increases with decreasing radius far from the neutron star, reaches a maximum at an intermediate radius, and decreases at small radii. A large fraction of the binding energy of the flow is transferred to the radiation through scattering before the flow strikes the surface of the neutron star. Following Miller's treatment of accretion at luminosites near the Eddington limit (which neglected general relativistic effects), analytic approximations for the decelerating phase of the flow's velocity profile are derived. The dependence of the solutions on the variable Eddington factor prescription chosen to close the radiation moment equations is also examined.
Document ID
19910048955
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Park, Myeong-Gu
(Illinois, University Urbana, United States)
Miller, Guy S.
(Los Alamos National Laboratory NM, United States)
Date Acquired
August 14, 2013
Publication Date
April 20, 1991
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 371
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
91A33578
Funding Number(s)
CONTRACT_GRANT: NSF PHY-86-00377
CONTRACT_GRANT: NAGW-1583
Distribution Limits
Public
Copyright
Other

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