Journal
ASTROPHYSICAL JOURNAL
Volume 731, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/731/2/121
Keywords
accretion, accretion disks; black hole physics; gravitation; X-rays: binaries
Categories
Funding
- Horace Hearne Institute for Theoretical Physics at Louisiana State University
- Michigan Center for Theoretical Physics at the University of Michigan
- World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan
- JSPS [22740147]
- NSF [PHY-0903631]
- Institute for the Physics and Mathematics of the Universe at The University of Tokyo
- Direct For Mathematical & Physical Scien
- Division Of Physics [903631] Funding Source: National Science Foundation
- Grants-in-Aid for Scientific Research [22740147] Funding Source: KAKEN
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Black holes in general relativity are known as Kerr black holes and are characterized solely by two parameters, the mass M and the spin J. All the higher multipole moments of the gravitational field are functions of these two parameters. For instance, the quadrupole moment is Q = -J(2)/M, which implies that a measurement of M, J, and Q for black hole candidates would allow one to test whether these objects are really black holes as described by general relativity. While future gravitational-wave experiments will be able to test the Kerr nature of these objects with very high accuracy, in this paper we show that it is possible to put constraints on the quadrupole moment of stellar-mass black hole candidates by using presently available X-ray data of the thermal spectrum of their accretion disk.
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