Estimating the Spin of Stellar-Mass Black Holes by Spectral Fitting of the X-Ray Continuum
Rebecca ShafeeDepartment of Physics, Harvard University, 17 Oxford Street, Cambridge, MA 02138Jeffrey E. McClintockHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Ramesh NarayanHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138Shane W. DavisDepartment of Physics, University of California, Santa Barbara, Santa Barbara, CA 93106-9530Li‐Xin LiMax-Planck-Institut für Astrophysik, Postfach 1317, D-85741 Garching, GermanyRonald A. RemillardKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139
2005en
ABI
Аннотация
We fit X-ray spectral data in the thermal-dominant, or high-soft, state of two dynamically confirmed black holes, GRO J1655-40 and 4U 1543-47, and estimate the dimensionless spin parameters a* a/M of the two holes. For GRO J1655-40, using a spectral hardening factor computed for a non-LTE relativistic accretion disk, we estimate a*similar to 0.75 and a*similar to 0.65-0.75, respectively, from ASCA and RXTE data. For 4U 1543-47, we estimate a*similar to 0.75-0.85 from RXTE data. Thus, neither black hole has a spin approaching the theoretical maximum a* = 1.
Идентификаторлар
Иқтибослар ва манбалар
18 та иқтибос0 та фойдаланилган манба
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