Application of a general relativistic accretion disk model to LMC X-1, LMC X-3, X1608 - 522, and X1636 - 536

Details Application of a general relativistic accretion disk model to LMC X-1, LMC X-3, X1608 - 522, and X1636 - 536 Application of a general relativistic accretion disk model to LMC X-1, LMC X-3, X1608 - 522, and X1636 - 536

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...367..213e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 367, Jan. 20, 1991, p. 213-220.

Astronomy and Astrophysics

Astronomy

75

Accretion Disks, Black Holes (Astronomy), Neutron Stars, Relativistic Theory, Stellar Models, X Ray Binaries, Doppler Effect, Stellar Mass, X Ray Sources

Scientific paper

The persistent X-ray spectra of black hole candidates and X-ray bursters are compared with a model spectrum of an accretion disk around either a black hole or a neutron star. The model takes account of general relativity and assumes that the accretion disk is geometrically thin and in a steady state. This general relativistic model is compared with other conventional model spectra that have been used to fit observations so far. It is shown that the general relativistic model, in shape, is quite similar to the multicolor disk model and the Sunyaev-Titarchuk Comptonization model. These conventional models are used to perform spectral fitting analysis on the black hole candidates LMC X-1 and LMC X-3 and on the X-ray bursters X1608 - 522 and X1636 - 536 using the general relativistic model. As a result, the lower limit of the masses of LMC X-1 and LMC X-3 and the probable masses of X1608 - 522 and X1636 - 536 are obtained. The former masses are larger than the theoretical upper limit of the neutron star mass, 2.5 solar masses, and the latter masses are consistent with the canonical neutron star mass, 1.4 solar mass.

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