Strong-field general relativity and quasi-periodic oscillations in x-ray binaries

Details Strong-field general relativity and quasi-periodic oscillations in x-ray binaries Strong-field general relativity and quasi-periodic oscillations in x-ray binaries

1997-01-16

arxiv.org/abs/astro-ph/9701101v1

Astronomy and Astrophysics

Astrophysics

4 pages, uses aas2pp4.sty, submitted to ApJL

Scientific paper

10.1086/310617

Quasi-periodic oscillations (QPOs) at frequencies near 1000 Hz were recently discovered in several x-ray binaries containing neutron stars. Two sources show no correlation between QPO frequency and source count rate (Berger et al. 1996, Zhang et al. 1996). We suggest that the QPO frequency is determined by the Keplerian orbital frequency near the marginally stable orbit predicted by general relativity in strong gravitational fields (Muchotrzeb-Czerny 1986, Paczynski 1987, Kluzniak et al. 1990). The QPO frequencies observed from 4U 1636-536 imply that the mass of the neutron star is 2.02 +/- 0.12 solar masses. Interpretation of the 4.1 keV absorption line observed from 4U 1636-536 (Waki et al. 1984) as due to Fe XXV ions then implies a neutron star radius of 9.6 +/-0.6 km.

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