Marginally stable orbits around neutron stars and QPOs in low-mass X-ray binaries

Details Marginally stable orbits around neutron stars and QPOs in low-mass X-ray binaries Marginally stable orbits around neutron stars and QPOs in low-mass X-ray binaries

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.2011m&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #20.11; Bulletin of the American Astronomical Society, Vol. 24, p.1154

Physics

2

Scientific paper

A variety of quasi-periodic intensity oscillations (QPOs) have been observed in low-mass X-ray binaries. To explain some of these QPOs, scenarios have been proposed that require the magnetic field of the neutron star to be negligible, the radius Rms of the marginally stable orbit to be greater than the equatorial radius R_eq of the star, and the character of the flow between Rms and R_eq to be significantly different from that outside Rms. Motivated in part by these scenarios, we have investigated further the physics of disk accretion by rotating nonmagnetic neutron stars. Among the important effects that must be included in any accurate treatment are the effect of rotation on the shape of the star, the effects of stellar rotation and oblateness on the metric, gravitational lensing, and the effects of radiation stresses on the accreting plasma. Although previous studies have considered some of these effects, ours is the first to consider all of them. We find that the character of the accretion flow near the neutron star is generally qualitatively different from that discussed by previous authors. We discuss the implications of our results for scenarios in which QPOs are produced in the flow near the neutron star. This work was supported in part by NSF grant PHY 91-00283 and NASA grant NAGW 1583.

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