Energy dependence of normal branch quasi-periodic intensity oscillations in low-mass X-ray binaries

Details Energy dependence of normal branch quasi-periodic intensity oscillations in low-mass X-ray binaries Energy dependence of normal branch quasi-periodic intensity oscillations in low-mass X-ray binaries

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...388..541m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 388, April 1, 1992, p. 541-554. Research supported by DOE.

Astronomy and Astrophysics

Astrophysics

34

Accretion Disks, Compton Effect, Neutron Stars, Spectral Energy Distribution, Stellar Oscillations, X Ray Binaries, Radial Flow, Stellar Mass, X Ray Spectra

Scientific paper

The properties of the approximately 6 Hz quasi-periodic X-ray intensity oscillations observed in the low-mass X-ray binary Cyg X-2 when it is on the normal spectral branch are shown to be consistent with a model in which photons from a central source with a fixed spectrum are Comptonized by an oscillating radial inflow. As the electron scattering optical depth of the flow varies, the spectrum of the escaping X-rays appears to rotate about a pivot energy that depends mainly on the electron temperature in the flow. The temperature derived from the observed energy dependence of the Cyg X-2 normal branch oscillations is approximately 1 keV, in good agreement with the estimated Compton temperature of its X-ray spectrum. The mean optical depth tau of the Comptonizing flow is inferred to be about 10, while the change in tau over an oscillation is estimated to be about 1; both values are in good agreement with radiation hydrodcode simulations of the radial flow.

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