Spectral and Temporal Behavior of Low Mass X-ray Binaries Observed by the Einstein SSS and MPC, and the Broad Band X-ray Telescope

Details Spectral and Temporal Behavior of Low Mass X-ray Binaries Observed by the Einstein SSS and MPC, and the Broad Band X-ray Telescope Spectral and Temporal Behavior of Low Mass X-ray Binaries Observed by the Einstein SSS and MPC, and the Broad Band X-ray Telescope

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.3204c&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #32.04D; Bulletin of the American Astronomical Society, Vol. 24, p.1169

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Scientific paper

An extensive survey of 50 low mass X-ray binaries was carried out using the HEAO-2 Einstein Solid State Spectrometer data (0.5-4.5 keV) with the Monitor Proportional Counter data (1.2-20.0 keV) and the Broad Band X-Ray Telescope (BBXRT) (0.5-12 keV). Spectra were selected on the basis of intensity and fit with a set of simple and complex spectral models. For all the subclasses, including Eddington-limited bulge sources, bursters, dippers, the soft spectrum black hole candidates, and a few transients in decline, the spectra could be fit acceptably with combinations of thermal bremsstrahlung and blackbody spectra or a Comptonized spectrum and a blackbody. The results rule out optically thick disk models for the bright Z sources and power law models for bursters. There is a progression of spectra as a function of X-ray luminosity for the bursters, Atoll and Z sources. Interpretation is discussed in terms of separate emission regions, one due to radial accretion onto a neutron star and the optically thick component that appears for higher luminosity due to a boundary layer or to high optical depth to scattering in the flow. A lower temperature blackbody required in some cases could be an expected contribution from the accretion disk. The soft spectrum sources are dominated by blackbody spectra, but for two, low effective area is a problem for the black hole interpretation. The strongest of previously reported low energy X-ray lines due to OVIII or Fe L transitions are confirmed. Similar line emission is seen for several other sources, in particular X0614+091. The photoionized gas in the inner part of an accretion disk corona can give Fe K lines from Fe XXV. BBXRT obtained upper limits for X0614+091 and M15 which are consistent with the coronal model.

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