The X ray absorption spectra of massive X ray binaries

Details The X ray absorption spectra of massive X ray binaries The X ray absorption spectra of massive X ray binaries

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296...31h&link_type=abstract

In its The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 1: X Ray Binaries p 31-37 (SEE N90-25711 19-89)

Astronomy and Astrophysics

Astronomy

3

Spectrum Analysis, Stellar Spectra, Stellar Winds, X Ray Absorption, X Ray Binaries, X Ray Spectra, European Space Programs, Exosat Satellite, Interstellar Gas, Stellar Flares

Scientific paper

Spectral variations in EXOSAT spectra from high mass X-ray binaries are discussed. An observation of the 4U1700-37/HD153919 system of almost one complete binary cycle of 3.41 days showed a sharp increase in absorption at binary phase 0.6. This increase can be modeled as due to a gas stream from the primary trailing the neutron star. The EXOSAT observations of Vela X-1 (4U0900-40/HD 77581) reveal sharp changes in the absorbing column density on top of a more gradual increase between eclipse egress and ingress of the X-ray source. The higher absorption after superior conjunction of the X-ray source indicates the presence of a dense gas stream similar to the one in the 4U1700-37/HD 153919 system. Spectra from 4U1700-37 taken near the peak intensity of flares around phase 0.5 and spectra from Vela X-1 at early orbital phase show an excess of NH at energies lower than 3 keV over that expected from a cold absorber. This excess can be modeled with absorption by ionized gas around the X-rays source. A much larger low energy excess is present at later phases where the NH is higher and can be explained by scattered X-rays.

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