Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.3207s&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #32.07; Bulletin of the American Astronomical Society, Vol. 24, p.1170
Astronomy and Astrophysics
Astronomy
Scientific paper
Vela X-1 was observed in the energy range 1-12 keV with the Broad Band X- ray Telescope (BBXRT) instruments for a continuous coverage of 2929 seconds which was about 10 of this binary X-ray pulsar's pulse period. The pulse modulation is clearly seen. The orbital phase was at 0.19 and the continuum spectrum was fitted to a simple power law with low energy absorption which showed low column density, 3times 10(22}cm({-2)) , and there was no obviously detectable absorption edge at 7.1-7.3 keV as was observed by previous experiments. The highly variable column density from 2times 10(22) to 5times 10(23}cm({-2)) at different orbital phase is attributed to the variability of the observations. The known variable Fe-K_alpha fluorescence line at 6.4 keV due to the X-ray beam interacting with the ambient cold matter, such as the accreting stellar wind, maybe of the accretion disk, and the atmosphere of the optical companion, HD 77581, was detected with a focal plane solid state detector, Si(Li), of which the energy resolution was 150 eV FWHM at 6 keV. No pulse phase modulation was found in the iron line parameters. It is a weak line with its equivalence width at 60 eV but it is first time resolved to a width of 155 eV FWHM. If the line width is broadened by the photons scattering off the thermal electrons, the temperature of the reprocessing site of the fluorescence iron line is no more than 4 times 10(5) K. The location of the reprocessing site is discussed.
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