Time Resolved UV Spectrometry of VELA X-1

Details Time Resolved UV Spectrometry of VELA X-1 Time Resolved UV Spectrometry of VELA X-1

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991hst..prop.2572m&link_type=abstract

HST Proposal ID #2572

Computer Science

Hst Proposal Id #2572

Scientific paper

We propose to observe HD77581, the optical counterpart of the X-ray source Vela X-1 (4U0900-40), in order to study the effects of X-ray ionization on the stellar wind from this star. UV Resonance line profile changes with orbital phase predicted by Hatchett and McCray (1977) are a familiar phenomenon in this system. The goals of this observing program are to search for theoretically predicted line profile changes correlated with the 283s pulse period of the compact X-ray source and to study correlations of the UV resonance line variability with X-ray variability in coordinated observations by the GINGA satellite. Observations of such line profile variability can tell us about the geometry of the radiation pattern from the pulsar and the dynamics of the accretion flow.

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