High energy X-ray observations of CYG X-3 from from OSO-8: Further evidence of a 34.1 day period

Details High energy X-ray observations of CYG X-3 from from OSO-8: Further evidence of a 34.1 day period High energy X-ray observations of CYG X-3 from from OSO-8: Further evidence of a 34.1 day period

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981stin...8218085d&link_type=abstract

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Astronomy and Astrophysics

Astronomy

Astronomical Spectroscopy, Binary Stars, Stellar Spectra, Variable Stars, X Ray Sources, X Ray Spectroscopy, Cygnus Constellation, Oso-8, Periodic Variations, Stellar Mass Accretion

Scientific paper

The X-ray source Cyg X-3 (=4U2030+40) was observed with the high energy X-ray spectrometer on OSO-8 for two weeks in 1975 and in 1976 and for one week in 1977. No change in spectral shape and intensity above 23 keV was observed from year to year. No correlation is observed between the source's intensity and the phase of the 34.1 day period discovered by Molteni, et al. (1980). The pulsed fraction of the 4.8 hour light curve between 23 and 73 keV varies from week to week, however, and the magnitude of the pulsed fraction appears to be correlated with the 34.1 day phase. No immediate explanation of this behavior is apparent in terms of previously proposed models of the source.

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