The energy distribution and the recent light history of X Persei

Details The energy distribution and the recent light history of X Persei The energy distribution and the recent light history of X Persei

Dec 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mnras.181..685p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 181, Dec. 1977, p. 685-693.

Astronomy and Astrophysics

Astronomy

19

B Stars, Binary Stars, Stellar Spectrophotometry, X Ray Sources, High Temperature Plasmas, Light Curve, Near Infrared Radiation, Stellar Envelopes, Stellar Luminosity, Stellar Mass Ejection, Stellar Models

Scientific paper

Results of UBVRI photoelectric photometry, IR observations, and objective-prism spectroscopy of X Per are used to study the energy distribution of the star during two different epochs, with particular regard to the IR spectrum and the nature of the observed luminosity variations. A model consisting of a neutron star moving around a Be primary with a period of 22 hr is adopted for the X Per/3U 0352+30 system. The color excess of the star and its Balmer discontinuity are discussed, physical parameters of the Be star are derived, and the IR energy distribution of X Per is examined. The long-term variability of this system is analyzed, and a model of plasma emission from a gaseous circumstellar disk is proposed as a more realistic interpretation of the IR excess. The mass-accretion rate of the X-ray source is computed, an upper limit of 0.46 is determined for the interstellar extinction toward X Per, and a correlation is suggested among expansion of the optical source's atmosphere, the X-ray flux, and the IR excess. It is concluded that the primary does not fill its Roche lobe and that the X-ray emission might be due to wind accretion onto the compact companion.

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