An eccentric close binary model for the X Persei system

Details An eccentric close binary model for the X Persei system An eccentric close binary model for the X Persei system

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....54..817h&link_type=abstract

Astronomy and Astrophysics, vol. 54, no. 3, Feb. 1977, p. 817-822. Research supported by the Nederlandse Organisatie voor Zuive

Astronomy and Astrophysics

Astrophysics

18

Astronomical Models, Binary Stars, Neutron Stars, X Ray Sources, Apsides, Eccentric Orbits, Stellar Evolution, Stellar Models, Stellar Motions, Stellar Winds, Systems Stability

Scientific paper

A model for the X-ray source 3U 0352 + 30, associated with the 6th-magnitude O9.5 V pe star X Per, is proposed. It is suggested that a 1.5-solar-mass neutron star pulsating with a 13.9-magnitude period is moving in 22.4 hr around a relatively normal O9.5 V star in an inclined slightly eccentric orbit, giving rise to a 22.4-hr modulation in the X-ray flux produced by capture of stellar-wind material from the main star, which slightly underfills its critical lobe at periastron. The apsidal motion of the elliptic orbit may explain the 581-day period observed in the wavelength shifts of the higher Balmer absorption lines. The system may be very close to tidal instability. Predictions for the X-ray as well as the optical behavior on the basis of the model are given.

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