Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..39..495s&link_type=abstract
Astrophysics and Space Science, vol. 39, Feb. 1976, p. 495-497.
Astronomy and Astrophysics
Astrophysics
3
B Stars, Binary Stars, Computerized Simulation, Stellar Envelopes, Stellar Models, Absorption Spectra, Orbital Velocity, Periodic Variations, Spectral Line Width, Stellar Temperature, Three Body Problem
Scientific paper
Preliminary results are reported for analysis of a set of computer simulation models using Hynek's (1940, 1944) data for the peculiar B2e star phi Persei. It is proposed that phi Persei is a binary system with a period of 126.7 days, that a stationary gas ring surrounds the primary, and that the observed periodic variations of the spectral line profiles result from the revolution of the system. The masses and orbital velocities of the two components, as well as the component separation, are derived from computations of emission and absorption profiles due to a completely opaque gas ring represented by a periodic orbit of the restricted three-body problem. It is suggested that the secondary is a helium star corresponding to case B of close binary evolution, that its He-core contains 90% of its total mass, and that its effective temperature is about 40,000 K.
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