Epsilon Coronae Austrinae - Evidence for binary star evolution

Details Epsilon Coronae Austrinae - Evidence for binary star evolution Epsilon Coronae Austrinae - Evidence for binary star evolution

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...200...98t&link_type=abstract

Astrophysical Journal, vol. 200, Aug. 15, 1975, pt. 1, p. 98-105. Research supported by the Association of Universities for Res

Astronomy and Astrophysics

Astronomy

25

Eclipsing Binary Stars, Radial Velocity, Stellar Evolution, Stellar Spectra, Line Spectra, Nuclear Fusion, Stellar Luminosity, Stellar Mass

Scientific paper

Spectroscopic radial velocity observations of epsilon Coronae Austrinae, the brightest W UMa type constant binary system, are reported. The parameters (masses, radii, luminosities) of the components of the system have been determined. The primary, of mass about 1.5 solar masses, is probably evolved and burning hydrogen in its core. The secondary has a very low mass, near 0.15 solar mass. It may be unevolved and deriving most of its luminosity from energy transfer from the primary; or it may be significantly evolved and burning hydrogen in a shell, with the present mass exchange the second one. Difficulties with the solution and possible evidence for gas streaming, mass loss, and angular momentum loss from the system are discussed.

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