Epsilon Aurigae in an evolutionary context

Details Epsilon Aurigae in an evolutionary context Epsilon Aurigae in an evolutionary context

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985eepa.rept...49w&link_type=abstract

In NASA, Washington The 1982-1984 Eclipse of Epsilon Aurigae p 49-60 (SEE N86-12168 02-89)

Physics

8

Auriga Constellation, Eclipsing Binary Stars, Pre-Main Sequence Stars, Stellar Evolution, Stellar Temperature, Helium, Hydrogen, Luminosity, Mass Transfer, Models, Supergiant Stars

Scientific paper

Basic observational data of Epsilon Aurigae are summarized and used as the basis of a discussion of possible evolutionary states of the system. Constraints posed by the presence of a cold disk surrounding the secondary star are also outlined. Possible evolutionary models of the F0 Ia supergiant range from pre-main sequence contraction through shell hydrogen burning, core helium burning, to shell helium burning, depending on the absolute luminosity of the system, for models in which no mass transfer has taken place. Models invoking binary interaction include core and shell helium burning stars, and pre-white dwarfs, again depending on the absolute luminosity of the system. A massive shell helium burning star or a pre-white dwarf mass transfer remnant would appear the most likely of these models at present. Observational tests of these models are briefly outlined.

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