The H-alpha variations of Epsilon Aurigae from the second to the fourth contact

Details The H-alpha variations of Epsilon Aurigae from the second to the fourth contact The H-alpha variations of Epsilon Aurigae from the second to the fourth contact

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985acaps...5..180t&link_type=abstract

(Acta Astrophysica Sinica, vol. 5, no. 3-4, 1985, p. 180-187) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 9, Dec.

Astronomy and Astrophysics

Astrophysics

2

Eclipsing Binary Stars, H Alpha Line, Stellar Envelopes, Stellar Models, Stellar Spectra, Supergiant Stars, B Stars, Radial Velocity, Variable Stars

Scientific paper

Epsilon Aurigae was observed in March, August 1983 and January, March 1984 with Reticon at coude focus of the McDonald 2.7 m and 2.1 m telescopes. Fifty-six observations were taken over eight nights during 2nd to 4th contact. The H-alpha shows noticeable variations in profile, radial velocity, and equivalent width of both absorption and emission components. A similar phenomenon was detected during the corresponding phase of the 1955-1957 eclipse. A model is proposed, in which the primary is a F0 supergiant surrounded by a thin ring (or disk) of radius R = 450 solar radii and rotating at velocity V(sini) = 60 - 70 km/s. This is the major source of the H-alpha emission component. The secondary is a type B star surrounded by a very extended envelope (R = 1000 solar radii) and its rotational speed is similar to that of the ring of the primary. The B star heats a portion of the envelope comparable in size with the primary with enough hydrogen atoms in the lowest excited states, which cause the absorption of the emission from the primary.

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