Evolution of the Hα profile of the Be star HD 184279.

Details Evolution of the Hα profile of the Be star HD 184279. Evolution of the Hα profile of the Be star HD 184279.

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990rmxaa..20....7a&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, Vol. 20, No. 1, p. 7 - 14

Astronomy and Astrophysics

Astronomy

2

Be Stars: Line Profiles, Be Stars: H Alpha, Be Stars: Circumstellar Shells

Scientific paper

The authors report new Hα spectral observations on the V/R Be and shell star HD 184279. The observations cover part of a cycle that is probably reaching the steady-state of an activity period that started around 1971. The physical mechanism that can explain the observations, suggests that electron scattering is responsible for the very large emission wings observed. A small and very variable shell is present around the star, probably in form of an elongated disk that develops and grows during part of the cycle. A picture with an eccentric disk with semi-axis of 2 and 15 stellar radius seems to be adequate for this star. This envelope has a total mass of 10-9 stellar masses.

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