On the evolutionary status of the variable Ae star V351 Ori

Details On the evolutionary status of the variable Ae star V351 Ori On the evolutionary status of the variable Ae star V351 Ori

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24..106k&link_type=abstract

Astronomy Letters, Volume 24, Issue 1, January 1998, pp.106-110; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 133

Astronomy and Astrophysics

Astronomy

6

Scientific paper

In addition to the previously reported peculiarities of the variable Ae star V351 Ori, which characterize it as a post-main-sequence star [peculiar light variations, low surface gravity, its position in the Hertzsprung-Russell (H-R) and T_eff-log g diagrams, no association with regions of star formation, etc.], an analysis of the profiles of hydrogen absorption lines has led us to conclude that the hydrogen abundance in the stellar photosphere is ~40%. A carefully reconstructed profile of the Hα emission line points to an outflow of matter rather than its accretion onto the star, as assumed earlier. Taken collectively, all these pieces of evidence strongly suggest that V351 Ori is a post-main-sequence star.

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