Rotational Mass Loss by Be Stars

Details Rotational Mass Loss by Be Stars Rotational Mass Loss by Be Stars

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003arep...47..826t&link_type=abstract

Astronomy Reports, vol. 47, Issue 10, p.826-830

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We have carried out a numerical study of rotational mass loss by rapidly rotating Be stars assuming preservation of rigid-body rotation during their main-sequence evolution. Evolutionary models are computed for stars with solar chemical composition and initial masses of 3, 10 and M &sun;. As a result of their rapid initial rotation, these stars can lose one to four percent of their initial mass during the main-sequence stage. The amount of mass lost increases with the initial mass of the star. The matter lost by Be stars can form gas-dust disks with masses comparable to the masses of planets, which, in principle, makes possible the formation of planetary systems around such stars.

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