期刊
ASTRONOMY & ASTROPHYSICS
卷 403, 期 3, 页码 1023-1029出版社
E D P SCIENCES
DOI: 10.1051/0004-6361:20030498
关键词
stars : emission line, Be; stars : winds, outflows; technique : interferometric
Using the SIMECA code developed by Stee Araujo (1994); Stee et al. (1995) for Be stars we obtain a correlation between the mass loss rates. (M)over dot and the Brgamma continuum luminosity as a function of the opening angle of the disk. We show that this correlation is similar to those obtained by Scuderi et al. (1998) for O-B supergiants. We found that the wind density at the base of the photosphere, from a sample of 8 Be stars, lies between 10(-13) and 10(-12) g cm(-3). We also present a relationship between the mass of the circumstellar disk and the 2.16 mum flux. Finally we emphasize how interferometric measurements can help to estimate the wind density and we present a sample of 16 Be stars with predicted visibilities that can be observed with the VLTI.
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