Mass loss from Be stars derived from UV spectra.
de Freitas Pacheco, J. A.
Brazil
Abstract
The present investigation considers the interpretation of UV line profiles of some Be stars obtained with the International Ultraviolet Explorer (IUE) spacecraft, giving particular attention to Pi Aqr. The mass-loss rates are estimated using the Sobolev approximation and assuming that the observed asymmetric UV lines are formed in an expanding envelope above and below the considered denser equatorial region. A mass-loss rate of 2.4 x 10 to the -9th solar mass per year is derived for Pi Aqr. The derived value for Pi Aqr is comparable to that deduced for Gamma Cas by Hensberge et al. (1980) and to that deduced for the BOV star Tau Sco by Lamers and Rogerson (1978).