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On the Equatorial Mass-Loss Rate of Be Stars

Published online by Cambridge University Press:  12 April 2016

A.T. Okazaki
A.T. Okazaki*
Affiliation:
Faculty of Engineering, Hokkai-Gakuen University, Toyohira-ku, Sapporo 062-8605, Japan

Abstract

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We numerically study the formation process of equatorial disks around isolated Be stars, using an SPH code. We find that the viscous decretion disk model naturally explains the observed disk formation episode of X Per, giving the equatorial mass-loss rate of several ×10−9 (ρ0/10−10 g cm−3) M⊙ yr−1, where ρ0 is the base density of the disk.

Type
Part 5. Mass Loss in Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 520 - 521
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

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