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On the Equatorial Mass-Loss Rate of Be Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
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.
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- Part 5. Mass Loss in Pulsating Stars
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- Copyright © Astronomical Society of the Pacific 2002