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Miras, mass loss, and the origin of planetary nebulae

Published online by Cambridge University Press:  12 April 2016

L. A. Willson
L. A. Willson*
Affiliation:
Erwin W. Fick Observatory, Physics Department, Iowa State University

Extract

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Mira variables are found at the tip of the asymptotic giant branch, with L≈3000-5000Lʘ and TeH3000K. (Feast 1981; Willson 1981a). They are fundamental mode pulsators (Willson 1979, 1981a). A typical Mira has P~350 days, R~200-300Rʘ, M~1-2Mʘ (Willson 1979; 1981a). From the atmospheric velocities of the Miras plus a fundamental mode period-massradius relation one finds present masses for the Miras which are not very different from their progenitor masses (Willson 1981a). This suggests that pre-Mira mass loss is moderate -- ≲20% of the mass is lost before pulsation starts. In fact one expects only moderate mass loss before the Mira stage;

Type
Session VI - Mass Loss and Stellar Evolution: Low Mass Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 353 - 356
Copyright
Copyright © Reidel 1981

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