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Stellar Pulsation: (I) Analysis of Stability of Envelope

Published online by Cambridge University Press:  12 April 2016

Yu Zhi-Yao
Yu Zhi-Yao*
Affiliation:
Shanghai Observatory, 80 Nandan Road, Shanghai 200030, China

Abstract

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The life-time of the star on AGB is approximately 6 × 104 yr. We divide it into front half and back half of AGB (including to optical Mira variable and OH/IR star) according to their evolution character. The observations show that the star has non-pulsation, but constant mass loss rate (~ 5 × 10−7M⊙ yr−1) on front half of AGB. Its circumstellar envelope is formed. When the star has pulsation on back half of AGB, its mass loss rate is relative with time, and increases gradually. In this time the star is on the stage of optical Mira variable. When the mass loss rate reaches the value of ~ 3 × 10−6M⊙ yr−1, the star evoluted from the stage of optical variable into the stage of radio bright OH/IR star. On the end of AGB the mass loss rate reaches ~10−4M⊙ yr−1. (Band and Habing 1983, Hermen and Habing 1985).

Type
II. Observational Facts
Information
International Astronomical Union Colloquium , Volume 134: Nonlinear Phenomena in Stellar Variability , 1993 , pp. 167 - 168
Copyright
Copyright © Kluwer 1993

References

Band, B. and Habing, H.J.: 1983, Astronomy and Astrophysics 127, 73.Google Scholar
Hermen, J. and Habing, H.J.: 1985, Phys. Rep. 124, 175.Google Scholar