Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210..167y&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 167-168 (IAU Colloquium 134)
Astronomy and Astrophysics
Astrophysics
Asymptotic Giant Branch Stars, Stellar Envelopes, Stellar Mass Ejection, Stellar Oscillations, Astrophysics, Mira Variables, Stellar Evolution
Scientific paper
The life-time of the star on asymptotic giant branch (AGB) is approximately 6 x 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 nonpulsation, but constant mass loss rate (approximately 5 x 10-7 solar mass/yr) 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 approximately 3 x 10-6 solar mass/yr, the star evolved 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 approximately 10-4 solar mass/yr.
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