OH/IR stars in the Magellanic Clouds

Details OH/IR stars in the Magellanic Clouds OH/IR stars in the Magellanic Clouds

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...397..552w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 397, no. 2, p. 552-569.

Astronomy and Astrophysics

Astronomy

149

Asymptotic Giant Branch Stars, Hydroxyl Emission, Infrared Stars, Interstellar Masers, Magellanic Clouds, Supergiant Stars, Infrared Astronomy Satellite, Light Curve, Line Spectra, Planetary Nebulae, Point Sources, Stellar Evolution

Scientific paper

A group of IRAS sources in the LMC and SMC have been monitored in the near infrared and pulsation period of over 1000 days have been determined for some of them. OH maser emission has been detected from some of the LMC objects. The OH line profiles indicate that stellar wind velocities in LMC stars are lower than in Galactic stars, a result attributed to the lower metallicity in the LMC. Evidence is presented that reducing metallicity lowers mass loss rates from AGB stars provided they do not turn into carbon stars. It is suggested that carbon star formation allows high mass loss rate to be maintained in AGB stars of low metallicity. There is no convincing evidence that AGB stars evolve significantly beyond the classical AGB limit of M(bol) about -7.1.

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