Near infrared photometry and OH observations of Mira variables - Implications for stellar evolution

Details Near infrared photometry and OH observations of Mira variables - Implications for stellar evolution Near infrared photometry and OH observations of Mira variables - Implications for stellar evolution

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....93..325m&link_type=abstract

Astronomy and Astrophysics, vol. 93, no. 1-2, Jan. 1981, p. 325-333.

Astronomy and Astrophysics

Astronomy

4

Hydroxyl Emission, Infrared Astronomy, Infrared Photometry, Mira Variables, Near Infrared Radiation, Stellar Evolution, Stellar Spectrophotometry, Variable Stars, Galactic Evolution, Light Curve, Milky Way Galaxy, Stellar Envelopes, Stellar Luminosity, Stellar Radiation

Scientific paper

A statistical study based on near-infrared photometry of long period variables of the Mira type observed by Lockwood (1972) is presented. The excess of infrared luminosity in OH miras (Foy et al., 1975) is confirmed. The OH emission is shown to be related to the strength of the VO band system at 1.05 μm.
Using homogeneous spectral types and the relation of Cahn and Wyatt (1978), we determine initial main sequence masses. In the framework of their model we establish that:
- the mira variables corresponding to a main sequence mass between 1.0 and 1.9 Msun begin their mira stage as non-OH stars, and after a time depending on their main sequence mass, become OH emitters.
- the OH miras which emit at 1612 MHz have a main sequence mass < 1.4 Msun, and will directly evolve to the white dwarf stage, whereas those that emit only at 1667/65 MHz can produce planetary nebulae. Though not yet detected at 1612 MHz, some stars are candidate emitters in this line.
The study of light curves (Garrique, 1980), together with the comparison of some radial optical and radio velocities, seems to indicate that a pulsating model may be possible for the OH miras emitting at 1667/65 MHz. The OH miras emitting at 1612 MHz are more disturbed, the perturbation being probably responsible for this satellite-line emission.

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