Short period Mira variables. I - Photometric metallicity estimates for field stars

Details Short period Mira variables. I - Photometric metallicity estimates for field stars Short period Mira variables. I - Photometric metallicity estimates for field stars

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..583h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 583-589.

Astronomy and Astrophysics

Astrophysics

17

Galactic Structure, Metallicity, Mira Variables, Stellar Composition, Stellar Spectrophotometry, Asymptotic Giant Branch Stars, Globular Clusters, Stellar Luminosity, Stellar Motions

Scientific paper

The group of short-period Mira variables (periods less than 200 days) is thought to be a mixture of metal-poor and disk stars. Possible ways are considered to separate stars of different metallicities on the basis of photometry and existing models for the atmospheres and pulsational properties of low-mass Miras. Photometric data combined with metal abundances for globular cluster Miras and the galactic kinematics of field Miras show that (Vmax - K)0 can be used to separate disk stars and metal-poor stars and to estimate metallicity differences. The available VJK-photometry for some field stars is consistent with a metallicity spread within this group of about -0.5 dex.

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