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Mira Variables: Statistical Parallaxes, Kinematics and Period–Luminosity Relation

Published online by Cambridge University Press:  12 April 2016

E. Kilpio
Affiliation:
Institute of Astronomy, 48 Pyatnitskaya Str., Moscow 109017, Russia
O. Malkov
Affiliation:
Institute of Astronomy, 48 Pyatnitskaya Str., Moscow 109017, Russia
N. Kharchenko
Affiliation:
Main Astrophysical Observatory, Golosiiv, 252650 Kiev, Ukraine
E. Schilbach
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
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Abstract

Based on the statistical parallaxes, the mean absolute magnitudes and the spatial kinematical parameters were determined as functions of the periods for Mira variables given in the GCVS-4 and selected stars for which new kinematical data were obtained during the last decade. The BC were derived for the oxygen-rich Miras and the P–L relation was compared with predictions from pulsation theory. The following findings result from this analysis:

1) With respect to Miras, the GCVS-4 is complete down to V = 9m.

2) The kinematical and orbital parameters indicate a higher age for the oxygen-rich Miras pulsating with smaller periods.

3) The M bol-period relation of the oxygen-rich Miras shows a low dispersion and does not depend on the pulsation mode. The resulting P–L relation is a superposition of P–L relations of different pulsation modes.

4) The fraction of the fundamental mode pulsators decreases with increasing pulsation period.

Type
Part 2. Variability of High-Luminosity Stars
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Barthès, D. 1998, A&A, 333, 647 Google Scholar
Kholopov, P.N. et al. 1985-1988, General Catalogue of Variable Stars, 4th Edition, (Moscow: Nauka), [GCVS-4]Google Scholar
Saio, H. & Yoshii, Y. 1979, PASP, 91, 553 CrossRefGoogle Scholar
Sharov, A.S. 1963, AZh, 40, 900 Google Scholar
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