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Implication of a P-L Relation of Mira Variables

Published online by Cambridge University Press:  15 February 2018

Hiromoto Shibahashi
Hiromoto Shibahashi*
Affiliation:
Department of Astronomy, University of Tokyo, Japan

Extract

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Feast et al. (1989) obtained observationally a period-luminosity (P-L) relation of Mira variables in LMC. Basically, fundamental periods of stellar pulsation should be determined by two quantities —a mass and a radius of the star. The existence of a P-L relation implies a special condition that reduces a function of two variables into a function of only a single variable. Though the AGB appears as a thin line in the HR diagram like the Cepheid instability strip, it is an “asymptotically” merged line of evolutionary tracks of stars in a range of about 0.5-3 solar masses. This fact means that the masses of stars on a point of the AGB are not unique though the radii and the effective temperatures are unique, respectively. Therefore we cannot expect, in the case of AGB stars, that a period is reduced to a function of a single variable.

Type
Variable Stars as Distance Indicators
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 103
Copyright
Copyright © Cambridge University Press 1993

References

Feast, M.W., Glass, I.S., Whitelock, P.A., and Catchpole, R.M. 1989, MNRAS, 241, 375.CrossRefGoogle Scholar