The P-L relation for RR Lyrae-like stars with 0.8d less than P less than 3d

Details The P-L relation for RR Lyrae-like stars with 0.8d less than P less than 3d The P-L relation for RR Lyrae-like stars with 0.8d less than P less than 3d

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..111s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 1, p. 111-120

Astronomy and Astrophysics

Astrophysics

23

Globular Clusters, Hertzsprung-Russell Diagram, Horizontal Branch Stars, Orbital Mechanics, Stellar Evolution, Variable Stars, Light Curve, Metallicity, Stellar Luminosity

Scientific paper

Data are summarized for 52 of the rare pulsating variables, here called AHB1 variables for 'above horizontal branch', that have RRab Lyrae-like light curves but periods in the range of 0.8 less than P less than 3d. The absolute magnitudes, calculated either from the pulsation equation or determined relative to the level of the globular cluster horizontal branch, range from Mv = +0.2 to Mv = -1.4. The P-L relation is well defined, with a ridge-line equation of Mbol = -2.00 log P - 0.10. The standard deviation of the present sample about the rigid-line is only 0.29 mag. Theoretical evolutionary tracks on the way from the ZAHB to the Asymptotic Giant Branch (AGB) conform well with the data and show that the P-L relation for AHB1 stars is independent of metallicity in this period range. This is in contrast to the absolute magnitudes of normal RR Lyraes near the horizontal branch in the period range from 0.4 to 0.8d, where there is a strong dependence of Mv on metallicity, also predicted by the models shown here. The rate of transversal through the instability strip is of the order of 100 times faster for these stars than for the ordinary RR Lyrae stars closer to the horizontal branch, making it likely that their observed period changes are due to secular evolution, well above pulsation 'noise'.

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