EDP Sciences
Free access
Issue
A&A
Volume 391, Number 2, August IV 2002
Page(s) 633 - 639
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20020867


A&A 391, 633-639 (2002)
DOI: 10.1051/0004-6361:20020867

Behaviour of the periods in double mode RR Lyrae, V26 in M15

M. Paparó1, B. Szeidl1, S. M. Saad2, Z. Kolláth1 and M. S. Abu Elazm2

1  Konkoly Observatory, 1525 Budapest XII, PO Box 67, Hungary
    e-mail: paparo@konkoly.hu, szeidl@konkoly.hu, kollath@konkoly.hu
2  Helwan Institute of Astronomy and Geophysics, Cairo, Egypt
    e-mail: astro3@frcu.eun.eg

(Received 3 September 2001/ Accepted 30 April 2002)

Abstract
The changes in the periods of the fundamental and first overtone pulsation of the variable V26 in the globular cluster M15 are studied. The analysis was based on published observations. The method of investigation was outlined in our previous paper (Paparó et al. 1998). The Fourier phase diagrams for both frequencies have been constructed. General guidelines concerning the cycle counting problems are discussed. In both periods a sudden increase took place around JD 2431500 ( $\approx$1945) and the changes were the same in sign but slightly different in magnitude. The period change behaviour of the fundamental mode was noticed for the first time. Before the abrupt change the fundamental and first overtone periods were $P_0 = 0\fd538898$ and $ P_1 = 0\fd402256$ days and after it $P_0 = 0\fd538979$ and $P_1 = 0\fd402273$ days. Although the fundamental component is very weak, there is a remarkable concordance between our period after the abrupt change and the period derived by Clement & Walker (1991). The disagreement between the observed period changes and the expectation of stellar evolutionary theory strongly suggest that period changes are dominated by short term changes governed by the physics of the star. Fast changes in oscillation frequency such as in V26/M15 cannot take place without sudden changes in the stellar structure. The possible physical processes are the mixing events in a small part of the semiconvective zone (Sweigart & Renzini 1979) or the dredge up of a small amount of helium by occasional convection overshooting (Cox 1998).


Key words: stars: individual: V26 in M15 -- stars: oscillations -- stars: variables: RR Lyrae -- globular cluster: individual: M15

Offprint request: M. Paparó, paparo@konkoly.hu




© ESO 2002