The light curves of the short-period variable stars in Omega Centauri

Details The light curves of the short-period variable stars in Omega Centauri The light curves of the short-period variable stars in Omega Centauri

1999-04-12

arxiv.org/abs/astro-ph/9904139v1

Astronomy and Astrophysics

Astrophysics

4 pages, 3 ps figures Accepted for publication in Astronomy & Astrophysics, Main Journal

Scientific paper

The Fourier decomposition was applied to the light curves of the short period variable stars discovered by the OGLE team in Omega Cen. The phi_21 parameters are confined in a narrow strip for periods between 0.042 d and 0.07 d. Toward longer periods, there is an overlapping with the values obtained in the case of galactic stars. Toward shorter periods, the tendency to decreasing phi_21 values is also verified. A careful analysis should take more details in consideration: 1) Attention should be paid to the scatter in the distribution of the phi_21 parameters around 0.050 d. By analogy to Cepheid light curves, such a change can be the signature of a resonance between the fundamental mode and a higher overtone. 2) The small bunch of points above the progression at 0.038 d suggests a different light curve family. Since this group of stars shows a very small amplitude, it is possible that they are nonradial pulsators, not necessarily radial pulsators in a higher overtone. 3) The very low phi_21 value emphasizes the anomalous light curve of OGLEGC 26. The fact that such a light curve is observed in a Pop.II object is quite surprising, since V1719 Cyg and V798 Cyg (whose light curves are similar) are very probably Pop.I stars. In many cases, it seems that the phenomenon at the origin of the anomalous brightness increase should be carefully evaluated when dealing with pulsating star models.

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