Long-term photometric monitoring of Messier 5 variables – I. Period changes of RR Lyrae stars

@article{Szeid2010LongtermPM,
  title={Long-term photometric monitoring of Messier 5 variables – I. Period changes of RR Lyrae stars},
  author={B. Szeid and Zs. Hurta and Johanna Jurcsik and Christine M. Coutts Clement and M. Lovas},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2010},
  volume={411},
  pages={1744-1762}
}
The period changes of 86 M5 RR Lyrae stars have been investigated on a 100-yr time base. The published observations have been supplemented by archival Asiago, Konkoly and Las Campanas photographic observations obtained between 1952 and 1993. About two-thirds of the O - C diagrams could be fitted by a straight line or a parabola. 21 RR Lyrae stars have increasing, 18 decreasing and 16 constant period. The mean rates of period change of these variables are: 〈β〉 = 〈P〉 = -0.006 ± 0.162 d Myr -1… 

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References

SHOWING 1-10 OF 32 REFERENCES

BV Photometry of the RR Lyrae Variables of the Globular Cluster M3

We present new BV CCD photometry, light curves, and ephemerides for 207 RR Lyrae variables in the globular cluster M3. For 127 of these we present observed minus calculated (O-C) diagrams. The data

Stellar evolution and period changes in RR Lyrae stars

The observed secular period changes of RR Lyrae stars in five globular clusters have been compared with those predicted by synthetic models of the horizontal branch (HB). It is shown that most of the

CCD Photometry of RR Lyrae Stars in M5 as a Test for the Pulsational Scenario

In this paper we present new CCD investigations of RR Lyrae pulsators in the Oo.I globular cluster M5. B V curves of light for 15 RR Lyrae are presented. With the addition of further 11 curves of

RR Lyrae Variables in the Globular Cluster M55. The First Evidence for Nonradial Pulsations in RR Lyrae Stars

We present the results of a photometric study of RR Lyrae variables in the field of the globular cluster M55. We have discovered nine new RR Lyrae stars, increasing the number of known RR Lyrae

Stellar evolution through the ages: period variations in galactic RRab stars as derived from the GEOS database and TAROT telescopes

Context. The theory of stellar evolution can be more closely tested if we have the opportunity to measure new quantities. Nowadays, observations of galactic RR Lyr stars are available on a time

PHOTOMETRY OF RR LYRAE VARIABLES IN THE GLOBULAR CLUSTERS M5 AND M92

Visual photometry at V and i has been obtained for five RR Lyrae variables in the extremely metal-poor globular cluster M92 and eight in the cluster M5, of intermediate metallicity, for use in a

The distance to M5 from its RR Lyrae variables

We have applied a variation of the Baade-Wesselink method to four RR Lyrae variables in the moderately metal-poor globular cluster M5. The radial velocity curves are from observations with the 200

Period Changes in ω Centauri RR Lyrae Stars

A century of observations of ω Centauri allows us to accurately follow the period changes of a large sample of variable stars. Although the period changes are composed of monotone and irregular

Stellar evolution and variability in the pre-ZAHB phase

Context. One of the most dramatic events in the life of a low-mass star is the He flash, which takes place at the tip of the red giant branch and is followed by a series of secondary flashes before

An RR Lyrae period shift in terms of the Fourier parameter Phi sub 31

The Fourier phase parameter Phi sub 31 has been determined for RRc stars in five globular clusters, NGC 6171, M5, M3, M53, and M15. The results indicate that the RRc stars in a given cluster show a