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Photometric Variability of the mCP Star CS Vir: Evolution of the Rotation Period

  • D. Ozuyar (a1) (a2), H. T. Sener (a3) and I. R. Stevens (a2)
Abstract

The aim of this study is to accurately calculate the rotational period of CS Vir by using STEREO observations and investigate a possible period variation of the star with the help of all accessible data. The STEREO data that cover 5-yr time interval between 2007 and 2011 are analysed by means of the Lomb–Scargle and Phase Dispersion Minimization methods. In order to obtain a reliable rotation period and its error value, computational algorithms such as the Levenberg–Marquardt and Monte Carlo simulation algorithms are applied to the data sets. Thus, the rotation period of CS Vir is improved to be 9.29572(12) d by using the 5-yr of combined data set. Also, the light elements are calculated as HJD max = 2454715.975(11) + 9d · 29572(12) × E + 9d · 78(1.13) × 10 − 8 × E 2 by means of the extremum times derived from the STEREO light curves and archives. Moreover, with this study, a period variation is revealed for the first time, and it is found that the period has lengthened by 0.66(8) s y−1, equivalent to 66 s per century. Additionally, a time-scale for a possible spin-down is calculated around τSD ~ 106 yr. The differential rotation and magnetic braking are thought to be responsible of the mentioned rotational deceleration. It is deduced that the spin-down time-scale of the star is nearly three orders of magnitude shorter than its main-sequence lifetime (τMS ~ 109 yr). It is, in return, suggested that the process of increase in the period might be reversible.

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Corresponding author
4 Email: dozuyar@ankara.edu.tr
References
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