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Monitoring Period Variations of Variable Stars using Precise Photometric Surveys

Published online by Cambridge University Press:  29 August 2019

Z. Mikulášek ,
M. Zejda ,
S. Hümmerich ,
J. Krtička ,
K. Bernhard ,
E. Paunzen ,
M. Skarka ,
S. de Villiers ,
M. Jagelka  and
V. Bakiş
Z. Mikulášek
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic email: [email protected]
M. Zejda
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic email: [email protected]
S. Hümmerich
Affiliation:
Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne, Berlin, Germany
J. Krtička
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic email: [email protected]
K. Bernhard
Affiliation:
Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne, Berlin, Germany
E. Paunzen
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic email: [email protected]
M. Skarka
Affiliation:
Astronomical Institute, Academy of Science of Czech Republic, Ondřejov, Czech Republic
S. de Villiers
Affiliation:
D. Burton Rd 61, Plumstead, Cape Town, South Africa
M. Jagelka
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic email: [email protected]
V. Bakiş
Affiliation:
Department of Astronomy & Space Physics, Akdeniz University, Antalya, Turkey
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Abstract

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The period variations of rotating, pulsating and eclipsing variable stars bear valuable astrophysical information about the presence of companions, evolutionary effects, and the inner structure of the stars. This talk described a universal method for de-trending and re-scaling precise photometric data (Kepler, MOST, CoRoT, OGLE, …) appropriate for period-change diagnostics of periodic variables. We demonstrated the potential of the method by analysing the period variability of one of the newly-identified Kepler magnetic chemically-peculiar (mCP) stars. We showed that, surprisingly, our target star displays near-sinusoidal changes in its observed light-variations, with a period of 2.85(6) years, which is apparently the result of the presence of a nearby stellar companion. The expected long-term changes of the rotational period, as have been observed in several mCP stars, have not been identified among the sample of Kepler mCP stars.

Keywords

Methods: statisticalsurveysstars: chemically peculiarstars: rotationstars: spotsbinaries: generalstars: low mass
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S339: Southern Horizons in Time-Domain Astronomy , November 2017 , pp. 110 - 113
Copyright
© International Astronomical Union 2019 

References

Hümmerich, S.Mikulášek, Z., Paunzen, E., Bernhard, K. et al. 2018, A&A, 619, A98Google Scholar
Mikulášek, Z. 2016, Contr. Sk. Pl. Obs. 26, 30Google Scholar
Mikulášek, Z., Krtička, J., Henry, G.W., Zverko, J., Žiňžovský, et al. 2008, A&A, 485, 585Google Scholar