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RR Lyrae studies with Kepler: showcasing RR Lyr

Published online by Cambridge University Press:  18 February 2014

Katrien Kolenberg ,
Robert L. Kurucz ,
Robert Stellingwerf ,
James M. Nemec ,
Paweł Moskalik ,
Luca Fossati  and
Thomas G. Barnes
Katrien Kolenberg
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA email: [email protected] Institute of Astronomy, Leuven University, Celestijnenlaan 200d, 3001 Heverlee, Belgium
Robert L. Kurucz
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138, USA email: [email protected]
Robert Stellingwerf
Affiliation:
Stellingwerf Consulting, 11033 Mathis Mountain Rd SE Huntsville AL35803-2813, USA
James M. Nemec
Affiliation:
Dept. of Physics & Astronomy, Camosun College, Victoria, Br. Columbia, V8P 5J2, Canada
Paweł Moskalik
Affiliation:
Copernicus Astronomical Centre, ul.Bartycka 18, 00-716, Warsaw, Poland
Luca Fossati
Affiliation:
Argelander-Inst. für Astronomie der Univ. Bonn, Auf dem Hügel 71, D-53121, Bonn, Germany
Thomas G. Barnes
Affiliation:
The University of Texas at Austin, McDonald Observatory, 82 Mt. Locke Rd. McDonald Observatory, Texas, 79734, USA
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Abstract

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Four years into the Kepler mission, an updated review on the results for RR Lyrae stars is in order. More than 50 RR Lyrae stars in the Kepler field are observed with Kepler and each one of them can provide us with new insight into this class of pulsating stars. Ground-based spectroscopy of the Kepler targets allows us to narrow down their physical parameters. Previously, we already reported a 50% occurrence rate of modulation in the RRab stars, a large variety of modulation behavior, period doubling in several Blazhko stars, the detection of higher- overtone radial modes, probable non-radial modes and new types of multiple-mode RR Lyrae pulsators, among both the RRab and the RRc stars. In addition, the quasi-continuous photometry obtained over several years with Kepler allows one to observe changes in Blazhko behavior and additional longer cycles. These observations have sparked new theoretical modelling efforts. In this short paper we showcase RR Lyr itself. The star has been observed with Kepler in short cadence, and some remarkable features of its pulsation behavior are unveiled in this long-studied prototype, through the Kepler photometry and additional spectroscopic data.

Keywords

stars: variables: RR Lyraestars: individual: RR Lyrtechniques: photometrictechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 257 - 260
Copyright
Copyright © International Astronomical Union 2014 

References

Benkő, J., Kolenberg, K., Szabó, R., et al. 2010, MNRAS, 409, 1585Google Scholar
Benkő, J, Szabó, R. & Paparó, M. 2011, MNRAS, 417, 974Google Scholar
Buchler, J. R. & Kolláth, Z. 2011, ApJ, 731, 24Google Scholar
Çelik, L., Ekmekçi, F., Nemec, J., et al. 2012, arXiv: 1202.3607Google Scholar
Detre, L. & Szeidl, B. 1973, IBVS, 764Google Scholar
Dziembowski, W. A. & Mizerski, T. 2004, AcA, 54, 363Google Scholar
Gillet, D. 2013, A&A, 554, A46Google Scholar
Guggenberger, E. 2012, AN, 333, 1044Google Scholar
Guggenberger, E., Kolenberg, K., Nemec, J. M., et al. 2012, MNRAS 424, 649Google Scholar
Kinemuchi, K., 2013, arXiv: 1310.0544Google Scholar
Kolenberg, K., Szabó, R., Kurtz, D. W.et al., 2010a, ApJ, 713, L198Google Scholar
Kolenberg, K., Fossati, L., Shulyak, D., et al., 2010b, A&A 519, 64Google Scholar
Kolenberg, K., Bryson, S., Szabó, R., et al., 2011, MNRAS 411, 878Google Scholar
Kolláth, Z., Molnár, L., & Szabó, R., 2011, MNRAS 414, 1111CrossRefGoogle Scholar
Molnár, L., Kolláth, Z., Szabó, R., et al., 2012, ApJ, 757, L13Google Scholar
Moskalik, P., Smolec, R., Kolenberg, K., et al., 2012, arXiv: 1208.4251Google Scholar
Nemec, J. M., Smolec, R., Benkő, J. M., et al., 2011, MNRAS, 417, 1022Google Scholar
Nemec, J. M., Cohen, J. G., Ripepi, V., et al., 2013, ApJ, 773, 181Google Scholar
Plachy, E., Kolláth, Z., & Molnár, L., 2013, MNRAS 433, 3590CrossRefGoogle Scholar
Shibahashi, H. & Takata, M., 1995, ASP-CS, 83, 42Google Scholar
Smolec, R. & Moskalik, P., 2012, MNRAS 426, 108Google Scholar
Smolec, R., Moskalik, P., Kolenberg, K., et al., 2011, MNRAS, 414, 2950Google Scholar
Stellingwerf, R. F., Nemec, J. M., & Moskalik, P., 2013, arXiv: 1310.0543Google Scholar
Szabó, R., Kolláth, Z., Molnár, L., et al., 2010, MNRAS, 409, 1244Google Scholar
Szeidl, B., 1988, in: Kovács, G., Szabados, L., & Szeidl, B. (eds.), Multimode Stellar Pulsations (Budapest: Konkoly Observatory, Kultura), p. 45Google Scholar