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arxiv: 1108.5683 · v1 · pith:ETFGDQ4Anew · submitted 2011-08-29 · 🌌 astro-ph.SR

Non-Blazhko RR Lyrae Stars Observed with the KEPLER Space Telescope

J.M. Nemec (1 , 2) , R. Smolec (3) , J.M. Benko (4) , P. Moskalik (5) , K. Kolenberg (3 , 6) , R. Szabo (4)
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D.W. Kurtz (7) S. Bryson (8) E. Guggenberger (3) M. Chadid (9) Y.-B. Jeon (10) A. Kunder (12) A.C. Layden (13) K. Kinemuchi (8) L.L. Kiss (4) E. Poretti (14) J. Christensen-Dalsgaard (11) H. Kjeldsen (11) D. Caldwell (15) V. Ripepi (16) A. Derekas (4) J. Nuspl (4) F.Mullally (15) S.E. Thompson (15) W.J. Borucki (8) ((1) Department of Physics Astronomy Camosun College Victoria Canada (2) International Statistics Research Corporation Brentwood Bay Canada (3) Institut fur Astronomie University of Vienna Vienna Austria (4) Konkoly Obs.Hung.Acad.Sciences Budapest Hungary (5) Copernicus Astronomical Center Warsaw Poland (6) Harvard College Observatory Cambridge USA (7) Jeremiah Horrocks Institute of Astrophysics Univ. Central Lancashire UK (8) NASA Ames Research Center Moffett Field CA USA (9) Obs. Cote d'Azur Univ.Nice Sophia-Antipolis Parc Valrose France (10) Korea Astronomy Space Science Institute Daejeon Korea (11) Department of Physics Aarhus University Aarhus Denmark (12) Cerro Tololo Inter-American Observatory La Serena Chile (13) Physics Astronomy Dept. Bowling Green State University OH USA (14) Osservatorio Astronomico di Brera Merate Italy (15) SETI Institute/NASA Ames Research Center USA (16) INAF-Osservatorio Astronomico di Capodimonte Napoli Italy)
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classification 🌌 astro-ph.SR
keywords starslyraeobservedvaluescomparedkeplernon-blazhkoperiods
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This paper summarizes the main results of our recent study of the non-Blazhko RR Lyrae stars observed with the Kepler space telescope. These stars offer the opportunity for studying the stability of the pulsations of RR Lyrae stars and for providing a reference against which the Blazhko RR Lyrae stars can be compared. Of particular interest is the stability of the low-dispersion (sigma < 1mmag) light curves constructed from ~18,000 long-cadence (30-min) and (for FN Lyr and AW Dra) the ~150,000 short-cadence (1-min) photometric data points. Fourier-based [Fe/H] values and other physical characteristics are also derived. When the observed periods are compared with periods computed with the Warsaw non-linear convective pulsation code better agreement is achieved assuming pulsational L and M values rather than the (higher) evolutionary L and M values.

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