FIRST
                    <i>KEPLER</i>
                    RESULTS ON RR LYRAE STARS

Kolenberg, K.; Szabo, Robert M.; Kurtz, D. W.; Gilliland, Ronald L.; Christensen‐Dalsgaard, J.; Kjeldsen, H.; Brown, Timothy M.; Benkő, J. M.; Chadid, M.; Derekas, A.; Criscienzo, M. Di; Guggenberger, E.; Kinemuchi, Karen; Kunder, Andrea; Kollath, Zoltán; Kopacki, G.; Moskalik, P.; Nemec, J. M.; Nuspl, J.; Silvotti, R.; Suran, M. D.; Borucki, W. J.; Koch, David; Jenkins, Jon M.

doi:10.1088/2041-8205/713/2/l198

Cited by 122 publications

(131 citation statements)

References 34 publications

(41 reference statements)

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“…The ratio f 2 / f 0 = 1.4908 ∼ 3/2 could be the signature of the period doubling bifurcation (Moskalik & Buchler 1990) first noticed in some RR Lyrae stars observed with Kepler (Kolenberg et al 2010).…”

Section: The Blazhko Frequency F Mmentioning

confidence: 67%

CoRoT light curves of RR Lyrae stars

Poretti¹,

Paparó

Deleuil

et al. 2010

A&A

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Context. The CoRoT (Convection, Rotation and planetary Transits) space mission provides a valuable opportunity to monitor stars with uninterrupted time sampling for up to 150 days at a time. The study of RR Lyrae stars, performed in the framework of the Additional Programmes belonging to the exoplanetary field, will particularly benefit from such dense, long-duration monitoring. Aims. The Blazhko effect in RR Lyrae stars is a long-standing, unsolved problem of stellar astrophysics. We used the CoRoT data of the new RR Lyrae variable CoRoT 101128793 ( f 0 = 2.119 d −1 , P = 0.4719296 d) to provide us with more detailed observational facts to understand the physical process behind the phenomenon. Methods. The CoRoT data were corrected for one jump and the long-term drift. We applied different period-finding techniques to the corrected timeseries to investigate amplitude and phase modulation. We detected 79 frequencies in the light curve of CoRoT 101128793. They have been identified as the main frequency f 0 and its harmonics, two independent terms, the terms related to the Blazhko frequency f m , and to several combination terms. Results. A Blazhko frequency f m = 0.056 d −1 and a triplet structure around the fundamental radial mode and harmonics were detected, as were a long-term variability on the Blazhko modulation. Indeed, the amplitude of the main oscillation is decreasing along the CoRoT survey. The Blazhko modulation is one of the smallest observed in RR Lyrae stars. Moreover, the additional modes f 1 = 3.630 and f 2 = 3.159 d −1 are detected. Taking its ratio with the fundamental radial mode into account, the term f 1 could be the identified as the second radial overtone. Detecting of these modes in horizontal branch stars is a new result obtained by CoRoT.

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Section: The Blazhko Frequency F Mmentioning

confidence: 67%

CoRoT light curves of RR Lyrae stars

Poretti¹,

Paparó

Deleuil

et al. 2010

A&A

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“…They belong to the asteroseismology dataset, part of which was analysed by us in Blomme et al (2010). Some first Kepler results on those RR Lyr stars are described in Kolenberg et al (2010).…”

Section: Number Of Variablesmentioning

confidence: 99%

Global stellar variability study in the field-of-view of theKeplersatellite

Debosscher

Blomme

Aerts

2011

A&A

113

114

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Aims. We present the results of an automated variability analysis of the Kepler public data measured in the first quarter (Q1) of the mission. In total, about 150 000 light curves have been analysed to detect stellar variability and to identify new members of known variability classes. We also focus on detecting variables present in eclipsing binary systems, given the strong constraints on stellar fundamental parameters they can provide.Methods. The methodology we use here is based on the automated variability classification pipeline, which was previously developed for and successfully applied to the CoRoT exofield database and to the limited subset of a few thousand Kepler asteroseismology light curves. We use a Fourier decomposition of the light curves to describe their variability behaviour and use the resulting parameters to perform a supervised classification. Several improvements were made, including a separate extractor method to detect the presence of eclipses when other variability is present in the light curves. We also included two new variability classes compared to previous work: variables showing signs of rotational modulation and of activity. Results. Statistics are given on the number of variables and the number of good candidates per class. A comparison is made with results obtained for the CoRoT exoplanet data. We present some special discoveries, including variable stars in eclipsing binary systems. Many new candidate non-radial pulsators are found, mainly δ Sct and γ Dor stars. We studied those samples in more detail by using 2MASS colours, and the full classification results are made available as an online catalogue.

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“…Ultra-precise data provided by these space telescopes allowed findings of, say, cycle-to-cycle variations now known as period doubling Kolenberg et al 2010;Benkő et al 2010) or longterm changes in the Blazhko effect and excitation of additional modes (Poretti et al 2010;Chadid et al 2010;Guggenberger et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

Skarka

2014

A&A

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Aims. Period study of 321 fundamental mode RR Lyrae type stars (RRab), which had appropriate data in ASAS and SuperWASP surveys, was performed to complement and extend the list of known Blazhko stars in galactic field with bright stars up to 12.5 mag in maximum light.Methods. An individual approach was applied to each studied star. Permanent visual supervision was maintained to each procedure in data analysis (data cleaning, frequency spectra examination) to avoid missing any possible sign of the Blazhko effect. Period analysis was performed using Period04 software. Results. We found 100 stars to be definitely modulated. In 25 cases, previously unknown modulation was revealed and 8 new candidates for Blazhko stars were identified. Their modulation needs to be confirmed. In 18 previously found Blazhko stars, no modulation was detectable. Multiple modulation was revealed for eight stars that were previously proposed to show simple modulation. In total, there were twelve stars with some peculiarity in their modulation in the sample. This brings the incidence rate of multiple/irregularlymodulated stars to 12%. The ratio of the modulation periods of five of the double-modulated stars was within the ratios of small integers. One of stars studied, IK Hya, showed a very interesting frequency spectrum, which we interpret as changing Blazhko period between 71.81 and 75.57 days and an additional 1403-day-long cycle analogous to a four-year cycle of the prototype RR Lyr. The limits of the shorter period produce a beating period that is approximately twice as big as a 1403-day period. The newly revealed Blazhko star RZ CVn seems to undergo changes in the amplitude of the modulation, as well as in the basic pulsation and Blazhko periods. We found that the incidence rate of the Blazhko RR Lyraes is at least 31%, more likely even higher. It was also found that the majority of the Blazhko variables show triplet structures in their frequency spectra and that in 89% of these cases, the peak with larger amplitude is on the right-hand side of the main pulsation component.

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FIRST KEPLER RESULTS ON RR LYRAE STARS

Cited by 122 publications

References 34 publications

CoRoT light curves of RR Lyrae stars

CoRoT light curves of RR Lyrae stars

Global stellar variability study in the field-of-view of theKeplersatellite

Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

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