Multiperiodic RR Lyrae stars in the Galactic Bulge and the SMC

Mizerski, Tomasz

doi:10.1017/s0252921100010460

Cited by 2 publications

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“…The data are much more scarce for RRc stars; these stars were not extensively observed from space yet. Incidence rates are clearly smaller; those reported in the analyses of ground-based data are below 10 % (Nagy & Kovács, 2006;Mizerski, 2003).…”

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confidence: 66%

The Blazhko Effect

Smolec¹

2016

Preprint

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We review the recent progress in our understanding of the Blazhko effect in RR Lyrae stars.1 Introduction RR Lyrae stars are low-mass, typically metal poor, Population II stars. In the HR diagram, they are located within the so-called classical instability strip. Their apparent large-amplitude brightness changes are due to oscillation in the radial modes: radial fundamental mode (RRab stars) or radial first overtone mode (RRc stars). Simultaneous pulsation in these two radial modes is also possible (RRd stars). As excellent distance indicators, RR Lyrae stars are invaluable in studies of the Galactic structure and evolution.RR Lyrae stars are considered a textbook examples of simple, single-periodic radially pulsating stars. In fact, they are much more complex and display phenomena that are not well understood. Recent analyses of top-quality ground-based and space-based photometry revealed that additional low-amplitude variability, attributed to nonradial modes, may be common, at least in RRc stars -see e.g. Szabó et al. (2014); Moskalik et al. (2015); Netzel et al. (2015); for recent review, see Moskalik (2014).Another puzzling effect, the Blazhko modulation, was discovered more than hundred years ago (Blažko, 1907). It manifests as a quasi-periodic modulation of pulsation amplitude and/or phase. Its cause remains a mystery. These proceedings are focused on recent progress in our understanding of the Blazhko phenomenon. Blazhko effect: new discoveries from the ground-based and space-based observationsBlazhko effect is one of the most stubborn problems of stellar astrophysics. Many efforts are devoted to study the phenomenon, both on observational side and on theoretical side. Until recently, the observations were limited to the ground-based only. RR Lyr, eponym of the class and a Blazhko variable, was a target of multi-site campaign (Kolenberg et al., 2006). Many Blazhko variables were discovered in the data gathered by the photometric sky surveys such as OGLE (e.g., Mizerski, 2003;Soszyński et al., 2011a) or MACHO (e.g. Alcock et al., 2003). Excellent observations, allowing detailed study of the light curve changes during the Blazhko cycle, were collected by the Konkoly Blazhko Survey (e.g., Jurcsik et al., 2008;Sódor et al., 2011). These observations also revealed that the Blazhko phenomenon might be common, at least in RRab stars, as it was detected in nearly 50 % of RRab stars for which high-quality photometry was gathered (Jurcsik et al., 2009).

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confidence: 66%

The Blazhko Effect

Smolec¹

2016

Preprint

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“…All these add to the flavor to the Blazhko phenomenon and could be instrumental at some stage in searching for the physical model, but the more general pattern described above constitutes the observational framework the models should deal with. > 7% * Sources: [70](SMC), [1](LMC), [46](SMC), [53](LMC), [19](Bulge), [77](Gal. Field), [51](compilation) † Note: See comments in text for the expected increase of the incidence rates for Galactic RR Lyrae stars and for the estimation of the rates in the case of multiple sources for the statistics.…”

Section: Observational Status -A Quick Glance Rr Lyrae Starsmentioning

confidence: 99%

The Blazhko Effect

Kovács¹

2009

AIP Conference Proceedings

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Current status of (the lack of) understanding Blazhko effect is reviewed. We focus mostly on the various components of the failure of the models and touch upon the observational issues only at a degree needed for the theoretical background. Attention is to be paid to models based on radial mode resonances, since they seem to be not fully explored yet, especially if we consider possible non-standard effects (e.g., heavy element enhancement). To aid further modeling efforts, we stress the need for accurate time-series spectral line analysis to reveal any possible non-radial component(s) and thereby let to include (or exclude) non-radial modes in explaining the Blazhko phenomenon.Comment: 12 pages, 3 figures, paper presented at a conference held in Santa Fe, NM, USA, May 31 - June 5, 2009. To appear in 'Stellar Pulsation: Challenges for Theory and Observation', AIP, Eds.: J. Guzik and P. Bradle

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Multiperiodic RR Lyrae stars in the Galactic Bulge and the SMC

Cited by 2 publications

References 2 publications

The Blazhko Effect

The Blazhko Effect

The Blazhko Effect

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