WHAT IS THE DIFFERENCE? BLAZHKO AND NON-BLAZHKO RRab STARS AND THE SPECIAL CASE OF V123 IN M3

Jurcsik, J.; Smitola, P.; Hajdu, G.; Pilachowski, Catherine A.; Kolenberg, K.; Sódor, Á.; Fürész, Gábor; Moór, A.; Kun, Emma; Saha, Abhijit; Prakash, P.; Blüm, P.; Tóth, I.

doi:10.1088/2041-8205/778/2/l27

Cited by 2 publications

(2 citation statements)

References 20 publications

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“…Similar behaviour was observed in OGLE-BLG-RRLYR-12245 (Soszyński et al 2014). Jurcsik et al (2013) found a very interesting stable star in the globular cluster M3, which mimics the behaviour of a Blazhko star. These objects could play an important role in understanding the nature of the Blazhko effect.…”

Section: Introductionsupporting

confidence: 82%

Characteristics of bright ab-type RR Lyrae stars from the ASAS and WASP surveys

Skarka

2014

Monthly Notices of the Royal Astronomical Society

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In this article, we present results based on high-density, high-precision Wide-Angle Search for Planets (WASP) light curves supplemented with lower-precision photometry from the All-Sky Automated Survey (ASAS) for 268 RR Lyrae stars (176 regular, 92 Blazhko). Light curves were Fourier-decomposed and coefficients from WASP were transformed to the ASAS standard using 24 common stars. Coefficients were then compared with similar data from Galactic globular clusters, the Galactic bulge and the Large and Small Magellanic Clouds (LMC and SMC). Using Fourier coefficients, we also calculated physical parameters via standard equations from the literature. We confirmed the results of previous authors, including lower amplitudes and longer rise times for Blazhko stars. It was found that in the R 31 vs. R 21 plot the location of a star depends mainly on its metallicity and that Blazhko stars prefer a different location than modulation-free stars. Field and globular-cluster RR Lyrae variables have a different φ 21 and φ 31 than stars in the LMC, SMC and in Galactic bulge. Although there are some weak indications that Blazhko stars could prefer a slightly lower metallicity and shorter periods, no convincing proof was found. The most interesting highlight is the identification of a very recently proposed new group of metal-rich RR Lyrae type stars. These low-luminous, metal-strong variables, which comprise both Blazhko and regular stars, have shorter periods and about a 180 K higher temperature at constant (B − V ) 0 than the rest of the stars in the sample.

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Section: Introductionsupporting

confidence: 82%

Characteristics of bright ab-type RR Lyrae stars from the ASAS and WASP surveys

Skarka

2014

Monthly Notices of the Royal Astronomical Society

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“…In order to find some special cases showing the temporal appearance of the Blazhko phenomenon (see e.g. V114/M3 and OGLE-BLG-RRLYR-07605 Jurcsik et al 2013;Soszyński et al 2014), we investigated these outlying-position stars. In several cases, the photometry seems to be affected by crowding, and the light curve is very noisy.…”

Section: Introductionmentioning

confidence: 99%

RRab variables with identical light-curve shapes at different pulsation periods

Jurcsik

Juhász

2022

Monthly Notices of the Royal Astronomical Society

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In this paper, we report on the detection of RRab stars with quasi-identical-shape light curves but period differences as large as 0.05 − 0.21 d using the Galactic bulge data of the OGLE-IV survey. We have examined stars with shorter periods than the Oosterhoff I ridge of the bulge. These stars generally have smaller amplitudes and larger Fourier phase-differences than the typical bulge RRab stars have at the same period. Many of these ”anomalous” stars have good-quality light curves without any sign of the Blazhko modulation. Examining their Fourier parameters revealed that several of these stars show very similar light-curve to the typical bulge RR Lyrae. We found hundreds of quasi-identical-shape light-curve pairs with different periods between the ”anomalous”- and the ”normal”-position RRab stars based on the OGLE I-band data. The OGLE V-band, and the archive VVV and MACHO surveys Ks-, b- and r-band data of these stars were also checked for light-curve-shape similarity. Finally, 149 pairs with identical-shape light curves in each available photometric band were identified. Calculating the physical properties of the variables using empirical formulae, on average, −0.5 dex, −0.13 mag, 0.67, and 165 K differences between the [Fe/H], MV, R/R⊙, and Teff values of the members of the pairs are derived, being the short-period stars less metal-poor, fainter, smaller and hotter than the long-period variables. To explain the existence of variables with different physical properties and pulsation periods but with identical-shape light curves is a challenging task for modelling.

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WHAT IS THE DIFFERENCE? BLAZHKO AND NON-BLAZHKO RRab STARS AND THE SPECIAL CASE OF V123 IN M3

Cited by 2 publications

References 20 publications

Characteristics of bright ab-type RR Lyrae stars from the ASAS and WASP surveys

Characteristics of bright ab-type RR Lyrae stars from the ASAS and WASP surveys

RRab variables with identical light-curve shapes at different pulsation periods

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