On the Nature of the 41-Day Cycle of RR Lyrae

Detre, L.; Szeidl, B.

doi:10.1007/978-94-010-2590-4_6

Cited by 35 publications

(37 citation statements)

References 5 publications

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“…As many previous investigations show ( LaCluyzé et al 2004;Sódor et al 2007;Detre & Szeidl 1973;Szeidl 1976;Le Borgne et al 2014;Guggenberger et al 2012), the BL modulation itself can change on year-long time scale. Although the ASAS and MACHO data sets span rather long time bases, they typically do not contain sufficient number of data points to investigate such details.…”

Section: Discussionmentioning

confidence: 73%

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The SERMON project: 48 new field Blazhko stars and an investigation of modulation-period distribution

Skarka

Liška

Auer³

et al. 2016

A&A

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Aims. We investigated 1234 fundamental mode RR Lyrae stars observed by the All Sky Automated Survey (ASAS) to identify the Blazhko (BL) effect. A sample of 1547 BL stars from the literature was collected to compare the modulation-period distribution with stars newly identified in our sample. Methods. A classical frequency spectra analysis was performed using Period04 software. Data points from each star from the ASAS database were analysed individually to avoid confusion with artificial peaks and aliases. Statistical methods were used in the investigation of the modulation-period distribution. Results. Altogether we identified 87 BL stars (48 new detections), 7 candidate stars, and 22 stars showing long-term period variations. The distribution of modulation periods of newly identified BL stars corresponds well to the distribution of modulation periods of stars located in the Galactic field, Galactic bulge, Large Magellanic Cloud, and globular cluster M5 collected from the literature. As a very important by-product of this comparison, we found that pulsation periods of BL stars follow Gaussian distribution with the mean period of 0.54 ± 0.07 d, while the modulation periods show log-normal distribution with centre at log(P m [d]) = 1.78 ± 0.30 dex. This means that 99.7% of all known modulated stars have BL periods between 7.6 and 478 days. We discuss the identification of long modulation periods and show, that a significant percentage of stars showing long-term period variations could be classified as BL stars.

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Section: Discussionmentioning

confidence: 73%

“…Guggenberger et al 2012;Benkő et al 2014;Szabó et al 2014). In some BL stars, for example in RR Lyrae itself, the modulation reappears cyclically during an additional four-year cycle (Detre & Szeidl 1973;Le Borgne et al 2014;Poretti et al 2016). There are many more interesting features of the BL effect.…”

Section: Introductionmentioning

confidence: 98%

The SERMON project: 48 new field Blazhko stars and an investigation of modulation-period distribution

Skarka

Liška

Auer³

et al. 2016

A&A

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“…Only three light curves fulfil both requirements: two light curves of RS Boo and one of RR Lyr. This light curve of RR Lyr is, however, not representative for the large amplitude modulation, as these observations were obtained during the minima of the 4-year cycle (JD 2 434 553 -2 434 560), when the amplitude of the modulation was smaller than 0.1 mag (Detre & Szeidl 1973). The behaviour of RS Boo differs from other Blazhko type variables in many respects, it has an unusually short fundamental mode period, a very long modulation period and only reduced changes in its light curve shape.…”

Section: Light Curve Shapesmentioning

confidence: 72%

Blazhko stars: Always distorted?

Jurcsik¹,

Benkő²,

Szeidl³

2002

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Abstract.A reexamination of the amplitude ratios of the photometric and radial velocity changes of Blazhko RRab stars in their different Blazhko phases shows that a normal amplitude ratio occurs near the phase of maximum amplitude. Checking the Fourier parameters of maximum amplitude light curves with different methods proved, however, that none of these light curves can be regarded as a normal RR Lyrae type light curve.

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“…In the framework of the oblique magnetic rotator model of the Blazhko phenomenon any long-term cyclic behaviour seems to be a natural consequence of changes in the global magnetic field strength. Thus the four-year cycle of RR Lyrae may also indicate a similar explanation (Detre & Szeidl 1973). According to recent results (Jurcsik et al 2002) the light curves of RR Lyrae correspond to that of non-Blazhko RRab stars during the minimal phase of the four-year cycle, when the amplitude of the modulation is small.…”

Section: Magnetic Cyclesmentioning

confidence: 80%

“…This can be described as a decrease of the amplitude of the modulation and a jump in the Blazhko phase about every four years (Detre & Szeidl 1973). In contrast, XZ Dra shows surprising stability of the Blazhko phases during the entire time interval covered by observations, notwithstanding the changes of its Blazhko period.…”

Section: Stability Of the Blazhko Phasementioning

confidence: 92%

Long-term photometric behaviour of XZ Dra

Jurcsik¹,

Benkő²,

Szeidl³

2002

A&A

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Abstract. The extended photometry available for XZ Dra, a Blazhko-type RR Lyrae star, makes it possible to study its longterm behavior. It is shown that its pulsation period exhibits cyclic, but not strictly regular variations with ≈7200 d period. The Blazhko period (≈76 d) seems to follow the observed period changes of the fundamental mode pulsation with dP B /dP 0 = 7.7 × 10 4 gradient. A binary model cannot explain this order of period change of the Blazhko modulation, nevertheless it can be brought into agreement with the O-C data of the pulsation. The possibility of occurrence of a magnetic cycle is raised.

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On the Nature of the 41-Day Cycle of RR Lyrae

Cited by 35 publications

References 5 publications

The SERMON project: 48 new field Blazhko stars and an investigation of modulation-period distribution

The SERMON project: 48 new field Blazhko stars and an investigation of modulation-period distribution

Blazhko stars: Always distorted?

Long-term photometric behaviour of XZ Dra

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