THE ALL-SKY GEOS RR Lyr SURVEY WITH THE TAROT TELESCOPES: ANALYSIS OF THE BLAZHKO EFFECT

Borgne, J. F. Le; Klotz, A.; Poretti, E.; Boër, M.; Butterworth, N.; Dumont, M.; Dvorak, Shawn; Hambsch, F. J.; Hund, F.; Kugel, F.; Vandenbroere, Jacqueline; Vilalta, J. M.

doi:10.1088/0004-6256/144/2/39

Cited by 21 publications

(23 citation statements)

References 40 publications

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“…No good quality light curve of RZ Lyr was published between 1972 and 2010. However, thanks to the efforts of mainly the GEOS 4 and Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne (BAV) 5 observers the maximum times available in the GEOS data base cover this period (Agerer & Huebscher 1996, 2000, 2003; Agerer, Dahm & Huebscher 2001; Huebscher 2005, 2011; Huebscher, Paschke & Walter 2005, 2006; Le Borgne, Klotz & Boër 2005, 2006a,b, 2007b,c, 2008a,b; Huebscher, Steinbach & Walter 2008, 2009; Le Borgne et al 2008c; Le Borgne, Klotz & Boër 2009a,b, 2010, 2011; Huebscher et al 2010; Samolyk 2010, 2011).…”

Section: Observations Of Rz Lyrmentioning

confidence: 99%

An extensive photometric study of the Blazhko RR Lyrae star RZ Lyr*

Jurcsik

Sódor

Hajdu

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Abstract The analysis of recent, extended multicolour CCD and archive photoelectric, photographic and visual observations has revealed several important properties of RZ Lyr, an RRab-type variable exhibiting large-amplitude Blazhko modulation. On the time base of ∼110 yr, a strict anticorrelation between the pulsation- and modulation-period changes is established. The light curve of RZ Lyr shows a remarkable bump on the descending branch in the small-amplitude phase of the modulation, similarly to the light curves of bump Cepheids. We speculate that the stellar structure temporally suits a 4:1 resonance between the periods of the fundamental and one of the higher order radial modes in this modulation phase. The light-curve variation of RZ Lyr can be correctly fitted with a two-modulation-component solution; the 121-d period of the main modulation is nearly but not exactly four times longer than the period of the secondary modulation component. Using the inverse photometric method, the variations in the pulsation-averaged values of the physical parameters in different phases of both modulation components are determined.

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Section: Observations Of Rz Lyrmentioning

confidence: 99%

An extensive photometric study of the Blazhko RR Lyrae star RZ Lyr*

Jurcsik

Sódor

Hajdu

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…An extensive study of the Blazhko effect is presented in the paper of Le Borgne et al (2012), which is based on observations made with TAROT telescopes (Klotz et al 2008(Klotz et al , 2009. Le Borgne et al (2012) also made use of O − C information stored in the A&A 562, A90 (2014) GEOS RR Lyr database (Le Borgne et al 2007) and gave a list of galactic field Blazhko stars. A regularly updated database of known Blazhko RR Lyraes situated in the galactic field (BlaSGalF, Skarka 2013) 2 recently contained about 270 objects.…”

Section: Introductionmentioning

confidence: 99%

“…The most conspicuous feature of the Blazhko effect is the change in amplitude of the light variations, which can be Borgne et al 2012;Guggenberger et al 2012).…”

Section: Introductory Remarks On the Blazhko Effectmentioning

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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“…Smith 1995;Le Borgne et al 2012), but an overall list has not been available until now. Such a list allows observers and all interested astronomers to quickly check the Blazhko instability of the star in one place and see whether the star needs further observations or not.…”

Section: Introductionmentioning

confidence: 99%