Analysing periodic amplitude changes in RR Lyrae and other types of variable stars

Guggenberger, E.; Kolenberg, K.; Breger, M.

doi:10.1088/1742-6596/118/1/012056

Cited by 3 publications

(4 citation statements)

References 6 publications

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“…The current work is related to that earlier work in the following way: It is found that the phase and amplitude dynamics of the second component of the earlier description can be approximately generated by adding together two constant amplitude sine waves, one with frequency ω 1 and a second of lower amplitude with frequency ω 1 + ω B . This was noted previously by Guggenberger et al (2008) who found this type of phase and amplitude behavior in several RR Lyrae stars and attributed it to this type of beating process. The first component corresponds to PO1a in the current model.…”

Section: Relation To Earlier Work By the Authorsupporting

confidence: 82%

“…There have been several previous papers in support of the beating-modes model, but the current work goes much further in terms of finding a simple model that actually provides a remarkably good fit to the observed Blazhko data, including the mysterious motion and disappearance of the socalled bump feature. Guggenberger et al (2008), building on earlier work by Breger & Kolenberg (2006), proposed a test of the phasing behavior in an effort to determine if beating was responsible for the Blazhko effect. They applied this to the two well-observed Blazhko RR Lyrae stars SS For and RR Lyr, with results consistent with the beating of two oscillations.…”

Section: Introductionmentioning

confidence: 99%

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Is the Blazhko Effect the Beating of a Near-Resonant Double-Mode Pulsation?

Bryant

2015

ApJ

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In this paper it is shown that the Blazhko effect may result from a near-resonant type of multi-mode pulsation, where two (or sometimes more) periodic oscillations with slightly different frequencies gradually slip in phase, producing a beat frequency type of modulation. Typically one of these oscillations is strongly non-sinusoidal. Two oscillations are sufficient for the standard Blazhko effect; additional oscillations are needed to explain multi-frequency modulation. Previous work on this hypothesis by Arthur N. Cox and others is extended in this paper by developing a simple (non-hydro) model that can accurately reproduce several important features found in Kepler data for RR Lyr, including the pulsation waveform, the upper and lower Blazhko envelope functions and the motion, disappearance and reappearance of the bump feature. The non-sinusoidal oscillation is probably generated by the fundamental mode and the other oscillations are probably generated by nonradial modes. This model provides an explanation for the strong asymmetry observed in the side peak spectra of most RR Lyrae stars. The motion and disappearance of the bump feature are shown to be an illusion, just an artifact of combining the oscillations. V445 Lyr is presented as an example with dual modulation. The mysterious double-maxima waveform observed for this star is explained, providing additional strong evidence that this beating-modes hypothesis is correct. Problems with other recent explanations of the Blazhko effect are discussed in some detail.

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Section: Relation To Earlier Work By the Authorsupporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

Is the Blazhko Effect the Beating of a Near-Resonant Double-Mode Pulsation?

Bryant

2015

ApJ

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“…Similar behavior was observed in CoRoT 104190253 (V620 Oph) by Benko (2016), who discovered the previous misclassification of the star and concluded that it was in fact an RRab star displaying the Blazhko effect. Guggenberger et al (2008) also observed similar variation in f 0 for RR Lyrae (and SS Fornacis) and associated it with the beating phenomenon. However, in RRd stars, two modes are already pulsating simultaneously, and in addition to that, the Blazhko modulation is observed.…”

Section: Resultssupporting

confidence: 55%

Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF

Varma,

Ngeow

2024

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RRd stars are a subclass of RR Lyrae stars that pulsate simultaneously in the fundamental and the first-overtone radial modes. We report the analysis of 10 RRd stars discovered in the Sloan Digital Sky Survey (SDSS) Stripe 82 region of the Galactic halo using SDSS and Zwicky Transient Facility data. By combining the two data sets, we constructed ∼23 yr long lightcurves in gri bands, and conclude that out of 10, 9 were the classical RRd stars and 1 was the anomalous RRd star. We also observed the long-term variation, the Blazhko effect, in 3 classical RRd stars out of 10 stars, giving an incidence rate of 30%. The shortest Blazhko period observed was 226.4 ± 0.8 days and the longest was 2799 ± 75 days.

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“…On the other hand, it is also possible that the triplet structure is an artefact appearing due to amplitude variation. However, Guggenberger et al (2008) demonstrated that the triplet (or effectively a doublet due to the weak central frequency) in the data from Kilkenny et al (1999) indeed is real.…”

Section: Multiplet Structurementioning

confidence: 99%

Amplitude variation and multiplet structures: Is PG1605+072 a slow rotator?

Langfellner,

Schuh,

MSST

et al. 2012

Preprint

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The subdwarf B star PG 1605+072, with an unusually low log (g/cm s −2 ) ∼ 5.3, shows a high number of non-radial pulsation modes, making it a promising candidate for asteroseismology. This could allow probing the star's interior to gain important insights in its structure and evolution. Comparison of previous work conducted over the last decade shows clear amplitude variation and hints of frequency variation. We analyse white light photometric data of the Multi-Site Spectroscopic Telescope (MSST) and Whole Earth Telescope (WET) XCov22 campaigns using prewhitening techniques and O−C diagrams. A total of 85 significant frequencies are identified, among them more than 20 frequency sums and harmonics. Moreover, it is shown that the main mode's amplitude varies like a sine with a period of ∼ 630 d, indicative of long-term beating. Strong hints for the existence of frequency multiplets support the hypothesis that PG 1605+072 is a slow rotator with V eq 0.9 km s −1 , contrary to previous claims. Existing asteroseismic models mainly suggest that the star possesses a high mass of ∼ 0.7 M ⊙ , presuming the main pulsation mode to be radial. This calls for an alternate formation channel.

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Analysing periodic amplitude changes in RR Lyrae and other types of variable stars

Cited by 3 publications

References 6 publications

Is the Blazhko Effect the Beating of a Near-Resonant Double-Mode Pulsation?

Is the Blazhko Effect the Beating of a Near-Resonant Double-Mode Pulsation?

Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF

Amplitude variation and multiplet structures: Is PG1605+072 a slow rotator?

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