Detection of 75+ pulsation frequencies in the<i>δ</i>Scuti star FG Virginis

Breger, M.; Lenz, P.; Antoci, V.; Guggenberger, E.; Shobbrook, R. R.; Handler, G.; Ngwato, B.; Rodler, F.; Rodrı́guez, E.; Coca, P. López de; Rolland, A.; Costa, V.

doi:10.1051/0004-6361:20042480

Cited by 94 publications

(110 citation statements)

References 18 publications

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“…Only 15 peaks are found with amplitudes higher than 0.5 mmag, but below the threshold of about 0.2 mmag, the number of detected peaks increases steeply in a nearly exponential way. This behaviour agrees with what is found by Breger et al (2005) for FG Vir, using the dataset provided by the longest ground-based photometric multisite campaign carried out to date for a δ Sct-type pulsator. However, in that case, the detection limit was only about 0.2 mmag.…”

Section: Distribution Of the Peakssupporting

confidence: 90%

Theγ Doradus CoRoT target HD 49434

Chapellier

Rodríguez‐López²,

Auvergne³

et al. 2010

A&A

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Context. HD 49434 is a bright (V = 5. m 75) and multiperiodic γ Dor-type pulsator that has been selected for the asteroseismic core programme of the CoRoT satellite.Aims. An extensive and detailed study has been carried out to investigate the pulsational content of this object on the basis of the 136.9 d (331291 useful datapoints) time series collected by the CoRoT satellite during the long-run LRa01 (October 2007-March 2008. Methods. The frequency analysis was carried out using the recently available software package SigSpec and Period04. Results. The results confirm HD 49434 as a complex pulsator with a very dense pulsation spectrum. A total of 1686 significant peaks are formally detected, essentially in the region below 15 d −1 . No significant pulsation peaks are detected for frequencies higher than 30 d −1 . Solar-type oscillations are not detected in this star. The reliability of such a high number of detected peaks has been investigated on the basis of two independent methods. As a result, we propose a total of 840 frequencies that can be assumed to be intrinsic to the star. Conclusions. The CoRoT mission provides very high-quality light curves and datasets, which are excellent for asteroseismic studies of complex pulsating stars beacause they allow investigation of the frequency content down to amplitude levels of a few μmag, unattainable with ground-based observations. In this way, hundreds of excited modes were detected in HD 49434. This is the first time that so many frequencies have been found in a γ Dor-type pulsator.

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Section: Distribution Of the Peakssupporting

confidence: 90%

Theγ Doradus CoRoT target HD 49434

Chapellier

Rodríguez‐López²,

Auvergne³

et al. 2010

A&A

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“…These stars can exhibit large numbers of simultaneous oscillation modes (Breger et al 2005;Catelan & Smith 2015, and references therein). Generally, δ Scutis are divided into two groups: high-amplitude δ Scutis (HADS, or AI Velorum stars: Bessell 1969) with amplitudes greater than ∼0.1 mag (Alcock et al 2000), and low-amplitude δ Scutis (LADS) with smaller amplitudes.…”

Section: δ Scutismentioning

confidence: 99%

The Catalina Surveys Southern periodic variable star catalogue

Drake

Djorgovski

Catelan

et al. 2017

Monthly Notices of the Royal Astronomical Society

159

133

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Here, we present the results from our analysis of 6 yr of optical photometry taken by the Siding Spring Survey (SSS). This completes a search for periodic variable stars within the 30 000 deg 2 of the sky covered by the Catalina Surveys. The current analysis covers 81 million sources with declinations between −20 • and −75 • with median magnitudes in the range 11 < V < 19.5. We find approximately 34 000 new periodic variable stars in addition to the ∼9000 RR Lyrae that we previously discovered in SSS data. This brings the total number of periodic variables identified in Catalina data to ∼110 000. The new SSS periodic variable stars mainly consist of eclipsing binaries, RR Lyrae, LPVs, RS CVn stars, δ Scutis, and Anomalous Cepheids. By cross-matching these variable stars with those from prior surveys, we find that ∼90 per cent of the sources are new discoveries and recover ∼95 per cent of the known periodic variables in the survey region. For the known sources, we find excellent agreement between our catalogue and prior values of luminosity, period, and amplitude. However, we find many variable stars that had previously been misclassified. Examining the distribution of RR Lyrae, we find a population associated with the Large Magellanic Cloud (LMC) that extends more than 20 • from its centre confirming recent evidence for the existence of a very extended stellar halo in the LMC. By combining SSS photometry with Dark Energy Survey data, we identify additional LMC halo RR Lyrae, thus confirming the significance of the population.

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“…The effects of rotation over the pulsation spectrum has been theoretically studied (e.g., Deupree 2011;Deupree et al 2012), as well as observed (e.g., Breger et al 1999bBreger et al , 2005Breger et al , 2012. The main effect of rotation is the splitting of the nonradial mode frequencies.…”

Section: The Effect Of Rotationmentioning

confidence: 99%

Pulsation analysis and its impact on primary transit modeling in WASP-33

Essen

Czesla

Wolter

et al. 2013

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Aims. To date, WASP-33 is the only δ Scuti star known to be orbited by a hot Jupiter. The pronounced stellar pulsations, showing periods comparable to the primary transit duration, interfere with the transit modeling. Therefore our main goal is to study the pulsation spectrum of the host star to redetermine the orbital parameters of the system by means of pulsation-cleaned primary transit light curves. Methods. Between August 2010 and October 2012 we obtained 457 h of photometry of WASP-33 using small and middle-class telescopes located mostly in Spain and in Germany. Our observations comprise the wavelength range between the blue and the red, and provide full phase coverage of the planetary orbit. After a careful detrend, we focus our pulsation studies in the high frequency regime, where the pulsations that mostly deform the primary transit exist. Results. The data allow us to identify, for the first time in the system, eight significant pulsation frequencies. The pulsations are likely associated with low-order p-modes. Furthermore, we find that pulsation phases evolve in time. We use our knowledge of the pulsations to clean the primary transit light curves and carry out an improved transit modeling. Surprisingly, taking into account the pulsations in the modeling has little influence on the derived orbital parameters. However, the uncertainties in the best-fit parameters decrease. Additionally, we find indications for a possible dependence between wavelength and transit depth, but only with marginal significance. A clear pulsation solution, in combination with an accurate orbital period, allows us to extend our studies and search for star-planet interactions (SPI). Although we find no conclusive evidence of SPI, we believe that the pulsation nature of the host star and the proximity between members make WASP-33 a promising system for further SPI studies.

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Detection of 75+ pulsation frequencies in theδScuti star FG Virginis

Cited by 94 publications

References 18 publications

Theγ Doradus CoRoT target HD 49434

Theγ Doradus CoRoT target HD 49434

The Catalina Surveys Southern periodic variable star catalogue

Pulsation analysis and its impact on primary transit modeling in WASP-33

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