The envelope of the power spectra of over a thousand <i>δ</i> Scuti stars

Forteza, S. Barceló; Cortés, T. Roca; García, R. A.

doi:10.1051/0004-6361/201731803

Cited by 31 publications

(19 citation statements)

References 48 publications

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“…This is in agreement with the predicted frequency distribution for the κ-mechanism (Dziembowski 1977) since we detected higher frequency modes for higher temperature δ Scuti stars. In fact, our relation is similar to that found by Barceló Forteza et al (2018). We also observed that old stars with low surface gravity present lower frequency ranges (see Eq.…”

Section: Discussionsupporting

confidence: 91%

“…Using the large amount of stellar data from space missions like CoRoT (Baglin et al 2006) or Kepler (Borucki et al 2010), the scientific community has also been looking for scaling relations for δ Scuti stars (e.g. Suárez et al 2014;García Hernández et al 2015;Michel et al 2017;Moya et al 2017;Barceló Forteza et al 2018;Bowman & Kurtz 2018). In a contribution to extend ensemble asteroseismology, Barceló Forteza et al (2018, -BF18 hereafter-) describe the envelope of δ Scuti stars with several metrics such as the number of modes (N env ), the frequency at Tables A.1 and A.2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.…”

Section: Introductionmentioning

confidence: 99%

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Unveiling the power spectra of δ Scuti stars with TESS

Forteza

Moya

Barrado

et al. 2020

A&A

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Thanks to high-precision photometric data legacy from space telescopes like CoRoT and Kepler, the scientific community could detect and characterize the power spectra of hundreds of thousands of stars. Using the scaling relations, it is possible to estimate masses and radii for solar-type pulsators. However, these stars are not the only kind of stellar objects that follow these rules: δ Scuti stars seem to be characterized with seismic indexes such as the large separation (Δν). Thanks to long-duration high-cadence TESS light curves, we analysed more than two thousand of this kind of classical pulsators. In that way, we propose the frequency at maximum power (νmax) as a proper seismic index since it is directly related with the intrinsic temperature, mass and radius of the star. This parameter seems not to be affected by rotation, inclination, extinction or resonances, with the exception of the evolution of the stellar parameters. Furthermore, we can constrain rotation and inclination using the departure of temperature produced by the gravity-darkening effect. This is especially feasible for fast rotators as most of δ Scuti stars seem to be.

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Section: Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Unveiling the power spectra of δ Scuti stars with TESS

Forteza

Moya

Barrado

et al. 2020

A&A

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“…This is also consistent with findings that Kepler δ Sct stars with higher T eff tend to have shorter dominant periods, i.e. a higher ν max (Balona & Dziembowski 2011;Barceló Forteza et al 2018).…”

Section: Interpretation Of the P-l Diagramsupporting

confidence: 92%

“…Many δ Sct stars were observed by Kepler during its fouryear nominal mission (e.g., Balona & Dziembowski 2011;Balona et al 2015;Bradley et al 2015;Moya et al 2017;Balona 2018;Barceló Forteza et al 2018;Bowman & Kurtz 2018). We have used the sample of about 2000 δ Sct stars identified by Murphy et al (2019) from Kepler long-cadence data.…”

Section: Kepler δ Sct Starsmentioning

confidence: 99%

The period–luminosity relation for δ Scuti stars using Gaia DR2 parallaxes

Ziaali

Bedding

Murphy

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have examined the period-luminosity (P-L) relation for δ Scuti stars using Gaia DR2 parallaxes. We included 228 stars from the catalogue of Rodriguez et al. (2000), as well as 1124 stars observed in the four-year Kepler mission. For each star we considered the dominant pulsation period, and used DR2 parallaxes and extinction corrections to determine absolute V magnitudes. Many stars fall along a sequence in the P-L relation coinciding with fundamental-mode pulsation, while others pulsate in shorter-period overtones. The latter stars tend to have higher effective temperatures, consistent with theoretical calculations. Surprisingly, we find an excess of stars lying on a ridge with periods half that of the fundamental. We suggest this may be due to a 2:1 resonance between the third or fourth overtone and the fundamental mode.

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“…An unexpected discovery was that many pulsating A and F stars are hybrid pulsators exhibiting both p and g modes (Grigahcène et al 2010;Balona & Dziembowski 2011;Uytterhoeven et al 2011), although pure pulsators of both types do exist (see e.g. Van Reeth et al 2015a;Bowman 2017;Barceló Forteza, Roca Cortés & García 2018;Li et al 2019a). The high incidence of hybrid stars remains unexplained, particularly if a single excitation mechanism should be responsible for both the p and g modes in hybrid stars (Balona, Daszyńska-Daszkiewicz & Pamyatnykh 2015;Xiong et al 2016).…”

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confidence: 99%

The first view of δ Scuti and γ Doradus stars with the TESS mission

Antoci

Cunha

Bowman

et al. 2019

Monthly Notices of the Royal Astronomical Society

105

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We present the first asteroseismic results for δ Scuti and γ Doradus stars observed in Sectors 1 and 2 of the TESS mission. We utilize the 2-min cadence TESS data for a sample of 117 stars to classify their behaviour regarding variability and place them in the Hertzsprung–Russell diagram using Gaia DR2 data. Included within our sample are the eponymous members of two pulsator classes, γ Doradus and SX Phoenicis. Our sample of pulsating intermediate-mass stars observed by TESS also allows us to confront theoretical models of pulsation driving in the classical instability strip for the first time and show that mixing processes in the outer envelope play an important role. We derive an empirical estimate of 74 per cent for the relative amplitude suppression factor as a result of the redder TESS passband compared to the Kepler mission using a pulsating eclipsing binary system. Furthermore, our sample contains many high-frequency pulsators, allowing us to probe the frequency variability of hot young δ Scuti stars, which were lacking in the Kepler mission data set, and identify promising targets for future asteroseismic modelling. The TESS data also allow us to refine the stellar parameters of SX Phoenicis, which is believed to be a blue straggler.

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The envelope of the power spectra of over a thousand δ Scuti stars

Cited by 31 publications

References 48 publications

Unveiling the power spectra of δ Scuti stars with TESS

Unveiling the power spectra of δ Scuti stars with TESS

The period–luminosity relation for δ Scuti stars using Gaia DR2 parallaxes

The first view of δ Scuti and γ Doradus stars with the TESS mission

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