White-Dwarf Asteroseismology With the Kepler Space Telescope

Córsico, Alejandro H.

doi:10.3389/fspas.2020.00047

Cited by 31 publications

(20 citation statements)

References 128 publications

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“…White-dwarf asteroseismology has undergone substantial progress, thanks to ground-based observations, mainly with the time-series photometric observations of the "Whole Earth Telescope" (WET; Nather et al 1990), followed by the spectral observations of the Sloan Digital Sky Survey (SDSS, York et al 2000), and in recent years by the availability of space missions that provide unprecedented high-quality data. Indeed, the Kepler satellite, both the main mission (Borucki et al 2010) and the K2 mode (Howell et al 2014), allowed the study of 32 ZZ Ceti stars and two V777 Her stars (Østensen et al 2011;Hermes et al 2017a,b;Córsico 2020), until it was out of operation by October 2018. The successor of Kepler is the Transiting Exoplanet Survey Satellite (TESS, Ricker et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS: I. Asteroseismology of the GW Vir stars RX J2117+3412, HS 2324+3944, NGC 6905, NGC 1501, NGC 2371, and K 1-16

Córsico,

Uzundag,

Kepler

et al. 2020

Preprint

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Section: Introductionmentioning

confidence: 99%

Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS: I. Asteroseismology of the GW Vir stars RX J2117+3412, HS 2324+3944, NGC 6905, NGC 1501, NGC 2371, and K 1-16

Córsico,

Uzundag,

Kepler

et al. 2020

Preprint

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“…Figure 15 demonstrates that the two techniques are found to be in good agreement within a few percent for hydrogen-atmosphere (DA) white dwarfs (Tremblay et al 2019;Genest-Beaulieu and Bergeron 2019). The advent of continuous observations from space (e.g., CoRoT, Kepler, and TESS missions) has also boosted the field of white dwarf asteroseismology (Co ´rsico et al 2019;Co ´rsico 2020). Asteroseismology of pulsating white dwarfs has also been successful in deriving accurate masses that are generally in agreement with spectroscopy and photometry (Romero et al 2012;Hermes et al 2017;Giammichele et al 2018).…”

Section: White Dwarfsmentioning

confidence: 86%

Weighing stars from birth to death: mass determination methods across the HRD

Serenelli

Weiß

Aerts

et al. 2021

Astron Astrophys Rev

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The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between ½0:3; 2% for the covered mass range of M 2 ½0:1; 16 M , 75% of which are stars burning hydrogen in their core and the other 25% covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a ''mass-ladder'' for stars.

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“…ZZ Ceti variables in detached white dwarf plus mainsequence (MS) binaries have also become known (Pyrzas et al 2015). For comprehensive reviews of the characteristics of pulsating white dwarf stars, we invite the reader to consult the papers of Winget & Kepler (2008), Fontaine & Brassard (2008), Althaus et al (2010), Córsico et al (2019), andCórsico (2020).…”

Section: Introductionmentioning

confidence: 99%

“…The study of white dwarf stars contributes to the understanding of star formation and evolution, and in addition, by investigating their interiors, we can use them as cosmic laboratories to study the behaviour of material under extreme pressure and temperature conditions, and measure the age of their parent stellar population. We are aware of 260 ZZ Ceti stars (Córsico 2020) currently; nonetheless, only a limited number of pulsation modes are known for most of them, usually the results of the short discovery runs. This is mainly because of the faintness of these objects and the limited access of ground-based telescopes large enough for follow-up observations.…”

Section: Introductionmentioning

confidence: 99%

“…During the nominal Kepler mission and its K2 extension, 81 ZZ Ceti stars were observed, and the analyses of 32 of them have been published so far (see e.g. Hermes et al 2017a,b;Bell et al 2017b;Córsico 2020). In addition, published results have already demonstrated the value of the TESS data, focussing on a DBV star (Bell et al 2019), several ZZ Ceti stars (Bognár et al 2020;Althaus et al 2020), and GW Vir variables (Córsico et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Exploring the pulsational properties of two ZZ Ceti stars

Bognár

Kalup

Sódor

2021

A&A

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Context. We continued our ground-based observing project with the season-long observations of ZZ Ceti stars at the Konkoly Observatory. Our present targets are the newly discovered PM J22299+3024 and the already known LP 119–10 variables. LP 119–10 was also observed by the TESS space telescope in 120-second cadence mode. Aims. Our main aims are to characterise the pulsation properties of the targets and extract pulsation modes from the data for asteroseismic investigations. Methods. We performed a standard Fourier analysis of the daily, weekly, and entire data sets, together with test data of different combinations of weekly observations. We then performed asteroseismic fits utilising the observed and the calculated pulsation periods. For the calculations of model grids necessary for the fits, we applied the 2018 version of the White Dwarf Evolution Code. Results. We derived six possible pulsation modes for PM J22299+3024 and five plus two TESS pulsation frequencies for LP 119–10. We note that further pulsation frequencies may be present in the data sets, but we found their detection ambiguous, so we omitted them from the final frequency list. Our asteroseismic fits of PM J22299+3024 give 11 400 K and 0.46 M⊙ for the effective temperature and the stellar mass, respectively. The temperature is ≈800 K higher, while the mass of the model star is exactly the same as was earlier derived by spectroscopy. Our model fits of LP 119–10 put the effective temperature in the range of 11 800−11 900 K, which is again higher than the spectroscopic 11 290 K value. Moreover, our best model solutions give M* = 0.70 M⊙ mass for this target, which is near to the spectroscopic value of 0.65 M⊙ and likewise in the case of PM J22299+3024. The seismic distances of our best-fit model stars agree with the Gaia astrometric distances of PM J22299+3024 and LP 119–10 within the errors, validating our model results.

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White-Dwarf Asteroseismology With the Kepler Space Telescope

Cited by 31 publications

References 128 publications

Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS: I. Asteroseismology of the GW Vir stars RX J2117+3412, HS 2324+3944, NGC 6905, NGC 1501, NGC 2371, and K 1-16

Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS: I. Asteroseismology of the GW Vir stars RX J2117+3412, HS 2324+3944, NGC 6905, NGC 1501, NGC 2371, and K 1-16

Weighing stars from birth to death: mass determination methods across the HRD

Exploring the pulsational properties of two ZZ Ceti stars

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