KIC 10080943: An eccentric binary system containing two pressure- and gravity-mode hybrid pulsators

Schmid, V. S.; Tkachenko, A.; Aerts, C.; Degroote, P.; Bloemen, S.; Murphy, Simon J.; Reeth, T. Van; Pápics, P. I.; Bedding, Timothy R.; Keen, Matthew A; Prša, Andrej; Menu, J.; Debosscher, J.; Hrudková, M.; Smedt, K. De; Lombaert, R.; Németh, P.

doi:10.1051/0004-6361/201526945

Cited by 56 publications

(69 citation statements)

References 70 publications

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“…We apply our methodology to three g-mode pulsating stars observed with Kepler. All targets are binary systems with at Van Reeth et al (2016), which have been previously studied in the literature (Pápics et al 2013;Schmid et al 2015;Schmid & Aerts 2016;Pápics et al 2017). The relevant spectroscopic and binary parameters are listed in Table 5.…”

Section: Kepler Samplementioning

confidence: 99%

Binary asteroseismic modelling: isochrone-cloud methodology and application toKeplergravity mode pulsators

Johnston

Tkachenko

Aerts

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The simultaneous presence of variability due to both pulsations and binarity is no rare phenomenon. Unfortunately, the complexities of dealing with even one of these sources of variability individually means that the other signal is often treated as a nuisance and discarded. However, both types of variability offer means to probe fundamental stellar properties in robust ways through asteroseismic and binary modelling. We present an efficient methodology that includes both binary and asteroseismic information to estimate fundamental stellar properties based on a grid-based modelling approach. We report parameters for three gravity mode pulsating Kepler binaries , such as mass, radius, age, as well the mass of the convective core and location of the overshoot region. We discuss the presence of parameter degeneracies and the way our methodology deals with them. We provide asteroseismically calibrated isochrone-clouds to the community; these are a generalisation of isochrones when allowing for different values of the core overshooting in the two components of the binary.

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Section: Kepler Samplementioning

confidence: 99%

Binary asteroseismic modelling: isochrone-cloud methodology and application toKeplergravity mode pulsators

Johnston

Tkachenko

Aerts

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Secure mode identification had to await nearly unin-Contact: joey.mombarg@kuleuven.be terrupted time series photometry with at least a factor ten longer time base, such as that assembled with the Kepler space telescope (Borucki et al 2010). Meanwhile, lots of progress has been made on the observational side in this topic over the past few years with firm detections of period spacing patterns reported in Pápics et al (2014Pápics et al ( , 2015; Kurtz et al (2014); Saio et al (2015); Van Reeth et al (2015a); Schmid et al (2015); Van Reeth et al (2016); Murphy et al (2016); Guo et al (2016); Ouazzani et al (2017); Saio et al (2017Saio et al ( , 2018; Szewczuk & Daszyńska-Daszkiewicz (2018) and Li et al (2019).…”

Section: Introductionmentioning

confidence: 99%

Asteroseismic masses, ages, and core properties of γ Doradus stars using gravito-inertial dipole modes and spectroscopy

Mombarg

Reeth

Pedersen

et al. 2019

Monthly Notices of the Royal Astronomical Society

119

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The asteroseismic modelling of period spacing patterns from gravito-inertial modes in stars with a convective core is a high-dimensional problem. We utilise the measured period spacing pattern of prograde dipole gravity modes (acquiring Π 0 ), in combination with the effective temperature (T eff ) and surface gravity (log g) derived from spectroscopy, to estimate the fundamental stellar parameters and core properties of 37 γ Doradus (γ Dor) stars whose rotation frequency has been derived from Kepler photometry. We make use of two 6D grids of stellar models, one with step core overshooting and one with exponential core overshooting, to evaluate correlations between the three observables Π 0 , T eff , and log g and the mass, age, core overshooting, metallicity, initial hydrogen mass fraction and envelope mixing. We provide multivariate linear model recipes relating the stellar parameters to be estimated to the three observables (Π 0 , T eff , log g). We estimate the (core) mass, age, core overshooting and metallicity of γ Dor stars from an ensemble analysis and achieve relative uncertainties of ∼ 10 per cent for the parameters. The asteroseismic age determination allows us to conclude that efficient angular momentum transport occurs already early on during the main sequence. We find that the nine stars with observed Rossby modes occur across almost the entire main-sequence phase, except close to core-hydrogen exhaustion. Future improvements of our work will come from the inclusion of more types of detected modes per star, larger samples, and modelling of individual mode frequencies.

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“…This is the first measurement of the internal rotation of F-or A-type stars in a synchronized close binary system. The two F-star components in the eccentric binary system KIC 10080943 (Schmid et al 2015) also show near-uniform interior rotation, as revealed from the splitting of g-modes.…”

Section: Identification Of Prograde Dipole G-modes Affected By Rotationmentioning

confidence: 97%

Gravity Modes Reveal the Internal Rotation of a Post-mass-transfer Gamma Doradus/Delta Scuti Hybrid Pulsator in Kepler Eclipsing Binary KIC 9592855

Guo

Gies

Matson

2017

ApJ

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We report the discovery of a post-mass transfer Gamma Doradus/Delta Scuti hybrid pulsator in the eclipsing binary KIC 9592855. This binary has a circular orbit, an orbital period of 1.2 days, and contains two stars of almost identical masses (M 1 = 1.72M ⊙ , M 2 = 1.71M ⊙ ). However, the cooler secondary star is more evolved (R 2 = 1.96R ⊙ ) while the hotter primary is still on the zero-agemain-sequence (R 1 = 1.53R ⊙ ). Coeval models from single star evolution cannot explain the observed masses and radii, and binary evolution with mass-transfer needs to be invoked. After subtracting the binary light curve, the Fourier spectrum shows low-order pressure-mode pulsations, and more dominantly, a cluster of low-frequency gravity modes at about 2 day −1 . These g-modes are nearly equally-spaced in period, and the period spacing pattern has a negative slope. We identify these g-modes as prograde dipole modes and find that they stem from the secondary star. The frequency range of unstable p-modes also agrees with that of the secondary. We derive the internal rotation rate of the convective core and the asymptotic period spacing from the observed g-modes. The resulting values suggest that the core and envelope rotate nearly uniformly, i.e., their rotation rates are both similar to the orbital frequency of this synchronized binary.-2 -

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KIC 10080943: An eccentric binary system containing two pressure- and gravity-mode hybrid pulsators

Cited by 56 publications

References 70 publications

Binary asteroseismic modelling: isochrone-cloud methodology and application toKeplergravity mode pulsators

Binary asteroseismic modelling: isochrone-cloud methodology and application toKeplergravity mode pulsators

Asteroseismic masses, ages, and core properties of γ Doradus stars using gravito-inertial dipole modes and spectroscopy

Gravity Modes Reveal the Internal Rotation of a Post-mass-transfer Gamma Doradus/Delta Scuti Hybrid Pulsator in Kepler Eclipsing Binary KIC 9592855

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