A Mass-accreting Gamma Doradus Pulsator with a Synchronized Core in Kepler Eclipsing Binary KIC 7385478

Guo, Zhao; Li, Gang

doi:10.3847/2041-8213/ab3a53

Cited by 18 publications

(15 citation statements)

References 43 publications

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“…Using the traditional approximation, Ouazzani et al (2017) thus defines the slope of this trend as a new observable that is directly linked to the rotation rate near the stellar core modulated by the azimuthal order m. These ridges were observed in many γDor (e.g. Bedding et al, 2015;Guo and Li, 2019;Li et al, 2020a,b;Garcia et al, 2022) and SPB stars (Pápics et al, 2017;Pedersen et al, 2021;Szewczuk et al, 2021Szewczuk et al, , 2022, with a variety of behaviors related to mixing and rotation.…”

Section: Mirouhmentioning

confidence: 99%

Forward modelling and the quest for mode identification in rapidly rotating stars

Mirouh

2022

Front. Astron. Space Sci.

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Asteroseismology has opened a window on the internal physics of thousands of stars, by relating oscillation spectra properties to the internal physics of stars. Mode identification, namely the process of associating a measured oscillation frequency to the corresponding mode geometry and properties, is the cornerstone of this analysis of seismic spectra. In rapidly rotating stars this identification is a challenging task that remains incomplete, as modes assume complex geometries and regular patterns in frequencies get scrambled under the influence of the Coriolis force and centrifugal flattening. In this article, I will first discuss the various classes of mode geometries that emerge in rapidly rotating stars and the related frequency and period patterns, as predicted by ray dynamics, complete (non-)adiabatic calculations, or using the traditional approximation of rotation. These patterns scale with structural quantities and help us derive crucial constraints on the structure and evolution of these stars. I will summarize the amazing progress accomplished over the last few years for the deciphering of gravity-mode pulsator oscillation spectra, and recent developments based on machine-learning classification techniques to distinguish oscillation modes and pattern analysis strategies that let us access the underlying physics of pressure-mode pulsators. These approaches pave the way to ensemble asteroseismology of classical pulsators. Finally, I will highlight how these recent progress can be combined to improve forward seismic modelling. I will focus on the example of Rasalhague, a well-known rapid rotator, to illustrate the process and the needed advances to obtain à-la-carte modelling of such stars.

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Section: Mirouhmentioning

confidence: 99%

Forward modelling and the quest for mode identification in rapidly rotating stars

Mirouh

2022

Front. Astron. Space Sci.

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“…There have been a total of 34 eclipsing binary systems with g-mode period-spacing patterns discovered so far in the Kepler data (Li et al 2020a), and only three have been modelled (Zhang et al 2018;Guo & Li 2019;Zhang et al 2020), none of which from the viewpoint of assessing internal mixing. As such, it is the goal of our study to add to the dearth of literature on the evolutionary and asteroseismic modelling of g-mode pulsators in eclipsing binary systems.…”

Section: Introductionmentioning

confidence: 99%

A comparison of the dynamical and model-derived parameters of the pulsating eclipsing binary KIC 9850387

Sekaran

Tkachenko

Johnston

et al. 2021

A&A

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Context. One-dimensional stellar evolutionary models incorporate interior mixing profiles as a simplification of multi-dimensional physical processes that have a significant impact on the evolution and lifetime of stars. As such, the proper calibration of interior mixing profiles is required for the reconciliation of observational parameters and theoretical predictions. The modelling and analysis of pulsating stars in eclipsing binary systems that display gravity-mode (g-mode) oscillations allows for the precise constraints on the interior mixing profiles through the combination of spectroscopic, binary and asteroseismic obervables. Aims. We aim to unravel the interior mixing profile of the pulsating eclipsing binary KIC 9850387 by comparing its dynamical parameters and the parameters derived through a combination of evolutionary and asteroseismic modelling. Methods. We created a grid of stellar evolutionary models using the stellar evolutionary code MESA and performed an isochrone-cloud (isocloud) based evolutionary modelling of the system. We then generated a grid of pulsational models using the stellar pulsation code GYRE based on the age constraints from the evolutionary modelling. Finally, we performed asteroseismic modelling of the observed ℓ = 1 and ℓ = 2 period-spacing patterns, utilising different combinations of observational constraints, merit functions, and asteroseismic observables to obtain strong constraints on the interior properties of the primary star. Results. Through a combination of asteroseismic modelling and dynamical constraints, we found that the system comprises two main-sequence components at an age of 1.2 ± 0.1 Gyr. We also observed that asteroseismic modelling provided stronger constraints on the interior properties than evolutionary modelling. Overall, we found high levels of interior mixing, when compared to similar studies, for the primary star. We posited that this is a result of intrinsic non-tidal mixing mechanisms due to a similar observed behaviour in single stars. We investigated the high-frequency regime of KIC 9850387 and found evidence of the surface effect due to the systematic frequency offset of the theoretical modes from the nearest observed modes. We also found evidence of rotational splitting in the form of a prograde-retrograde dipole g1 mode doublet with a missing zonal mode, implying an envelope rotational frequency that is three times higher than the core rotational frequency and about 20 times slower than the orbital frequency, but we note that this result is based completely on the rotational splitting of a single dipole mode. Conclusions. We find that the dynamical parameters and the parameters extracted from the asteroseismic modelling of period-spacing patterns are only barely compliant, reinforcing the need for homogeneous analyses of samples of pulsating eclipsing binaries that aim to calibrating interior mixing profiles.

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“…The complementary nature of binarity and g-mode asteroseismology is well-known, with a number of individual case studies on particular stars (e.g. Maceroni et al 2009Maceroni et al , 2013Welsh et al 2011;Chapellier & Mathias 2013;Debosscher et al 2013;Hambleton et al 2013;Keen et al 2015;Schmid et al 2015;Schmid & Aerts 2016;Matson et al 2016;Lee & Park 2018;Zhang et al 2018Zhang et al , 2020Guo & Li 2019;Guo et al 2017aGuo et al ,b, 2019Guo et al , 2020. However, these case studies tend to be either (1) purely observational, (2) feature only tidally excited g modes (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Debosscher et al 2013). Also, of these studies only Schmid & Aerts (2016), Zhang et al (2018Zhang et al ( , 2020, and Guo & Li (2019) include detailed asteroseismic modelling, with Schmid & Aerts (2016) presenting the most detailed modelling effort of the three as they used theoretical periodspacing patterns, derived from evolutionary models, to match their observed period-spacing patterns. This provides stronger constraints on the stellar structure when compared to, for example, fitting for Π 0 (Ouazzani et al 2019;Mombarg et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Tango of celestial dancers: A sample of detached eclipsing binary systems containingg-mode pulsating components

Sekaran

Tkachenko

Abdul-Masih

et al. 2020

A&A

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Context. Eclipsing binary systems with components that pulsate in gravity modes (g modes) allow for simultaneous and independent constraints of the chemical mixing profiles of stars. The high precision of the dynamical masses and radii as well as the imposition of identical initial chemical compositions and equivalent ages provide strong constraints during the modelling of g-mode period-spacing patterns. Aims. We aim to assemble a sample of g-mode pulsators in detached eclipsing binaries with the purpose of finding good candidates for future evolutionary and asteroseismic modelling. In addition, we present a case study of the eclipsing binary KIC9850387, identified as our most promising candidate, and detail the results of the observational spectroscopic, photometric, and asteroseismic analysis of the system. Methods. We selected all of the detached eclipsing binaries in the Kepler eclipsing binary catalogue with Kepler Input Catalogue (KIC) temperatures between 6000 K and 10 000 K, and performed a visual inspection to determine the presence and density of g modes, and the presence of g-mode period-spacing patterns in their frequency spectra. We then characterised our sample based on their g-mode pulsational parameters and binary and atmospheric parameters. A spectroscopic follow-up of our most promising candidate was then performed, and the orbital elements of the system were extracted. We then performed spectral disentangling followed by atmospheric modelling and abundance analysis for the primary star. We utilised an iterative approach to simultaneously optimise the pulsational and eclipse models, and subsequently performed an analysis of the pressure- (p-) and g-mode pulsational frequencies. Results. We compiled a sample of 93 Kepler eclipsing binary stars with g-mode pulsating components and identified clear g-mode period-spacing patterns in the frequency spectra of seven of these systems. We also identified 11 systems that contained hybrid p- and g-mode pulsators. We found that the g-mode pulsational parameters and the binary and atmospheric parameters of our sample are weakly correlated at best, as expected for detached main-sequence binaries. We find that the eclipsing binary KIC9850387 is a double-lined spectroscopic binary in a near-circular orbit with a hybrid p- and g-mode pulsating primary with Mp = 1.66−0.01+0.01 M⊙ and Rp = 2.154−0.004+0.002 R⊙, and a solar-like secondary with Ms = 1.062−0.005+0.003 M⊙ and Rs = 1.081−0.002+0.003 R⊙. We find ℓ = 1 and ℓ = 2 period-spacing patterns in the frequency spectrum of KIC9850387 spanning more than ten radial orders each, which will allow for stringent constraints of stellar structure during future asteroseismic modelling.

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A Mass-accreting Gamma Doradus Pulsator with a Synchronized Core in Kepler Eclipsing Binary KIC 7385478

Cited by 18 publications

References 43 publications

Forward modelling and the quest for mode identification in rapidly rotating stars

Forward modelling and the quest for mode identification in rapidly rotating stars

A comparison of the dynamical and model-derived parameters of the pulsating eclipsing binary KIC 9850387

Tango of celestial dancers: A sample of detached eclipsing binary systems containingg-mode pulsating components

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