Probing the interior physics of stars through asteroseismology

Aerts, C.

doi:10.1103/revmodphys.93.015001

Cited by 217 publications

(152 citation statements)

References 553 publications

(695 reference statements)

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“…Suggested reasons for this are (1) the limitations of 1D stellar models in terms of chemical mixing, (2) the use of a time-independent simplified convection theory for the thin stellar envelope and (3) the fact that tidal effects in the system were not accounted for (these forces were estimated to be small although the (orbit-dependent) rotational splitting of the p modes may be a clue). Including these aspects in the theoretical framework (e.g., with MESA) may allow for an improved and successful modelling of this interesting system in the future [56] .…”

Section: Conclusion-discussionmentioning

confidence: 99%

“…The orbital properties too play a role, as we have seen, since different effects are detected in close, circular versus eccentric systems. In turn, tidally excited non-radial oscillations can affect the evolution of close binaries (for details see Aerts [56], Section IV.F., and references therein). Such in-depth studies are very pertinent and necessary for stellar physics in general.…”

Section: Discussionmentioning

confidence: 99%

“…Not only for a deeper understanding of the pulsations under different circumstances (systems versus single stars), but also for a profound understanding of the evolution of the rotational profile and angular momentum in stars and of the evolution of the systems, with as well as without tides. Finally, we need advanced theoretical models to improve our understanding of the interior physics of the components themselves [56]. Thanks to the excellent light curves acquired from space, we are just beginning to explore the complex reality of what could be called "tidal asteroseismology".…”

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Lampens

2021

Galaxies

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Eclipsing systems are essential objects for understanding the properties of stars and stellar systems. Eclipsing systems with pulsating components are furthermore advantageous because they provide accurate constraints on the component properties, as well as a complementary method for pulsation mode determination, crucial for precise asteroseismology. The outcome of space missions aiming at delivering high-accuracy light curves for many thousands of stars in search of planetary systems has also generated new insights in the field of variable stars and revived the interest of binary systems in general. The detection of eclipsing systems with pulsating components has particularly benefitted from this, and progress in this field is growing fast. In this review, we showcase some of the recent results obtained from studies of eclipsing systems with pulsating components based on data acquired by the space missions Kepler or TESS. We consider different system configurations including semi-detached eclipsing binaries in (near-)circular orbits, a (near-)circular and non-synchronized eclipsing binary with a chemically peculiar component, eclipsing binaries showing the heartbeat phenomenon, as well as detached, eccentric double-lined systems. All display one or more pulsating component(s). Among the great variety of known classes of pulsating stars, we discuss unevolved or slightly evolved pulsators of spectral type B, A or F and red giants with solar-like oscillations. Some systems exhibit additional phenomena such as tidal effects, angular momentum transfer, (occasional) mass transfer between the components and/or magnetic activity. How these phenomena and the orbital changes affect the different types of pulsations excited in one or more components, offers a new window of opportunity to better understand the physics of pulsations.

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Section: Conclusion-discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Lampens

2021

Galaxies

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“…The subsequent gravity waves cannot pass the critical layer and waves dissipate strongly. Observationally, single upper main-sequence stars tend to have a nearly uniform rotation profile in the radiative envelope, inferred from asteroseismology (Bowman, 2020;Aerts, 2021) 3 . The gmode pulsating γ Dor stars (spectral type A-F-) in close binaries with P orb ≤ 10 d show a convective-core-boundary rotation period that is similar to the orbital period, suggesting that the tidal synchronization has already reached the deep interior Li et al, 2020a;Saio, 2020).…”

Section: Tidally Excited Oscillations (Teos) In Heartbeat Starsmentioning

confidence: 99%

Asteroseismology of Close Binary Stars: Tides and Mass Transfer

Guo

2021

Front. Astron. Space Sci.

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The study of stellar oscillations allows us to infer the properties of stellar interiors. Meanwhile, fundamental parameters such as mass and radius can be obtained by studying stars in binary systems. The synergy between binarity and asteroseismology can constrain the parameter space of stellar properties and facilitate the asteroseismic inference. On the other hand, binarity also introduces additional complexities such tides and mass transfer. From an observational perspective, we briefly review the recent advances in the study of tidal effects on stellar oscillations, focusing on upper main sequence stars (F-, A-, or OB- type). The effect can be roughly divided into two categories. The first one concerns the tidally excited oscillations (TEOs) in eccentric binaries where TEOs are mostly due to resonances between dynamical tides and gravity modes of the star. TEOs appear as orbital-harmonic oscillations on top of the eccentric ellipsoidal light curve variations (the “heartbeat” feature). The second category is regarding the self-excited oscillations perturbed by static tides in circularized and synchronized close binaries. It includes the tidal deformation of the propagation cavity and its effect on eigenfrequencies, eigenfunctions, and the pulsation alignment. We list binary systems that show these two types of tidal effect and summarize the orbital and pulsation observables. We also discuss the theoretical approaches used to model these tidal oscillations and relevant complications such as non-linear mode coupling and resonance locking. Further information can be extracted from the observations of these oscillations which will improve our understanding of tides. We also discuss the effect of mass transfer, the extreme result of tides, on stellar oscillations. We bring to the readers' attention: (1) oscillating stars undergoing mass accretion (A-, F-, and OB type pulsators and white dwarfs), for which the pulsation properties may be changed significantly by accretion; (2) post-mass transfer pulsators, which have undergone a stable or unstable Roche-Lobe overflow. These pulsators have great potential in probing detailed physical processes in stellar interiors and mass transfer, as well as in studying the binary star populations.

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“…The classifiers were implemented using TensorFlow software and its high-level Keras API (Abadi et al 2015;Chollet & Others 2015). We used the binary cross-entropy loss function, the Adam optimizer (Kingma & Ba 2014), a batch size of 64, and an 81%/9%/10% training/validation/test data split with a fixed random seed for reproducibility.…”

Section: Data Set Assembly and Classifier Trainingmentioning

confidence: 99%

The ZTF Source Classification Project. I. Methods and Infrastructure

Roestel

Duev

Mahabal

et al. 2021

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The Zwicky Transient Facility (ZTF) has been observing the entire northern sky since the start of 2018 down to a magnitude of 20.5 (5σ for 30 s exposure) in the g, r, and i filters. Over the course of two years, ZTF has obtained light curves of more than a billion sources, each with 50-1000 epochs per light curve in g and r, and fewer in i. To be able to use the information contained in the light curves of variable sources for new scientific discoveries, an efficient and flexible framework is needed to classify them. In this paper, we introduce the methods and infrastructure that will be used to classify all ZTF light curves. Our approach aims to be flexible and modular and allows the use of a dynamical classification scheme and labels, continuously evolving training sets, and the use of different machine-learning classifier types and architectures. With this setup, we are able to continuously update and improve the classification of ZTF light curves as new data become available, training samples are updated, and new classes need to be incorporated.

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Probing the interior physics of stars through asteroseismology

Cited by 217 publications

References 553 publications

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Eclipsing Systems with Pulsating Components (Types β Cep, δ Sct, γ Dor or Red Giant) in the Era of High-Accuracy Space Data

Asteroseismology of Close Binary Stars: Tides and Mass Transfer

The ZTF Source Classification Project. I. Methods and Infrastructure

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