Energy of solar-like oscillations in red giants

Grosjean, M.; Dupret, Marc‐Antoine; Belkacem, K.; Montalbán, J.; Samadi, R.

doi:10.1017/s1743921313014555

Cited by 3 publications

(5 citation statements)

References 7 publications

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“…In fact, we should expect to observe less mixed modes as the inertia ratio increases, which is the case for models with better trapped dipole modes. We are aware that this detectability limit is an arbitrary choice since the relation between inertia and amplitude is only a proxy, nevertheless the current available non-adiabatic computations confirm that assumption (Dupret et al 2009;Grosjean et al 2013). Moreover, we can expect more modes to be detected in longer time series, changing the value of ∆P obtained from the mean value of individual measured period spacings, and ∆P a being an upper limit.…”

Section: Period Spacing In the Red-clump And Secondary-clump Stars: A...mentioning

confidence: 99%

Testing Convective-Core Overshooting Using Period Spacings of Dipole Modes in Red Giants

Montalbán

Miglio

Noels

et al. 2013

ApJ

129

122

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Uncertainties on central mixing in main sequence (MS) and core He-burning (He-B) phases affect key predictions of stellar evolution such as late evolutionary phases, chemical enrichment, ages etc. We propose a test of the extension of extra-mixing in two relevant evolutionary phases based on period spacing (∆P ) of solar-like oscillating giants. From stellar models and their corresponding adiabatic frequencies (respectively computed with ATON and LOSC codes) we provide the first predictions of the observable ∆P for stars in the red giant branch (RGB) and in the red clump (RC). We find: i) a clear correlation between ∆P and the mass of the helium core (M He ); the latter in intermediate-mass stars depends on the MS overshooting, hence it can be used to set constraints on extra mixing during MS when coupled with chemical composition; ii) a linear dependence of the average value of the asymptotic period spacing ( ∆P a ) during the He-B phase on the size of the convective core. A first comparison with the inferred asymptotic period spacing for Kepler RC stars suggests the need for extra mixing also during this phase, as evinced from other observational facts.

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Section: Period Spacing In the Red-clump And Secondary-clump Stars: A...mentioning

confidence: 99%

Testing Convective-Core Overshooting Using Period Spacings of Dipole Modes in Red Giants

Montalbán

Miglio

Noels

et al. 2013

ApJ

129

122

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“…Another reason for the non-detection of g-dominated modes is radiative damping near the bottom of the hydrogen-burning shell, such as in the model depicted in the left panel of Figure 13, which becomes stronger with increasing density contrast between core and envelope. The Fourier power spectrum of red-giant stars can, therefore, be of large complexity (Dupret et al, 2009;Grosjean et al, 2014).…”

Section: Red-giant Starsmentioning

confidence: 99%

“…The first model is that by Gough (1977a,b), which has been used, for example, by Baker and Gough (1979), Balmforth (1992a), Houdek et al (1995), Rosenthal et al (1995), Houdek (1997Houdek ( , 2000, Houdek et al (1999a), andChaplin et al (2005). The second model is that by Unno (1967Unno ( , 1977, upon which the generalized models by Gabriel (1996) and Grigahcène et al (2005) are based, with applications by Dupret et al (2005c,a,b, 2006a,b,c, 2009), Belkacem et al (2008, 2009, and Grosjean et al (2014). 3.2 Two time-dependent convection models for radially pulsating stars Unno (1967) and Gough (1965Gough ( , 1977a generalized the mixing-length formulation for modelling the interaction of the turbulent velocity field with radial pulsation. Both authors adopted the Boussinesq approximation.…”

Section: Introductionmentioning

confidence: 99%

“…The first model is that by Gough (1977a,b), which has been used, for example, by Baker and Gough (1979), Balmforth (1992a, Rosenthal et al (1995), Houdek (1997, Houdek et al (1999a), andChaplin et al (2005). The second model is that by Unno (1967Unno ( , 1977, upon which the generalized models by Gabriel (1996) and Grigahcène et al (2005) are based, with applications by Dupret et al (2005cDupret et al ( ,a,b, 2006aDupret et al ( ,b,c, 2009, Belkacem et al (2008Belkacem et al ( , 2009Belkacem et al ( , 2012, and Grosjean et al (2014).…”

Section: Introductionmentioning

confidence: 99%

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Interaction Between Convection and Pulsation

Houdek

Dupret

2015

Living Rev. Sol. Phys.

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This article reviews our current understanding of modelling convection dynamics in stars. Several semi-analytical time-dependent convection models have been proposed for pulsating one-dimensional stellar structures with different formulations for how the convective turbulent velocity field couples with the global stellar oscillations. In this review we put emphasis on two, widely used, time-dependent convection formulations for estimating pulsation properties in one-dimensional stellar models. Applications to pulsating stars are presented with results for oscillation properties, such as the effects of convection dynamics on the oscillation frequencies, or the stability of pulsation modes, in classical pulsators and in stars supporting solar-type oscillations. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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“…Predictions of frequency-dependent damping rates in more than 100 main-sequence stellar models were reported by Houdek et al (1999), who used Gough's (1977aGough's ( , 1977b nonlocal, time-dependent convection formulation, as did Balmforth (1992a) for the Sun, in the nonadiabatic stability calculations. Frequency-dependent damping rates in red giants were addressed by, for example, Houdek & Gough (2002), Dupret et al (2009), Grosjean et al (2014) and Aarslev et al (2018). Belkacem et al (2012) compared theoretical damping rates with main-sequence and red-giant linewidth observations from CoRoT (Baglin et al 2009) and Kepler at frequencies near the maximum oscillation power, ν max .…”

Section: Introductionmentioning

confidence: 99%

Damping rates and frequency corrections of Kepler LEGACY stars

Houdek

Lund

Trampedach

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Linear damping rates and modal frequency corrections of radial oscillation modes in selected LEGACY main-sequence stars are estimated by means of a nonadiabatic stability analysis. The selected stellar sample covers stars observed by Kepler with a large range of surface temperatures and surface gravities. A nonlocal, time-dependent convection model is perturbed to assess stability against pulsation modes. The mixinglength parameter is calibrated to the surface-convection-zone depth of a stellar model obtained from fitting adiabatic frequencies to the LEGACY observations, and two of the nonlocal convection parameters are calibrated to the corresponding LEGACY linewidth measurements. The remaining nonlocal convection parameters in the 1D calculations are calibrated so as to reproduce profiles of turbulent pressure and of the anisotropy of the turbulent velocity field of corresponding 3D hydrodynamical simulations. The atmospheric structure in the 1D stability analysis adopts a temperatureoptical-depth relation derived from 3D hydrodynamical simulations. Despite the small number of parameters to adjust, we find good agreement with detailed shapes of both turbulent pressure profiles and anisotropy profiles with depth, and with damping rates as a function of frequency. Furthermore, we find the absolute modal frequency corrections, relative to a standard adiabatic pulsation calculation, to increase with surface temperature and surface gravity.

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Energy of solar-like oscillations in red giants

Cited by 3 publications

References 7 publications

Testing Convective-Core Overshooting Using Period Spacings of Dipole Modes in Red Giants

Testing Convective-Core Overshooting Using Period Spacings of Dipole Modes in Red Giants

Interaction Between Convection and Pulsation

Damping rates and frequency corrections of Kepler LEGACY stars

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