Reference grids of stellar models and oscillation frequencies

Lebreton, Y.; Michel, E.

doi:10.1007/s10509-008-9781-z

Cited by 4 publications

(4 citation statements)

References 21 publications

(17 reference statements)

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“…HR diagram featuring stars for which mode structure has been observed in photometry (red squares), a power excess has been detected in photometry (green circles), and a detection has been performed in radial velocity (blue stars). Stellar evolutionary tracks are taken from (20), for solar chemical composition. Red giant pulsators (~6 objects) are out of the upper right corner of the figure.…”

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confidence: 99%

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CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun

Michel

Baglin

Auvergne

et al. 2008

Science

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211

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Oscillations of the Sun have been used to understand its interior structure. The extension of similar studies to more distant stars has raised many difficulties despite the strong efforts of the international community over the past decades. The CoRoT (Convection Rotation and Planetary Transits) satellite, launched in December 2006, has now measured oscillations and the stellar granulation signature in three main sequence stars that are noticeably hotter than the sun. The oscillation amplitudes are about 1.5 times as large as those in the Sun; the stellar granulation is up to three times as high. The stellar amplitudes are about 25% below the theoretic values, providing a measurement of the nonadiabaticity of the process ruling the oscillations in the outer layers of the stars.

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confidence: 99%

“…Laboratoire d'Astrophysique de Toulouse-Tarbes, Université de Toulouse, CNRS (UMR 5572), 14 Avenue Edouard Belin, F-31400 Toulouse, France. Centro de Astrofisica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 20. Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Brera Via Emilio Bianchi 46, 23807 Merate (LC), Italy 21.…”

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CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun

Michel

Baglin

Auvergne

et al. 2008

Science

Self Cite

211

164

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“…In order to ensure a correct computation of the adiabatic oscillations, we imposed a number of shells in which the stellar structure is radially distributed to be above 2000 approximately, as suggested by the ESTA/CoRoT working group (Moya & Garrido 2008;Lebreton et al 2008). Moreover, the stellar models were computed to rotate with Ω/Ω C 0.7, the vast majority below 0.5.…”

Section: The Equilibrium Modelsmentioning

confidence: 99%

Study of the low-order $Δν$-${\bar ρ}$ relation for moderately-rotating $δ$ Scuti stars and its impact on their characterisation

Rodríguez-Martín,

Hernández,

Suárez

et al. 2020

Preprint

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The large separation in the low radial order regime is considered as a highly valuable observable to derive mean densities of 𝛿 Scuti stars, due to its independence with rotation. Up to now, theoretical studies of this Δ𝜈ρ relation have been limited to 1D non-rotating models, and 2D pseudo-evolutionary models. The present work aims at completing this scenario by investigating quantitatively the impact of rotation in this relation on a large grid of 1D asteroseismic models representative of 𝛿 Scuti stars. These include rotation effects on both the stellar evolution and the interaction with pulsation. This allowed us to compute the stellar deformation, get the polar and equatorial radii, and correct the stellar mean densities. We found that the new Δ𝜈ρ relation for rotating models is compatible with previous works. We explained the dispersion of the points around the linear fits as caused mainly by the distribution of the stellar mass, and partially by the evolutionary stage. The new fit is found to be close to the previous theoretical studies for lower masses (1.3 − 1.81 M ). However, the opposite holds for the observations: for the higher masses (1.81 − 3 M ) the fit is more compatible with the empirical relation. To avoid such discrepancies, we provided new limits to the fit that encompass any possible dependency on mass. We applied these results to characterise the two well-known 𝛿 Scuti stars observed by CoRoT, HD 174936 and HD 174966, and compared the physical parameters with those of previous works. Inclusion of rotation in the modelling causes a tendency towards greater masses, radii, luminosities and lower density values. Comparison between Δ𝜈 and Gaia's luminosities also allowed us to constraint the inclination angles and rotational velocities of both stars. The present results pave the way to systematically constrain the angle of inclination (and thereby the actual surface rotation velocity) of 𝛿 Scuti stars.

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“…The best agreement is achieved by the present study, despite the fact that the diffusion process is not included. The differences are small, but it seems that Schaller et al (1992;Schal92) and CESAM's (Code d'Evolution Stellaire Adaptatif et Modulaire; Lebreton & Michel 2008) codes are not well calibrated on the solar parameters. The evolutionary track of Claret (2004;Claret04), on the other hand, substantially deviates from the data for the Sun.…”

Section: Comparison Of Solar Modelsmentioning

confidence: 99%

Grids of stellar models including second harmonic and colors: solar composition (Z= 0.0172,X= 0.7024)

Yıldız¹

2015

Res. Astron. Astrophys.

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Grids of stellar evolution are required in many fields of astronomy/astrophysics, such as planet hosting stars, binaries, clusters, chemically peculiar stars, etc. In this study, a grid of stellar evolution models with updated ingredients and recently determined solar abundaces is presented. The solar values for the initial abundances of hydrogen, heavy elements and mixing-length parameter are 0.0172, 0.7024 and 1.98, respectively. The mass step is small enough (0.01 M ⊙ ) that interpolation for a given star mass is not required. The range of stellar mass is 0.74 to 10.00 M ⊙ . We present results in different forms of tables for easy and general application. The second stellar harmonic, required for analysis of apsidal motion of eclipsing binaries, is also listed. We also construct rotating models to determine effect of rotation on stellar structure and derive fitting formula for luminosity, radius and the second stellar harmonic as a function of rotational parameter. We also compute and list colours and bolometric corrections of models required for transformation between theoretical and observational results. The results are tested for the Sun, the Hyades cluster, the slowly rotating chemically peculiar Am stars and the eclipsing binaries with apsidal motion. The theoretical and observational results along isochrones are in good agreement. The grids are also applicable to rotating stars provided that equatorial velocity is given.

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Reference grids of stellar models and oscillation frequencies

Cited by 4 publications

References 21 publications

CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun

CoRoT Measures Solar-Like Oscillations and Granulation in Stars Hotter Than the Sun

Study of the low-order $Δν$-${\bar ρ}$ relation for moderately-rotating $δ$ Scuti stars and its impact on their characterisation

Grids of stellar models including second harmonic and colors: solar composition (Z= 0.0172,X= 0.7024)

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