Effects of rotational mixing on the asteroseismic properties of solar-type stars

Eggenberger, P.; Meynet, Georges; Maeder, A.; Miglio, A.; Montalbán, J.; Carrier, F.; Mathis, S.; Charbonnel, C.; Talon, Suzanne

doi:10.1051/0004-6361/201014713

Cited by 76 publications

(72 citation statements)

References 45 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is a difference that could, at least partially, be influencing our results. Indeed, rotation during the main sequence is able to change the stellar core masses, chemical profile, and main sequence lifetimes (Eggenberger et al 2010;Lagarde et al 2016). A spread in rotational velocities among coeval stars might then cause the spread in the properties of the red giants, which might not be captured in our grids of non-rotating stellar models.…”

Section: Discussionmentioning

confidence: 97%

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Rodrigues

Bossini

Miglio

et al. 2017

Mon. Not. R. Astron. Soc.

105

119

View full text Add to dashboard Cite

Asteroseismic parameters allow us to measure the basic stellar properties of field giants observed far across the Galaxy. Most of such determinations are, up to now, based on simple scaling relations involving the large frequency separation, ∆ν, and the frequency of maximum power, ν max . In this work, we implement ∆ν and the period spacing, ∆P , computed along detailed grids of stellar evolutionary tracks, into stellar isochrones and hence in a Bayesian method of parameter estimation. Tests with synthetic data reveal that masses and ages can be determined with typical precision of 5 and 19 per cent, respectively, provided precise seismic parameters are available. Adding independent information on the stellar luminosity, these values can decrease down to 3 and 10 per cent respectively. The application of these methods to NGC 6819 giants produces a mean age in agreement with those derived from isochrone fitting, and no evidence of systematic differences between RGB and RC stars. The age dispersion of NGC 6819 stars, however, is larger than expected, with at least part of the spread ascribable to stars that underwent mass-transfer events.

show abstract

Section: Discussionmentioning

confidence: 97%

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Rodrigues

Bossini

Miglio

et al. 2017

Mon. Not. R. Astron. Soc.

105

119

View full text Add to dashboard Cite

show abstract

“…The change of initial velocity causes a different degree of rotation-mixing in the radiative region, resulting in different processes of lithium depletion (Li et al 2012). Moreover, rotational mixing also affects the asteroseismic properties of solar-type stars, which has been discussed by Eggenberger et al (2010). Higher values of the large frequency separation were found for rotating models than for non-rotating ones at the same evolutionary stage in Eggenberger et al (2010), because rotational mixing increased the effective temperature and to a smaller radius and hence to an increase of the stellar mean density.…”

Section: Discussionmentioning

confidence: 99%

Stellar parameters and seismological analysis of the star 18 Scorpii

Liu

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. We constructed models of the structure and evolution of the stars including diffusion and extra-mixing caused by rotation to estimate stellar parameters of the solar twin 18 Scorpii. Methods. Based on the classical observed features, we considered three additional constraints, i.e., lithium abundance log N(Li), rotational period P eq rot , and average large frequency separation ν , by combing stellar models with observations to determine stellar parameters and the possible evolutionary status of 18 Scorpii. Results. More accurate results of mass and age were found by our model than in previous studies. We estimate that the mass and age of 18 Scorpii are 1.030 ± 0.010 M and 3.66 +0.44 −0.50 Gyr, respectively. Moreover, the model gave better constraints of atmospheric features due to the accurate age estimation. Conclusions. The consideration of lithium, rotational period, and the average large frequency separation may help us in obtaining more accurate parameters of the star. Our results indicate that 18 Scorpii is a solar twin slightly more massive and younger than the Sun.

show abstract

“…4) with a significant impact on asteroseismic observables. In the case of main-sequence solar-type stars, rotation is found to shift the evolutionary tracks to the blue part of the HR diagram resulting in higher values of the large frequency separation for rotating models than for nonrotating ones at a given evolutionary stage (Eggenberger et al 2010a). For red giants, rotating models are found to decrease the determined value of the stellar mass of a star located at a given luminosity in the HR diagram and to increase the value of its age.…”

Section: Global Asteroseismic Quantitiesmentioning

confidence: 91%

Thermohaline instability and rotation-induced mixing

Lagarde

Decressin

Charbonnel

et al. 2012

A&A

Self Cite

273

433

View full text Add to dashboard Cite

Context. The availability of asteroseismic constraints for a large sample of stars from the missions CoRoT and Kepler paves the way for various statistical studies of the seismic properties of stellar populations. Aims. We evaluate the impact of rotation-induced mixing and thermohaline instability on the global asteroseismic parameters at different stages of the stellar evolution from the zero age main sequence to the thermally pulsating asymptotic giant branch to distinguish stellar populations. Methods. We present a grid of stellar evolutionary models for four metallicities (Z = 0.0001, 0.002, 0.004, and 0.014) in the mass range from 0.85 to 6.0 M . The models are computed either with standard prescriptions or including both thermohaline convection and rotation-induced mixing. For the whole grid, we provide the usual stellar parameters (luminosity, effective temperature, lifetimes, ... ), together with the global seismic parameters, i.e. the large frequency separation and asymptotic relations, the frequency corresponding to the maximum oscillation power ν max , the maximal amplitude A max , the asymptotic period spacing of g-modes, and different acoustic radii. Results. We discuss a signature of rotation-induced mixing on the global asteroseismic quantities, that can be detected observationally. Thermohaline mixing whose effects can be identified using spectroscopic studies cannot be characterized by the global seismic parameters studied here. However, we cannot exclude that individual mode frequencies or other well chosen asteroseismic quantities might help us to constrain this mixing.

show abstract

Effects of rotational mixing on the asteroseismic properties of solar-type stars

Cited by 76 publications

References 45 publications

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Determining stellar parameters of asteroseismic targets: going beyond the use of scaling relations

Stellar parameters and seismological analysis of the star 18 Scorpii

Thermohaline instability and rotation-induced mixing

Contact Info

Product

Resources

About