Thermohaline instability and rotation-induced mixing - III. Grid of stellar models and asymptotic asteroseismic quantities from the pre-main sequence up to the AGB for low- and intermediate-mass…

By N. Lagarde, T. Decressin, C. Charbonnel, P. Eggenberger, S. Ekström, A. Palacios. 2012

195 citations recorded by the source corpus.

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 Msun. 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 νmax, the maximal amplitude Amax, 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. Results tables are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/543/A108

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/09db9fd3f630d733c18a943ceb265451299adf42

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In Astronomy and Astrophysics

1. W. Chaplin
2. D. Stello
3. B. Mosser
4. T. Bedding
5. D. Huber
6. S. Hekker
7. Y. Elsworth
8. J. Ridder

In Geophysics

1. Nuno C. Santos
2. Jon Fortney

Citations in the corpus

• Spin down of the core rotation in red giants (2012, background): “Therefore, a direct measurement of rotation inside red giants would give us an unprecedented opportunity 25 to perform a leap forward on our understanding of angular momentum transport in stellar interiors (e.g. Lagarde et al. 2012; Eggenberger et al. 2012).”
• Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, unknown): “…and the redistribution of angular momentum in the stellar interior at all phases of evolution (MacGregor & Brenner 1991; Allain 1998; Talon & Charbonnel 2003, 2005; Palacios et al. 2003, 2006; Charbonnel & Talon 2005; Charbonnel & Lagarde 2010; Lagarde et al. 2011, 2012; Charbonnel et al. 2013).”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “3 the relationship between mass and the [C/N] ratio after the first dredge-up in the models of Lagarde et al. (2012) as well as models computed with the GARching STellar Evolution Code (GARSTEC; Weiss & Schlattl 2008) for stars of solar metallicity: there is a decrease of [C/N] with increasing…”
• Mixed modes in red giants: a window on stellar evolution (2014, methodology): “They most probably correspond to stars in which the core is contracting because helium becomes exhausted, leaving the main region of the red clump and preparing to ascend the AGB (Lagarde et al. 2012; Corsaro et al. 2012; Montalbán & Noels 2013).”
• SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, methodology): “We used the latest version of the STAREVOL stellar evolution code (Charbonnel & Palacios 2004; Lagarde et al. 2012, Amard et al., in prep.)”
• Improved angular momentum evolution model for solar-like stars (2013, background): “…discontinuity of the angular velocity at the core-envelope interface, and should be considered as a simple-minded approximation of more physically-driven internal rotational profiles (e.g., Spada et al. 2010; Denissenkov et al. 2010; Brun et al. 2011; Turck-Chieze et al. 2011; Lagarde et al. 2012).”
• THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽ M/M☉ ⩽ 8.0 (2013, methodology): “In E12, r1 declines monotonically with the model mass (orange and red squares).”