Hydrodynamical stellar models including rotation, internal gravity waves, and atomic diffusion - I. Formalism and tests on Pop I dwarfs

By Suzanne Talon, C. Charbonnel. 2005

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In Astronomy and Astrophysics

Citations in the corpus

Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, background): “…active, the most commonly invoked being diffusion by turbulent viscosity, transport by meridional circulation (Maeder & Zahn 1998; Zahn 1992), torques due to magnetic fields (Maeder & Meynet 2004; Mathis & Zahn 2005; Strugarek et al. 2011), and transport by gravity waves (Talon & Charbonnel 2005).”
Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, unknown): “…et al. 2015), 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…”
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, background): “Different proposed extra mixing mechanisms are: rotation and atomic diffusion (Maeder & Meynet 2012), internal gravity waves (Talon & Charbonnel 2005), magnetic dynamo (Busso et al. 2007), and thermohaline mixing after the sub-giant phase (Charbonnel & Zahn 2007; Cantiello & Langer 2010).”
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…transfer(Packet 1981; Shu & Lubow 1981) and tidal interactions(Petrovic et al. 2005), as well as internal mixing of the stellar layers across the core-envelope boundary via magnetic torquing(Spruit 2002; Maeder & Meynet 2003) and gravity waves(Talon & Charbonnel 2005, 2008; Fuller et al. 2015).”
Rotational mixing in low-mass stars: II. Self-consistent models of Pop II RGB stars (2006, background): “For a complete discussion of this problem, the reader is referred to Talon & Charbonnel (1998), as well as to Talon & Charbonnel (2005) and Charbonnel & Talon (2005), which describe how internal gravity waves could help resolve this issue in Pop II stars.”
Asteroseismology of Solar-Type and Red-Giant Stars (2013, background): “…Maeder 1975, Ventura et al. 1998), microscopic diffusion (Michaud et al. 2004), rotationally induced mixing (e.g., see Maeder & Meynet 2000, Mathis, Palacios & Zahn 2004,and references therein), and mixing generated by propagation of internal waves (e.g. Young et al. 2003, Talon & Charbonnel 2005).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “…1969; Fricke & Kippenhahn 1972; Tassoul 1978; Zahn 1983; Pinsonneault 1997; Heger et al. 2000; Maeder & Meynet 2000; Palacios et al. 2003; Talon & Charbonnel 2005; Denissenkov & Pinsonneault 2007; Hunter et al. 2007; Chieffi & Limongi 2013; Cantiello et al. 2014), but it remains as one…”
INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT (2013, background): “The varying results between numerical simulations and analytic models with regard to mixing and angular momentum transport can certainly be traced to differences in the spectra and wave amplitudes employed (Denissenkov et al. 2008; Talon & Charbonnel 2005; Rogers & MacGregor 2011).”
Angular momentum transport by heat-driven g-modes in slowly pulsating B stars (2017, background): “…of angular momentum is well studied in the context of lower-mass stars (e.g., Schatzman 1993; Kumar & Quataert 1997; Zahn et al. 1997; Talon et al. 2002; Talon & Charbonnel 2005; Rogers et al. 2008), and a number of authors explore whether the same process might be important in more-massive stars.”