Transport and mixing in the radiation zones of rotating stars. I. Hydrodynamical processes
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The purpose of this paper is to improve the modelization of the rotational mixing which occurs in stellar radiation zones, through the combined action of the thermally driven meridional circulation and of the turbulence generated by the shear of differential rotation. The turbulence is assumed to be anisotropic, due to the stratification, with stronger transport in the horizontal directions than in the vertical. The main difference with the former treatments by Zahn (1992, AA it will be included in forthcoming papers.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/afcdfa58abb7b3221ca7d589d3e4827bd4493887
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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, methodology): “Higher order eff cts, included in the formalism developed by Mathis & Zahn (2004), are not considered here for the moment.”
- 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 stars of various metallicities (2012, methodology): “…evolution of the internal angular momentum profile is accounted for using the complete formalism developed by Zahn (1992), Maeder & Zahn (1998), and Mathis & Zahn (2004), which takes into account advection by meridional circulation and diffusion by shear turbulence (see Palacios et al. 2003, 2006;…”
- Rotation and magnetism of Kepler pulsating solar-like stars : Towards asteroseismically calibrated age-rotation relations (2014, background): “Stellar rotation fundamentally modifies stellar interiors (e.g. Zahn 1992; Pinsonneault 1997; Mathis & Zahn 2004; Decressin et al. 2009; Eggenberger et al. 2010; Ceillier et al. 2013; Marques et al. 2013).”