Stellar evolution with rotation and magnetic fields - IV. The solar rotation profile

By P. Eggenberger, Andre Maeder, G. Meynet. 2005

143 citations recorded by the source corpus.

We examine the generation of a magnetic field in a solar-like star and its effects on the internal distribution of the angular velocity. We suggest that the evolution of a rotating star with magnetic fields leads to an equilibrium value of the differential rotation. This equilibrium is determined by the magnetic coupling, which favours a constant rotation profile, and meridional circulation which tends to build differential rotation. The global equilibrium stage is close to solid body rotation between about 0.7 and 0.2 $R_{\odot}$, in good agreement with helioseismic measurements.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/05f661c0c7aa73374c1a92afba32f4489c6cd557

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In Astronomy and Astrophysics

Citations in the corpus

Lithium depletion and the rotational history of exoplanet host stars (2008, background): “Candidates include magnetic field (Eggenberger et al. 2005) and internal gravity waves (Talon et al. 2002).”
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, background): “…through the action of meridional circulation and shear turbulence, combined possibly with other processes induced by internal gravity waves or magnetic fields (see e.g. Zahn 1992; Zahn et al. 1997; Maeder & Zahn 1998; Talon & Charbonnel 1998; Eggenberger et al. 2005; Charbonnel & Talon 2005, 2008).”
Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants (2012, background): “…the modelling of angular momentum transport shows that rotating models including meridional circulation and shear turbulence are unable to reproduce the near uniformity of the solar rotation profile (Pinsonneault et al. 1989; Chaboyer et al. 1995; Eggenberger et al. 2005; Turck-Chièze et al. 2010).”
On magnetic instabilities and dynamo action in stellar radiation zones (2007, background): “Applying essentially Spruit’s prescriptions, Maeder and Meynet (2003, 2004, 2005), Eggenberger et al. (2005) and Heger et al. (2005) introduced this dynamo, and the turbulent transport believed to be associated with it, in their stellar evolution calculations.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “…torques from ST dynamo fields can reproduce the flat rotation profile in the solar interior (Mestel & Weiss 1987; Charbonneau & MacGregor 1993; Eggenberger et al. 2005) and the observed spin rates of WDs and neutron stars (Heger et al. 2005; Suijs et al. 2008), although they still cannot…”
ANGULAR MOMENTUM TRANSPORT WITHIN EVOLVED LOW-MASS STARS (2014, background): “…ay 2 01 4 NSs) are in much better agreement with models including this angular momentum transport mechanism (Heger et al. 2005; Suijs et al. 2008), which has also been discussed in the context of the rigid rotation of the solar core (Eggenberger et al. 2005), but see also Denissenkov et al. (2010).”