Stellar evolution with rotation and magnetic fields III. The interplay of circulation and dynamo

By Andre Maeder, G. Meynet. 2005

137 citations recorded by the source corpus.

We examine the effects of the magnetic field created by the Tayler-Spruit dynamo in differentially rotating stars. Magnetic fields of the order of a few 10 4 G are present through most of the stellar envelope, with the exception of the outer layers. The diffusion coefficient for the transport of angular momentum is very large and it imposes nearly solid body rotation during the MS phase. In turn, solid body rotation drives meridional circulation currents which are much faster than usual and leads to much larger diffusion coefficients than the magnetic diffusivity for the chemical species. The consequence is that the interplay of the thermal and magnetic instabilities favours the chemical transport of elements, while there would be no transport in models with magnetic field only. We also discuss the effects on the stellar interior, lifetimes and HR diagram.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4ce0d336a0f4be9377da54b0445c7e2a3abca0d5

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In Astronomy and Astrophysics

1. N. Langer
2. Selma de Mink
3. G. Meynet
4. S. Ekström
5. R. Hirschi
6. N. Smith
7. Stan Woosley
8. S. Smartt

Citations in the corpus

• The surprising magnetic topology of τ Sco: fossil remnant or dynamo output? (2006, unknown): “…the outer radiative envelope could also be involved in genuine dynamo processes, in a subsurface shear layer (Tout & Pringle 1995; Ligni`eres et al. 1996) or even throughout the whole envelope (Spruit 2002; MacDonald & Mullan 2004; Mullan & MacDonald 2005; Maeder & Meynet 2005; Braithwaite 2006).”
• s-process production in rotating massive stars at solar and low metallicities (2015, methodology): “If we compare models computed with the Tayler–Spruit dynamo and models without, we observed that starting from the same initial conditions (mass, metallicity, rotation), models with the Tayler–Spruit dynamo are more mixed (see for instance Maeder & Meynet 2005).”
• THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “One option is the inheritance from stellar evolution (Maeder & Meynet 2004, 2005), which is a long standing unsolved problem.”
• The most massive stars in the Arches cluster (2007, background): “Recently, Maeder & Meynet (2005) have shown that the presence of magnetic fields in massive stars could favor solid body rotation and consequently chemical mixing.”
• Mass loss from hot massive stars (2008, methodology): “This dynamo has been incorporated into recent stellar structure/evolution calculations (Maeder and Meynet 2003a, 2004, 2005, Heger et al 2005,Brott et al 2008) to understand the internal angular momentum transport (thoug the induced mixing processes might be too strong, e.g., Brott et al 2008).”
• Evolution towards the critical limit and the origin of Be stars (2007, background): “A magnetic field, following the Tayler-Spruit dynamo (Spruit 2002), will tend to impose solid body rotation during the MS phase (Maeder & Meynet 2005), thus making the approach of the critical limit easier (stronger coupling between thecore and the envelope).”
• 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.”
• The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class (2014, background): “A faster rotation increases the WR lifetime and decreases the minimum initial mass for the WR phase, mainly due to a more efficient internal mixing (Maeder & Meynet 2005).”
• Magnetic Fields of Nondegenerate Stars (2009, background): “Due to their strong angular rotation gradient, massive stars are potentially capable of stretching/amplifying their magnetic fields, reducing/suppressing their differential rotation and modifying their evolution (Maeder & Meynet 2003, 2004, 2005).”
• Rotating massive main-sequence stars - I. Grids of evolutionary models and isochrones (2011, background): “In agreement with Maeder & Meynet (2005) we find that magnetic fields keep the star near rigid rotation throughout its main sequence evolution, suppressing the mixing induced by shear between neighboring layers.”
• Stellar evolution with rotation - XIII. Predicted GRB rates at various Z (2005, background): “Maeder & Meynet (2005) show that the treatment of meridional circulation as an advective process is crucial for modelling the interplay between circulation and magnetic braking.”
• Single star progenitors of long gamma-ray bursts - I. Model grids and redshift dependent GRB rate (2006, methodology): “…& Spruit 2005; Petrovic et al. 2005), while they can consistently explain the spin rates of young neutron stars (Heger, Woosley & Spruit 2005; cf. Ott et al. 2006) and white dwarfs (Suijs et al. 2006), as well as the internal rotational profile of the Sun (Eggenberger, Maeder & Meynet 2005).”
• Effects of rotation on the evolution of primordial stars (2008, background): “They have been shown to change many features in stellar evolution (Heger et al. 2005; Maeder & Meynet 2005), and to provide the strong core-envelope coupling that is lacking in the Z = 0 models.”
• Very low-metallicity massive stars: - Pre-SN evolution models and primary nitrogen production (2006, background): “The effects of magnetic fields (Yoon & Langer 2005; Woosley & Heger 2006; Maeder & Meynet 2005) on the results will be studied in the near future.”
• The Galactic WN stars. Spectral analyses with line-blanketed model atmospheres versus stellar evolut (2006, background): “Maeder & Meynet (2005) expect significant effects of the predicted field on the stellar evolution, but corresponding sets of tracks are not yet available.”
• The Geneva stellar evolution code (2008, background): “This equilibrium is determined by the magnetic coupling, which favours a constant rotation profile, and meridional circulation which tends to build differential rotation (Maeder and Meynet 2003, 2004b, 2005; Eggenberger et al. 2005b).”
• Evolution of rapidly rotating metal-poor massive stars towards gamma-ray bursts (2005, background): “…therein), which includes the effect of the centrifugal force on the stellar structure, chemical mixing and transport of angular momentum due to rotationally induced hydrodynamic instabilities, and the transport of angular momentum due to magnetic torque (Spruit 2002; Maeder & Meynet 2005).”