Magnetic confinement of the solar tachocline: II. Coupling to a convection zone
arXiv:1107.3665 · doi:10.1051/0004-6361/201116518
Abstract
The reason for the observed thinness of the solar tachocline is still not well understood. One of the explanations that have been proposed is that a primordial magnetic field renders the rotation uniform in the radiation zone. We test here the validity of this magnetic scenario through 3D numerical MHD simulations that encompass both the radiation zone and the convection zone. The numerical simulations are performed with the anelastic spherical harmonics (ASH) code. The computational domain extends from to . In the parameter regime we explored, a dipolar fossil field aligned with the rotation axis can not remain confined in the radiation zone. When the field lines are allowed to interact with turbulent unstationary convective motions at the base of the convection zone, 3D effects prevent the field confinement. In agreement with previous work, we find that a dipolar fossil field, even when it is initially buried deep inside the radiation zone, will spread into the convective zone. According to Ferraro's law of iso-rotation, it then imprints on the radiation zone the latitudinal differential rotation of the convection zone, which is not observed.
arXiv comment16 pages, 18 figures, to appear in A&A
References in corpus (15)
- A fossil origin for the magnetic fields of A-stars and white dwarfs
- Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
- Turbulent Convection Under the Influence of Rotation: Sustaining a Strong Differential Rotation
- On magnetic instabilities and dynamo action in stellar radiation zones
- Persistent Magnetic Wreaths in a Rapidly Rotating Sun
- Magnetic confinement of the solar tachocline
- Dynamics of the solar tachocline I: an incompressible study
- Seismic tests for solar models with tachocline mixing
- Dynamics of the solar tachocline II: the stratified case
- On Differential Rotation and Convection in the Sun
- Is the solar convection zone in strict thermal wind balance?
- Self-consistent theory of turbulent transport in the solar tachocline. II. Tachocline confinement
- Structure and stability of the magnetic solar tachocline
- Self-consistent theory of turbulent transport in the solar tachocline. III. Gravity waves
- Confinement of the Sun's interior magnetic field: some exact boundary-layer solutions
Cited by in corpus (43)
- Seismic constraints on the radial dependence of the internal rotation profiles of six Kepler subgiants and young red giants
- Seismic diagnostics for transport of angular momentum in stars 1. Rotational splittings from the PMS to the RGB
- Angular Momentum Transport in Stellar Interiors
- Understanding angular momentum transport in red giants: the case of KIC 7341231
- The Magnetic Fields at the Surface of Active Single G-K Giants
- Theoretical seismology in 3D : nonlinear simulations of internal gravity waves in solar-like stars
- Rotation rate of the solar core as a key constraint to magnetic angular momentum transport in stellar interiors
- Magnetic signatures on mixed-mode frequencies. I. An axisymmetric fossil field inside the core of red giants
- Anisotropic turbulent transport in stably stratified rotating stellar radiation zones
- How accurate are stellar ages based on stellar models ? I. The impact of stellar models uncertainties
- Extreme value statistics for two-dimensional convective penetration in a pre-Main Sequence star
- Characterizing the propagation of gravity waves in 3D nonlinear simulations of solar-like stars
- Dynamics of the solar tachocline III: Numerical solutions of the Gough and McIntyre model
- The magnetic strip(s) in the advanced phases of stellar evolution - Theoretical convective turnover timescale and Rossby number for low- and intermediate-mass stars up to the AGB at various metallicities
- Magnetic braking of stellar cores in red giants and supergiants
- The coupling between internal waves and shear-induced turbulence in stellar radiation zones: the critical layer
- Convective overshooting and penetration in a Boussinesq spherical shell
- Seismic probing of the first dredge-up event through the eccentric red-giant & red-giant spectroscopic binary KIC9163796
- Magnetic and tidal migration of close-in planets. Influence of secular evolution on their population
- A dominant magnetic dipole for the evolved Ap star candidate EK Eridani
- Characterizing the feedback of magnetic field on the differential rotation of solar-like stars
- Spherical-shell boundaries for two-dimensional compressible convection in a star
- Horizontal shear instabilities in rotating stellar radiation zones: II. Effects of the full Coriolis acceleration
- Magnetic signatures on mixed-mode frequencies. II. Period spacings as a probe of the internal magnetism of red giants
- Attempts to reproduce the rotation profile of the red giant KIC 7341231 observed by Kepler
- Detecting deep axisymmetric toroidal magnetic fields in stars. The traditional approximation of rotation for differentially rotating deep spherical shells with a general azimuthal magnetic field
- Magnetic field structure in single late-type giants: Beta Ceti in 2010 - 2012
- Transport by meridional circulations in solar-type stars
- Magnetic confinement of the solar tachocline: The oblique dipole
- A self-consistent model of the solar tachocline
- Confinement of the solar tachocline by a cyclic dynamo magnetic field
- Meridional Circulation Dynamics in a Cyclic Convective Dynamo
- Angular momentum transport, layering, and zonal jet formation by the GSF instability: nonlinear simulations at a general latitude
- Some glimpses from helioseismology at the dynamics of the deep solar interior
- A Compressible High-Order Unstructured Spectral Difference Code for Stratified Convection in Rotating Spherical Shells
- Magnetic field structure in single late-type giants: The weak G-band giant 37 Comae from 2008 to 2011
- Baroclinic Instability in Stellar Radiation Zones
- On the compatibility of a flux transport dynamo with a fast tachocline scenario
- On the dynamical interaction between overshooting convection and an underlying dipole magnetic field -- I. The non-dynamo regime
- The 2D dynamics of radiative zones of low-mass stars
- Constraining the Rotation Profile in a Low-Luminosity Subgiant with a Surface Rotation Measurement
- 2D dynamics of the radiative core of low mass stars
- Co-existence of Internal Gravity Waves and Tayler-Spruit Magnetic Fields in the Radiative Core of Low-mass Stars