On the dynamical interaction between overshooting convection and an underlying dipole magnetic field -- I. The non-dynamo regime
| Autor: | L. Korre, Pascale Garaud, Nicholas H. Brummell, Céline Guervilly |
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| Rok vydání: | 2020 |
| Předmět: |
Convection
astro-ph.SR Field (physics) MHD FOS: Physical sciences Tachocline Astronomy & Astrophysics 01 natural sciences 010305 fluids & plasmas Physics::Fluid Dynamics 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics 010303 astronomy & astrophysics convection Solar and Stellar Astrophysics (astro-ph.SR) Physics interiors [stars] Turbulent diffusion interior [Sun] Fluid Dynamics (physics.flu-dyn) Astronomy and Astrophysics Mechanics Physics - Fluid Dynamics Radiation zone physics.flu-dyn Convection zone Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science Magnetohydrodynamics Magnetic dipole Astronomical and Space Sciences |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, vol 503, iss 1 MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol 503, iss 1 |
| DOI: | 10.48550/arxiv.2008.01857 |
| Popis: | Motivated by the dynamics in the deep interiors of many stars, we study the interaction between overshooting convection and the large-scale poloidal fields residing in radiative zones. We have run a suite of 3D Boussinesq numerical calculations in a spherical shell that consists of a convection zone with an underlying stable region that initially compactly contains a dipole field. By varying the strength of the convective driving, we find that, in the less turbulent regime, convection acts as turbulent diffusion that removes the field faster than solely molecular diffusion would do. However, in the more turbulent regime, turbulent pumping becomes more efficient and partially counteracts turbulent diffusion, leading to a local accumulation of the field below the overshoot region. These simulations suggest that dipole fields might be confined in underlying stable regions by highly turbulent convective motions at stellar parameters. The confinement is of large-scale field in an average sense and we show that it is reasonably modeled by mean-field ideas. Our findings are particularly interesting for certain models of the Sun, which require a large-scale, poloidal magnetic field to be confined in the solar radiative zone in order to explain simultaneously the uniform rotation of the latter and the thinness of the solar tachocline. Comment: Accepted to MNRAS, 14 figures |
| Databáze: | OpenAIRE |
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