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Effects of rotation and surface forcing on deep stellar convection zones

Published online by Cambridge University Press:  23 December 2024

Petri J. Käpylä Open the ORCID record for Petri J. Käpylä [Opens in a new window]
Petri J. Käpylä*
Affiliation:
Leibniz-Insitute for Solar Physics (KIS), Schöneckstraße 6, 79104 Freiburg im Breisgau, Germany
*
email: pkapyla@leibniz-kis.de
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Abstract

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The canonical undestanding of stellar convection has recently been put under doubt due to helioseismic results and global 3D convection simulations. This “convective conundrum” is manifested by much higher velocity amplitudes in simulations at large scales in comparison to helioseismic results, and the difficulty in reproducing the solar differential rotation and dynamo with global 3D simulations. Here some aspects of this conundrum are discussed from the viewpoint of hydrodynamic Cartesian 3D simulations targeted at testing the rotational influence and surface forcing on deep convection. More specifically, the dominant scale of convection and the depths of the convection zone and the weakly subadiabatic – yet convecting – Deardorff zone are discussed in detail.

Keywords

ConvectionturbulenceSun: rotationSun: interior
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 5 - 15
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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