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Advances and Challenges in Observations and Modeling of the Global-Sun Dynamics and Dynamo

Published online by Cambridge University Press:  20 January 2023

Alexander Kosovichev
Affiliation:
Center for Computational Heliophysics, New Jersey Institute of Technology, University Heights, Newark, NJ 07102, U.S.A. email: [email protected] NASA Ames Research Center, Moffett Field, CA 94035 U.S.A.
Gustavo Guerrero
Affiliation:
Center for Computational Heliophysics, New Jersey Institute of Technology, University Heights, Newark, NJ 07102, U.S.A. email: [email protected] Physics Department, Universidade Federal de Minas Gerais Av. Antonio Carlos, 6627, Belo Horizonte, MG 31270-901, Brazil email: [email protected]
Andrey Stejko
Affiliation:
Center for Computational Heliophysics, New Jersey Institute of Technology, University Heights, Newark, NJ 07102, U.S.A. email: [email protected]
Valery Pipin
Affiliation:
Institute of Solar-Terrestrial Physics, Russian Academy of Sciences Irkutsk, 664033, Russia email: [email protected]
Alexander Getling
Affiliation:
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, 119991 Russia email: [email protected]
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Abstract

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Computational heliophysics has shed light on the fundamental physical processes inside the Sun, such as the differential rotation, meridional circulation, and dynamo-generation of magnetic fields. However, despite the substantial advances, the current results of 3D MHD simulations are still far from reproducing helioseismic inferences and surface observations. The reason is the multi-scale nature of the solar dynamics, covering a vast range of scales, which cannot be solved with the current computational resources. In such a situation, significant progress has been achieved by the mean-field approach, based on the separation of small-scale turbulence and large-scale dynamics. The mean-field simulations can reproduce solar observations, qualitatively and quantitatively, and uncover new phenomena. However, they do not reveal the complex physics of large-scale convection, solar magnetic cycles, and the magnetic self-organization that causes sunspots and solar eruptions. Thus, developing a synergy of these approaches seems to be a necessary but very challenging task.

Type
Contributed Paper
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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