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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 Open the ORCID record for Alexander Kosovichev [Opens in a new window] ,
Gustavo Guerrero ,
Andrey Stejko ,
Valery Pipin  and
Alexander Getling
Alexander Kosovichev
Affiliation:
Center for Computational Heliophysics, New Jersey Institute of Technology, University Heights, Newark, NJ 07102, U.S.A. email: alexander.g.kosovichev@njit.edu 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: alexander.g.kosovichev@njit.edu Physics Department, Universidade Federal de Minas Gerais Av. Antonio Carlos, 6627, Belo Horizonte, MG 31270-901, Brazil email: guerrero@fisica.ufmg.br
Andrey Stejko
Affiliation:
Center for Computational Heliophysics, New Jersey Institute of Technology, University Heights, Newark, NJ 07102, U.S.A. email: alexander.g.kosovichev@njit.edu
Valery Pipin
Affiliation:
Institute of Solar-Terrestrial Physics, Russian Academy of Sciences Irkutsk, 664033, Russia email: pip@iszf.irk.ru
Alexander Getling
Affiliation:
Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, 119991 Russia email: A.Getling@mail.ru
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Abstract

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.

Keywords

Sun: activitySun: helioseismologySun: magnetic fieldsSun: interiorMHDturbulence
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 333 - 352
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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