Turbulent Processes and Mean-Field Dynamo

被引:10
作者
Brandenburg, Axel [1 ,2 ,3 ,4 ,5 ,6 ]
Elstner, Detlef [7 ]
Masada, Youhei [8 ]
Pipin, Valery [9 ]
机构
[1] KTH Royal Inst Technol, Nordita, Hannes Alfvens Vag 12, S-10691 Stockholm, Sweden
[2] Stockholm Univ, Hannes Alfvens Vag 12, S-10691 Stockholm, Sweden
[3] Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden
[4] Ilia State Univ, Sch Nat Sci & Med, Tbilisi 0194, Georgia
[5] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA
[6] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA
[7] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany
[8] Fukuoka Univ, Dept Appl Phys, Fac Sci, Fukuoka 8140180, Japan
[9] Russian Acad Sci, Inst Solar Terr Phys, Irkutsk 664033, Russia
基金
瑞典研究理事会;
关键词
Large-scale dynamos; Turbulence; Stellar magnetism; Magnetic helicity; LARGE-SCALE DYNAMOS; SOLAR TORSIONAL OSCILLATIONS; DIRECT NUMERICAL SIMULATIONS; MAGNETIC HELICITY; CROSS-HELICITY; ROTATING MAGNETOCONVECTION; ASTROPHYSICAL DYNAMOS; ELECTROMOTIVE-FORCE; CONVECTION ZONE; NONLOCAL ALPHA;
D O I
10.1007/s11214-023-00999-3
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Mean-field dynamo theory has important applications in solar physics and galactic magnetism. We discuss some of the many turbulence effects relevant to the generation of large-scale magnetic fields in the solar convection zone. The mean-field description is then used to illustrate the physics of the a effect, turbulent pumping, turbulent magnetic diffusivity, and other effects on a modern solar dynamo model. We also discuss how turbulence transport coefficients are derived from local simulations of convection and then used in mean-field models.
引用
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页数:57
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