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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.
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页数:57
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