Thermal Convection, Magnetic Field, and Differential Rotation in Solar-type Stars
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Beschreibung
This thesis describes the studies on the solar interior where turbulent thermal convection plays an important role. The author solved, for the first time, one of the long-standing issues in solar physics, i.e., the maintenance mechanism of the solar differential rotation in the near-surface shear layer. The author attacked this problem with a newly developed approach, the reduced speed of sound technique, which enabled him to investigate the surface and deep solar layers in a self-consistent manner. This technique also made it possible to achieve an unprecedented performance in the solar convection simulations for the usage of the massively parallel supercomputers such as the RIKEN K system. It was found that the turbulence and the mean flows such as the differential rotation and the meridional circulation mutually interact with each other to maintain the flow structures in the Sun. Recent observations by helioseismology support the author's proposed theoretical mechanism. The book also addresses the generation of the magnetic field in such turbulent convective motions, which is an important step forward for solar cyclic dynamo research.
This thesis describes the studies on the solar interior where turbulent thermal convection plays an important role. The author solved, for the first time, one of the long-standing issues in solar physics, i.e., the maintenance mechanism of the solar differential rotation in the near-surface shear layer. The author attacked this problem with a newly developed approach, the reduced speed of sound technique, which enabled him to investigate the surface and deep solar layers in a self-consistent manner. This technique also made it possible to achieve an unprecedented performance in the solar convection simulations for the usage of the massively parallel supercomputers such as the RIKEN K system. It was found that the turbulence and the mean flows such as the differential rotation and the meridional circulation mutually interact with each other to maintain the flow structures in the Sun. Recent observations by helioseismology support the author's proposed theoretical mechanism. The book also addresses the generation of the magnetic field in such turbulent convective motions, which is an important step forward for solar cyclic dynamo research.
This is a prize winning thesis, nominated for Springer Theses by the University of Tokyo Reveals for the first time in the research filed, the understanding of the solar mechanism near surface shear layer Provides detailed description of the development of numerical code Contains numerical calculation of solar convection zone with highest number of grid points to help readers understand Includes supplementary material: sn.pub/extras
Autor*in
Hideyuki Hotta
Themen in »Thermal Convection, Magnetic Field, and Differential Rotation in Solar-type Stars«
Ionization Effect in Solar Global Model RIKEN K Computer Reduced Speed of Sound Technique (RSST) Solar Differential Rotation Solar Global Simulation Solar Local Dynamo in Global Scale