scholarly journals Relativistic Stars with Poloidal and Toroidal Magnetic Fields and Meridional Flow

2004 ◽  
Vol 600 (1) ◽  
pp. 296-316 ◽  
Author(s):  
Kunihito Ioka ◽  
Misao Sasaki
Keyword(s):  
Magnetic Fields ◽  
Meridional Flow ◽  
Relativistic Stars

Probing solar-cycle variations of magnetic fields in the convection zone using meridional flows

2019 ◽  
Vol 15 (S354) ◽  
pp. 160-165
Author(s):  
Chia-Hsien Lin ◽  
Dean-Yi Chou
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Convection Zone ◽  
Deep Convection ◽  
Meridional Flow ◽  
Meridional Plane ◽  
Solar Magnetic Fields ◽  
Magnetic Field Effects ◽  
Astrophysical Journal ◽  
The Magnetic Field

AbstractSolar magnetic fields are believed to originate from the base of convection zone. However, it has been difficult to obtain convincing observational evidence of the magnetic fields in the deep convection zone. The goal of this study is to investigate whether solar meridional flows can be used to detect the magnetic-field effects. Meridional flows are axisymmetric flows on the meridional plane. Our result shows that the flow pattern in the entire convection zone changes significantly from solar minimum to maximum. The changes all centered around active latitudes, suggesting that the magnetic fields are responsible for the changes. The results indicate that the meridional flow can be used to detect the effects of magnetic field in the deep convection zone.The results have been published in the Astrophysical Journal (lc2018).

scholarly journals Magnetohydrodynamic Simulation of the Evolution of Bipolar Magnetic Regions

1993 ◽  
Vol 141 ◽  
pp. 98-107 ◽  
Author(s):  
S. T. Wu ◽  
C. L. Yin ◽  
P. Mcintosh ◽  
E. Hildner
Keyword(s):  
Magnetic Fields ◽  
Magnetic Flux ◽  
Differential Rotation ◽  
Solar Surface ◽  
Effective Diffusion ◽  
Three Dimensional ◽  
Meridional Flow ◽  
Flux Transport ◽  
Turbulence Effects ◽  
Convective Motions

AbstractIt has been recognized that the magnetic flux observed on the solar surface appears first in low latitudes, and then this flux is gradually dispersed by super granular convective motions and meridional circulation. Theoretically, the magnetic flux transport could be explained by the interactions between magnetic fields and plasma flows on the solar surface through the theory of magnetohydrodynamics.To understand this physical scenario, a quasi-three-dimensional, time-dependent, MHD model with differential rotation, meridional flow and effective diffusion as well as cyclonic turbulence effects is developed. Numerical experiments are presented for the study of Bipolar Magnetic Regions (BMRs). When the MHD effects are ignored, our model produced the classical results (Leighton, Astrophys. J., 146, 1547, 1964). The full model’s numerical results demonstrate that the interaction between magnetic fields and plasma flow (i.e., MHD effects), observed together with differential rotation and meridional flow, gives rise to the observed complexity of the evolution of BMRs.

scholarly journals Large-Scale Flow Patterns in the Solar Atmosphere

1990 ◽  
Vol 142 ◽  
pp. 101-105
Author(s):  
K.R. Sivaraman
Keyword(s):  
Solar Cycle ◽  
Magnetic Fields ◽  
Time Evolution ◽  
Large Scale ◽  
Opposite Polarity ◽  
Meridional Flow ◽  
The Sun ◽  
Solar Cycle Variation ◽  
Large Scale Flow ◽  
Good Agreement

It is now well established (McIntosh 1979; Makarov and Sivaraman 1983) that the filament and filament channels seen in the H-alpha spectroheliograms (or filtergrams) can be used as reliable tracers for studying the time evolution of large-scale magnetic fields on the Sun. These features represent the neutral lines between the unipolar regions of opposite polarity. Comparison of the synoptic charts compiled from H-alpha pictures with those from full-disc magnetograms for the same period shows very good agreement and hence the former can be used with confidence for time evolution studies of large-scale unipolar regions for those periods when the magnetographs did not even exist. In this paper we shall present one of the results of our study (Makarov and Sivaraman 1983, 1989) on the migration of H-alpha filaments, namely, the existence of the meridional flow on the Sun. We shall extend it further to show the participation of this meridional flow in the solar cycle variation.

scholarly journals New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields

2019 ◽  
Vol 100 (12) ◽  
Author(s):  
Kōji Uryū ◽  
Shijun Yoshida ◽  
Eric Gourgoulhon ◽  
Charalampos Markakis ◽  
Kotaro Fujisawa ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Initial Data ◽  
Compact Objects ◽  
Relativistic Stars

scholarly journals INSTABILITY-DRIVEN EVOLUTION OF POLOIDAL MAGNETIC FIELDS IN RELATIVISTIC STARS

2011 ◽  
Vol 736 (1) ◽  
pp. L6 ◽  
Author(s):  
Riccardo Ciolfi ◽  
Samuel K. Lander ◽  
Gian Mario Manca ◽  
Luciano Rezzolla
Keyword(s):  
Magnetic Fields ◽  
Relativistic Stars ◽  
Poloidal Magnetic Fields

scholarly journals Magnetic fields in anisotropic relativistic stars

2015 ◽  
Vol 91 (4) ◽  
Author(s):  
Vladimir Folomeev ◽  
Vladimir Dzhunushaliev
Keyword(s):  
Magnetic Fields ◽  
Relativistic Stars ◽  
Anisotropic Relativistic Stars
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