scholarly journals Transport of Toroidal Magnetic Field by the Meridional Flow at the Base of the Solar Convection Zone

2006 ◽  
Vol 637 (2) ◽  
pp. 1135-1142 ◽  
Author(s):  
Matthias Rempel
Keyword(s):  
Magnetic Field ◽  
Convection Zone ◽  
Meridional Flow ◽  
Toroidal Magnetic Field ◽  
Solar Convection Zone ◽  
Solar Convection

scholarly journals Magnetic fields in the solar convection zone

2021 ◽  
Vol 18 (1) ◽  
Author(s):  
Yuhong Fan
Keyword(s):  
Magnetic Field ◽  
Convection Zone ◽  
Active Regions ◽  
Toroidal Magnetic Field ◽  
Near Surface ◽  
New Developments ◽  
Solar Convection Zone ◽  
Flux Tubes ◽  
Solar Convection ◽  
Dynamo Mechanism

AbstractIt has been a prevailing picture that active regions on the solar surface originate from a strong toroidal magnetic field stored in the overshoot region at the base of the solar convection zone, generated by a deep seated solar dynamo mechanism. This article reviews the studies in regard to how the toroidal magnetic field can destabilize and rise through the convection zone to form the observed solar active regions at the surface. Furthermore, new results from the global simulations of the convective dynamos, and from the near-surface layer simulations of active region formation, together with helioseismic investigations of the pre-emergence active regions, are calling into question the picture of active regions as buoyantly rising flux tubes originating from the bottom of the convection zone. This article also gives a review on these new developments.

scholarly journals Helicity transport from solar convection zone to interplanetary space

2012 ◽  
Vol 8 (S294) ◽  
pp. 505-518
Author(s):  
Mei Zhang
Keyword(s):  
Magnetic Field ◽  
Convection Zone ◽  
Interplanetary Space ◽  
Magnetic Helicity ◽  
Solar Photosphere ◽  
Solar Magnetic Fields ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Magnetic Flux Ropes ◽  
Solar Winds

AbstractMagnetic helicity is a physical quantity that describes field topology. It is also a conserved quantity as Berger in 1984 demonstrated that the total magnetic helicity is still conserved in the corona even when there is a fast magnetic reconnection. It is generally believed that solar magnetic fields, together with their helicity, are created in the convection zone by various dynamo processes. These fields and helicity are transported into the corona through solar photosphere and finally released into the interplanetary space via various processes such as coronal mass ejections (CMEs) and solar winds. Here I will give a brief review on our recent works, first on helicity observations on the photosphere and how to understand these observations via dynamo models. Mostly, I will talk about what are the possible consequences of magnetic helicity accumulation in the corona, namely, the formation of magnetic flux ropes, CMEs taking place as an unavoidable product of coronal evolution, and flux emergences as a trigger of CMEs. Finally, I will address on in what a form magnetic field in the interplanetary space would accommodate a large amount of magnetic helicity that solar dynamo processes have been continuously producing.

scholarly journals Mean-Field Magnetohydrodynamics of the Solar Convection Zone

1976 ◽  
Vol 71 ◽  
pp. 305-321
Author(s):  
F. Krause
Keyword(s):  
Magnetic Field ◽  
Velocity Field ◽  
Convection Zone ◽  
Solar Surface ◽  
Mean Field ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Random Character ◽  
Physical Quantities ◽  
The Magnetic Field

Observations of the solar surface show that some of the physical quantities, especially the velocity field and the magnetic field, show random character.

scholarly journals Helicity–vorticity turbulent pumping of magnetic fields in the solar dynamo

2012 ◽  
Vol 8 (S294) ◽  
pp. 367-368
Author(s):  
V. V. Pipin
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Differential Rotation ◽  
Large Scale ◽  
Convection Zone ◽  
Solar Dynamo ◽  
Solar Convection Zone ◽  
Solar Convection ◽  
Large Scale Magnetic Field ◽  
Convective Motions

AbstractThe interaction of helical convective motions and differential rotation in the solar convection zone results in turbulent drift of a large-scale magnetic field. We discuss the pumping mechanism and its impact on the solar dynamo.

scholarly journals MERIDIONAL FLOW IN THE SOLAR CONVECTION ZONE. I. MEASUREMENTS FROM GONG DATA

2014 ◽  
Vol 784 (2) ◽  
pp. 145 ◽  
Author(s):  
S. Kholikov ◽  
A. Serebryanskiy ◽  
J. Jackiewicz
Keyword(s):  
Convection Zone ◽  
Meridional Flow ◽  
Solar Convection Zone ◽  
Solar Convection

scholarly journals Formation of Arching Flux Tubes at the Base of the Solar Convection Zone

2001 ◽  
Vol 203 ◽  
pp. 273-275
Author(s):  
Y. Fan
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Linear Growth ◽  
Convection Zone ◽  
Active Regions ◽  
Solar Convection Zone ◽  
Flux Tubes ◽  
Solar Convection ◽  
Neutrally Buoyant ◽  
Dynamo Process

Solar active regions are believed to correspond to the topmost portions of Ω-shaped arching flux tubes that have risen buoyantly from the base of the solar convection zone, where strong toroidal magnetic fields are being generated by the dynamo process. The development of such emerging Ω-loops is likely a result of the buoyant instability associated with the submerged toroidal magnetic field. Using an anelastic MHD code, we simulate the formation of buoyant, arching flux tube structures as a result of the non-linear growth of the undular instability of a neutrally buoyant layer of horizontal, unidirectional magnetic field at the base of the solar convection zone.

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