The influence of magnetic field topology and orientation on the 1 distribution of thermal electrons in the Martian magnetotail 2

This paper provides a brief overview of the formation of stellar fossil magnetic fields and what potential instabilities may occur given certain configurations of the magnetic field. One such instability is the purely magnetic Tayler instability, which can occur for poloidal, toroidal, and mixed poloidal-toroidal axisymmetric magnetic field configurations. However, most of the magnetic field configurations observed at the surface of massive stars are non-axisymmetric. Thus, extending earlier studies in spherical geometry, we introduce a formulation for the global change in the potential energy contained in a convectively-stable region for both axisymmetric and non-axisymmetric magnetic fields.

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Coronal mass ejection and solar flare initiation processes without appreciable changes of the large-scale magnetic field topology

Advances in Space Research ◽

10.1016/j.asr.2005.03.084 ◽

2006 ◽

Vol 37 (7) ◽

pp. 1305-1312 ◽

Cited By ~ 3

Author(s):

I.S. Veselovsky ◽

O.A. Panasenco

Keyword(s):

Magnetic Field ◽

Solar Flare ◽

Coronal Mass Ejection ◽

Large Scale ◽

Magnetic Field Topology ◽

Large Scale Magnetic Field ◽

Mass Ejection

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Influence of the Magnetic Field Topology on Hall Thruster Discharge Channel Wall Erosion

IEEE Transactions on Applied Superconductivity ◽

10.1109/tasc.2012.2185028 ◽

2012 ◽

Vol 22 (3) ◽

pp. 4904105-4904105 ◽

Cited By ~ 1

Author(s):

Chang Liu ◽

Zuo Gu ◽

Kan Xie ◽

Yunkui Sun ◽

Haibin Tang

Keyword(s):

Magnetic Field ◽

Channel Wall ◽

Discharge Channel ◽

Hall Thruster ◽

Magnetic Field Topology ◽

The Magnetic Field

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Magnetic field line braiding in the solar atmosphere

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317001818 ◽

2016 ◽

Vol 12 (S327) ◽

pp. 77-81

Author(s):

S. Candelaresi ◽

D. I. Pontin ◽

G. Hornig

Keyword(s):

Magnetic Field ◽

Magnetic Fields ◽

Solar Corona ◽

Field Line ◽

Solar Atmosphere ◽

Magnetic Field Line ◽

Solar Magnetic Field ◽

Near Surface ◽

Magnetic Field Topology ◽

The Magnetic Field

AbstractUsing a magnetic carpet as model for the near surface solar magnetic field we study its effects on the propagation of energy injectected by photospheric footpoint motions. Such a magnetic carpet structure is topologically highly non-trivial and with its magnetic nulls exhibits qualitatively different behavior than simpler magnetic fields. We show that the presence of magnetic fields connecting back to the photosphere inhibits the propagation of energy into higher layers of the solar atmosphere, like the solar corona. By applying certain types of footpoint motions the magnetic field topology is is greatly reduced through magnetic field reconnection which facilitates the propagation of energy and disturbances from the photosphere.

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