scholarly journals The Influence of Magnetic Field Topology and Orientation on the Distribution of Thermal Electrons in the Martian Magnetotail

2021 ◽  
Vol 126 (3) ◽  
Author(s):  
Murti Nauth ◽  
Christopher M. Fowler ◽  
Laila Andersson ◽  
Gina A. DiBraccio ◽  
Shaosui Xu ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Field Topology

Magnetic field topology by MDI data: Active region

2012 ◽  
Vol 38 (8) ◽  
pp. 531-542 ◽  
Author(s):  
N. G. Makarenko ◽  
I. S. Knyazeva ◽  
L. M. Karimova
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Magnetic Field Topology

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

2020 ◽  
Author(s):  
Murti Nauth ◽  
Christopher M Fowler ◽  
Laila Andersson ◽  
Gina A Dibraccio ◽  
Shaosui Xu ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Field Topology

scholarly journals PERIODIC RADIO EMISSION FROM THE M7 DWARF 2MASS J13142039+1320011: IMPLICATIONS FOR THE MAGNETIC FIELD TOPOLOGY

2011 ◽  
Vol 741 (1) ◽  
pp. 27 ◽  
Author(s):  
M. McLean ◽  
E. Berger ◽  
J. Irwin ◽  
J. Forbrich ◽  
A. Reiners
Keyword(s):  
Magnetic Field ◽  
Radio Emission ◽  
Magnetic Field Topology ◽  
The Magnetic Field

scholarly journals On the magnetic field topology in reconnection region

2018 ◽  
Vol 1100 ◽  
pp. 012007
Author(s):  
G Consolini ◽  
V Quattrociocchi ◽  
M F Marcucci
Keyword(s):  
Magnetic Field ◽  
Magnetic Field Topology ◽  
Reconnection Region ◽  
The Magnetic Field

scholarly journals On the stability of a general magnetic field topology in stellar radiative zones

2019 ◽  
Vol 82 ◽  
pp. 365-371
Author(s):  
K. Augustson ◽  
S. Mathis ◽  
A. Strugarek
Keyword(s):  
Magnetic Field ◽  
Global Change ◽  
Magnetic Fields ◽  
Potential Energy ◽  
Massive Stars ◽  
Spherical Geometry ◽  
Stable Region ◽  
Magnetic Field Topology ◽  
The Stability ◽  
The Magnetic Field

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.

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

2012 ◽  
Vol 22 (3) ◽  
pp. 4904105-4904105 ◽  
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

scholarly journals Magnetic field line braiding in the solar atmosphere

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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