Parallel heat flux and flow acceleration in open field line plasmas with magnetic trapping

Abstract The magnetic field of magnetars may be twisted compared with that of normal pulsars. Previous works mainly discussed magnetic energy release in the closed field line regions of magnetars. For a twisted magnetic field, the field lines will inflate in the radial direction. Similar to normal pulsars, the idea of light cylinder radius is introduced. More field lines will cross the light cylinder and become open for a twisted magnetic field. Therefore, magnetars may have a large polar cap, which may correspond to the hot spot during outburst. Particle flow in the open field line regions will result in the untwisting of the magnetic field. Magnetic energy release in the open field line regions can be calculated. The model calculations can catch the general trend of magnetar outburst: decreasing X-ray luminosity, shrinking hot spot etc. For magnetic energy release in the open field line regions, the geometry will be the same for different outburst in one magnetar.

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MHD turbulence and heating of the open field-line solar corona

Nonlinear Processes in Geophysics ◽

10.5194/npg-10-93-2003 ◽

2003 ◽

Vol 10 (1/2) ◽

pp. 93-100 ◽

Cited By ~ 13

Author(s):

W. H. Matthaeus ◽

D. J. Mullan ◽

P. Dmitruk ◽

L. Milano ◽

S. Oughton

Keyword(s):

Solar Corona ◽

Field Line ◽

Open Field ◽

Coronal Holes ◽

Low Frequency ◽

Small Scale ◽

Mhd Turbulence ◽

Ion Heating ◽

Open Field Line ◽

Intense Electron Beams

Abstract. This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations. Reflection from coronal inhomogeneities plays an important role in sustaining the cascade. Physical and observational constraints are discussed. Kinetic processes that convert cascaded energy into heat must occur in regions of turbulent small-scale reconnection, and may be similar in some respects to ion heating due to intense electron beams observed in the aurora.

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Full-fversion of GENE for turbulence in open-field-line systems

Physics of Plasmas ◽

10.1063/1.5008895 ◽

2018 ◽

Vol 25 (6) ◽

pp. 062303 ◽

Cited By ~ 10

Author(s):

Q. Pan ◽

D. Told ◽

E. L. Shi ◽

G. W. Hammett ◽

F. Jenko

Keyword(s):

Field Line ◽

Open Field ◽

Open Field Line

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Numerical Study on Acceleration and Deceleration Mechanism of Weakly Ionized Plasma Flowing Supersonically Through Open Field Line

IEEE Transactions on Plasma Science ◽

10.1109/tps.2014.2336254 ◽

2014 ◽

Vol 42 (12) ◽

pp. 3732-3741 ◽

Cited By ~ 6

Author(s):

Satoshi Tsuno ◽

Takeshi Nakahagi ◽

Ryutaro Yamashiro ◽

Atsushi Nezu ◽

Haruaki Matsuura ◽

...

Keyword(s):

Field Line ◽

Open Field ◽

Numerical Study ◽

Open Field Line ◽

Weakly Ionized ◽

Acceleration And Deceleration ◽

Weakly Ionized Plasma

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Large-scale auroral distribution and the open field line region

Planetary and Space Science ◽

10.1016/0032-0633(84)90046-1 ◽

1984 ◽

Vol 32 (1) ◽

pp. 105-109 ◽

Cited By ~ 4

Author(s):

J.S. Murphree ◽

C.D. Anger ◽

C.-I. Meng ◽

S.-I. Akasofu

Keyword(s):

Field Line ◽

Open Field ◽

Large Scale ◽

Line Region ◽

Open Field Line

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Magnetopause mapping to the ionosphere for northward IMF

Annales Geophysicae ◽

10.5194/angeo-25-2615-2007 ◽

2007 ◽

Vol 25 (12) ◽

pp. 2615-2625 ◽

Cited By ~ 4

Author(s):

I. I. Alexeev ◽

E. S. Belenkaya ◽

S. Yu. Bobrovnikov ◽

V. V. Kalegaev ◽

J. A. Cumnock ◽

...

Keyword(s):

Solar Wind ◽

Field Line ◽

Open Field ◽

Electric Fields ◽

Interplanetary Space ◽

Potential Drop ◽

Wind Pressure ◽

Polar Ionosphere ◽

Polar Cap ◽

Open Field Line

Abstract. We study the topological structure of the magnetosphere for northward IMF. Using a magnetospheric magnetic field model we study the high-latitude response to prolonged periods of northward IMF. For forced solar wind conditions we investigate the location of the polar cap region, the polar cap potential drop, and the field-aligned acceleration potentials, depending on the solar wind pressure and IMF By and Bx changes. The open field line bundles, which connect the Earth's polar ionosphere with interplanetary space, are calculated. The locations of the magnetospheric plasma domains relative to the polar ionosphere are studied. The specific features of the open field line regions arising when IMF is northward are demonstrated. The coefficients of attenuation of the solar wind magnetic and electric fields which penetrate into the magnetosphere are determined.

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