Numerical study of electric potential formation in a weakly ionized plasma flowing supersonically through open magnetic field lines

2016 ◽  
Vol 56 (1) ◽  
pp. 016201
Author(s):  
Ampan Laosunthara ◽  
Jun Takeda ◽  
Hiroshi Akatsuka
Keyword(s):  
Magnetic Field ◽  
Electric Potential ◽  
Numerical Study ◽  
Weakly Ionized ◽  
Potential Formation ◽  
Weakly Ionized Plasma ◽  
Field Lines ◽  
Open Magnetic Field

Frozen-In Magnetic Field Lines and Alfvén Wave Generation in Weakly Ionized Plasma

Solar Physics ◽  
2015 ◽  
Vol 290 (7) ◽  
pp. 1923-1929
Author(s):  
Y. T. Tsap ◽  
A. V. Stepanov ◽  
Y. G. Kopylova
Keyword(s):  
Magnetic Field ◽  
Wave Generation ◽  
Alfven Wave ◽  
Weakly Ionized ◽  
Weakly Ionized Plasma ◽  
Field Lines ◽  
Alfvén Wave Generation

Collisionless plasma transport mechanisms in stochastic open magnetic field lines in tokamaks

2021 ◽  
Author(s):  
Min-Gu Yoo ◽  
Weixing Wang ◽  
Edward A Startsev ◽  
Chenhao Ma ◽  
S Ethier ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Collisionless Plasma ◽  
Plasma Transport ◽  
Transport Mechanisms ◽  
Field Lines ◽  
Open Magnetic Field

Fluid description of collisional current filamentation instability of a weakly ionized plasma in the presence of magnetic field

2019 ◽  
Vol 19 (1) ◽  
pp. 157-166
Author(s):  
K Hajisharifi ◽  
S Tajik-Nezhad ◽  
H Mehdian ◽  
◽  
◽  
...  
Keyword(s):  
Magnetic Field ◽  
Weakly Ionized ◽  
Weakly Ionized Plasma ◽  
Filamentation Instability

scholarly journals Dynamical Galactic Halos

1993 ◽  
Vol 157 ◽  
pp. 415-419
Author(s):  
D. Breitschwerdt ◽  
H.J. Völk ◽  
V. Ptuskin ◽  
V. Zirakashvili
Keyword(s):  
Magnetic Field ◽  
Cosmic Rays ◽  
The Other ◽  
Galactic Rotation ◽  
Galactic Halos ◽  
Magnetic Forces ◽  
Dynamical Coupling ◽  
Field Lines ◽  
The Magnetic Field ◽  
Open Magnetic Field

It is argued that the description of the magnetic field in halos of galaxies should take into account its dynamical coupling to the other major components of the interstellar medium, namely thermal plasma and cosmic rays (CR's). It is then inevitable to have some loss of gas and CR's (galactic wind) provided that there exist some “open” magnetic field lines, facilitating their escape, and a sufficient level of self-generated waves which couple the particles to the gas. We discuss qualitatively the topology of the magnetic field in the halo and show how galactic rotation and magnetic forces can be included in such an outflow picture.

Ballooning modes on open magnetic field lines

1999 ◽  
Vol 6 (3) ◽  
pp. 674-685 ◽  
Author(s):  
Eliezer Hameiri
Keyword(s):  
Magnetic Field ◽  
Field Lines ◽  
Open Magnetic Field

scholarly journals Transition Between Type I and Type III Bursts in Closed or Open Magnetic Field Lines

1980 ◽  
Vol 86 ◽  
pp. 363-368
Author(s):  
Monique G. Aubier
Keyword(s):  
Magnetic Field ◽  
Velocity Component ◽  
Low Frequency ◽  
Critical Value ◽  
Type I ◽  
Accelerated Electrons ◽  
Type Iii ◽  
Field Lines ◽  
Parallel Momentum ◽  
Open Magnetic Field

When studying the propagation of accelerated electrons outwards in the corona, we have shown that the perpendicular momentum of the electrons remaining after the type I process is transformed into parallel momentum during the propagation along the decreasing magnetic field, and that type III emission can occur when the parallel velocity component reaches a critical value. With this model we explain in particular the low frequency cut-off of type I emission, the characteristics of the type III bursts near their starting frequency and the transition between type III- and type I-like decameter emission observed in few cases.

Examining the optical intensity and magnetic field expansion factor in the open magnetic field regions associated with coronal holes

2019 ◽  
Vol 15 (S354) ◽  
pp. 228-231
Author(s):  
Chia-Hsien Lin ◽  
Guan-Han Huang ◽  
Lou-Chuang Lee
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Coronal Holes ◽  
Closed Field ◽  
Logarithmic Scale ◽  
Expansion Factor ◽  
Astrophysical Journal ◽  
Field Lines ◽  
The Relationship ◽  
Open Magnetic Field

AbstractCoronal holes can be identified as the darkest regions in EUV or soft X-ray images with predominantly unipolar magnetic fields (LIRs) or as the regions with open magnetic fields (OMF). Our study reveals that only 12% of OMF regions are coincident with LIRs. The aim of this study is to investigate the conditions that affect the EUV intensity of OMF regions. Our results indicate that the EUV intensity and the magnetic field expansion factor of the OMF regions are weakly positively correlated when plotted in logarithmic scale, and that the bright OMF regions are likely to locate inside or next to the regions with closed field lines. We empirically determined a linear relationship between the expansion factor and the EUV intensity. The relationship is demonstrated to improve the consistency from 12% to 23%. The results have been published in Astrophysical Journal (Huang et al. 2019).

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