Heat Flux Dependence of Ambipolar Potential and Plasma Profile in a Long Mean-Free-Path Plasma Along Non-Uniform Open Magnetic Field Lines

2012 ◽  
Vol 52 (5-6) ◽  
pp. 523-528 ◽  
Author(s):  
Z. Guo ◽  
X.-Z. Tang
Keyword(s):  
Magnetic Field ◽  
Heat Flux ◽  
Free Path ◽  
Mean Free Path ◽  
Field Lines ◽  
Plasma Profile ◽  
Open Magnetic Field

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

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

Quantum Theory of Stokes Parameters for Thomson Scattering in a Magnetised Plasma

1991 ◽  
Vol 9 (2) ◽  
pp. 325-325
Author(s):  
Chih-Kang Chou ◽  
Hui-Hwa Chen
Keyword(s):  
Magnetic Field ◽  
Angular Distribution ◽  
Quantum Theory ◽  
Free Path ◽  
Strong Magnetic Field ◽  
Cross Section ◽  
Mean Free Path ◽  
Thomson Scattering ◽  
Stokes Parameters ◽  
Scattering Process

Extended abstractThomson scattering in pulsar magnetospheres has previously been studied by several authors. The most distinguishing feature is the fact that the super-strong magnetic field (B ~ 1012 G) greatly affects the Thomson scattering process, resulting in resonances in the scattering cross-section (Canuto et al. 1971; Herold 1979; Chou 1986; Daugherty and Harding 1986). The important consequences of these cyclotron resonances are the increase in the photon mean free path in the scattering regions, and strongly affecting the angular distribution, and polarisation properties of the scattered photons (Chou 1986; Chou et al. 1989).

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).

Sign in / Sign up

Export Citation Format

Share Document