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Journal articles on the topic 'Plasma flow in magnetic field'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Ho, Ching Yen, Yu Hsiang Tsai, and Chung Ma. "Effects of External Magnetic Field on Intensity of Plasma Flow." Applied Mechanics and Materials 597 (July 2014): 272–75. http://dx.doi.org/10.4028/www.scientific.net/amm.597.272.

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This paper investigates the intensity distribution along the radial direction for plasma flow subject to external magnetic Field. The toroidal external magnetism is applied in the transverse direction of plasma flow. Considering the steady-state continuity and momentum of the plasma flow subject to external magnetic field, the intensity profile of the plasma is obtained. The results quantitatively verify the intensity enhancement of the plasma with the increasing external magnetic field.

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2

Nickeler, D. H., and T. Wiegelmann. "Thin current sheets caused by plasma flow gradients in space and astrophysical plasma." Annales Geophysicae 28, no. 8 (2010): 1523–32. http://dx.doi.org/10.5194/angeo-28-1523-2010.

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Abstract. Strong gradients in plasma flows play a major role in space and astrophysical plasmas. A typical situation is that a static plasma equilibrium is surrounded by a plasma flow, which can lead to strong plasma flow gradients at the separatrices between field lines with different magnetic topologies, e.g., planetary magnetospheres, helmet streamers in the solar corona, or at the boundary between the heliosphere and interstellar medium. Within this work we make a first step to understand the influence of these flows towards the occurrence of current sheets in a stationary state situation.

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MOHAPATRA, RANJITA K., P. S. SAUMIA, and AJIT M. SRIVASTAVA. "ENHANCEMENT OF FLOW ANISOTROPIES DUE TO MAGNETIC FIELD IN RELATIVISTIC HEAVY-ION COLLISIONS." Modern Physics Letters A 26, no. 33 (2011): 2477–86. http://dx.doi.org/10.1142/s0217732311036711.

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It is known that the presence of background magnetic field in cosmic plasma distorts the acoustic peaks in CMBR. This primarily results from different types of waves in the plasma with velocities depending on the angle between the magnetic field and the wave vector. We consider the consequences of these effects in relativistic heavy-ion collisions where very strong magnetic fields arise during early stages of the plasma evolution. We show that flow coefficients can be significantly affected by these effects when the magnetic field remains strong during early stages due to strong induced fields

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4

Alexeev, I. I., and V. V. Kalegaev. "Magnetic field and plasma flow structure near the magnetopause." Journal of Geophysical Research 100, A10 (1995): 19267. http://dx.doi.org/10.1029/95ja01345.

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5

Korobkin, Yu V., N. V. Lebedev, and V. L. Paperny. "Charge separation of plasma flow in curvilinear magnetic field." Technical Physics Letters 38, no. 3 (2012): 254–57. http://dx.doi.org/10.1134/s1063785012030248.

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6

Kotalik, P., and H. Nishiyama. "An effect of magnetic field on arc plasma flow." IEEE Transactions on Plasma Science 30, no. 1 (2002): 160–61. http://dx.doi.org/10.1109/tps.2002.1003973.

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7

Juusola, Liisa, Sanni Hoilijoki, Yann Pfau-Kempf, et al. "Fast plasma sheet flows and X line motion in the Earth's magnetotail: results from a global hybrid-Vlasov simulation." Annales Geophysicae 36, no. 5 (2018): 1183–99. http://dx.doi.org/10.5194/angeo-36-1183-2018.

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Abstract. Fast plasma flows produced as outflow jets from reconnection sites or X lines are a key feature of the dynamics in the Earth's magnetosphere. We have used a polar plane simulation of the hybrid-Vlasov model Vlasiator, driven by steady southward interplanetary magnetic field and fast solar wind, to study fast plasma sheet ion flows and related magnetic field structures in the Earth's magnetotail. In the simulation, lobe reconnection starts to produce fast flows after the increasing pressure in the lobes has caused the plasma sheet to thin sufficiently. The characteristics of the earth

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8

Rincon, François, Francesco Califano, Alexander A. Schekochihin, and Francesco Valentini. "Turbulent dynamo in a collisionless plasma." Proceedings of the National Academy of Sciences 113, no. 15 (2016): 3950–53. http://dx.doi.org/10.1073/pnas.1525194113.

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Magnetic fields pervade the entire universe and affect the formation and evolution of astrophysical systems from cosmological to planetary scales. The generation and dynamical amplification of extragalactic magnetic fields through cosmic times (up to microgauss levels reported in nearby galaxy clusters, near equipartition with kinetic energy of plasma motions, and on scales of at least tens of kiloparsecs) are major puzzles largely unconstrained by observations. A dynamo effect converting kinetic flow energy into magnetic energy is often invoked in that context; however, extragalactic plasmas

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9

Petralia, A., F. Reale, and P. Testa. "Guided flows in coronal magnetic flux tubes." Astronomy & Astrophysics 609 (December 22, 2017): A18. http://dx.doi.org/10.1051/0004-6361/201731827.

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Context. There is evidence that coronal plasma flows break down into fragments and become laminar. Aims. We investigate this effect by modelling flows confined along magnetic channels. Methods. We consider a full magnetohydrodynamic (MHD) model of a solar atmosphere box with a dipole magnetic field. We compare the propagation of a cylindrical flow perfectly aligned with the field to that of another flow with a slight misalignment. We assume a flow speed of 200 km s-1 and an ambient magnetic field of 30 G. Results. We find that although the aligned flow maintains its cylindrical symmetry while

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10

Alekseeva, Liliya M. "Instabilities of a Hall plasma flowing across a magnetic field." Laser and Particle Beams 15, no. 1 (1997): 65–72. http://dx.doi.org/10.1017/s0263034600010752.

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Under certain restrictions imposed on the plasma parameters, an analytical 2D solution to the magnetohydrodynamic equations, taking into account the Hall effect [of the HMHD (Hall magnetohydrodynamic) equations], is found for the case when plasma flows across a magnetic field. This solution has the form of the sum of a rather arbitrary steady flow and a small time-dependent disturbance. We show that waves of a purely acoustic nature can propagate against the background of the flow. The magnetic field manifests itself in this process only in that it produces an effective gravity force, the “gra

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11

Wei, Jian Ping, and Da Pei Tang. "Flow Characteristics of DC Plasma Torch Controlled by Magnetic Field." Applied Mechanics and Materials 268-270 (December 2012): 610–13. http://dx.doi.org/10.4028/www.scientific.net/amm.268-270.610.

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A magneto-hydrodynamic(MHD) model of magnetic controlled DC plasma torch is presented. The model includes the Navier-Stokes and the energy equations modified by the addition of some source terms, which reflect the Lorentz force due to the self-induced and the external magnetic fields, the radiative cooling and the Joule heating. In addition, the generalized Ohm's law, and the Maxwell's equations are also modeled. The MHD model is solved with the software FLUENT . The distribution of the velocity in the torch is obtained. The results show that the larger the current size of external current-car

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12

Tang, Da Pei, Qing Gao, Ying Hui Li, and Fan Xiu Lu. "Effect of External Magnetic Field on the Flow and Heat Transfer in DC Arc Plasma Torch." Advanced Materials Research 97-101 (March 2010): 2797–800. http://dx.doi.org/10.4028/www.scientific.net/amr.97-101.2797.

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A multiple fields’ coupled model of new magnetic controlled DC plasma torch, which was used for CVD diamond film, was presented. In this model, the effects of electric field and magnetic field on the flow field and temperature field were taken into account, and the fluid dynamics equations were modified by the addition of some source terms relating to electromagnetic field, such as Lorentz force, joule heating, and radiative cooling. Conversely, the generalized ohm’s law was used to solve the current density, which reflected the effects of flow field and temperature field on the electric field

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13

Bobashev, Sergei V., Yurii P. Golovachov, and David M. Van Wie. "Deceleration of Supersonic Plasma Flow by an Applied Magnetic Field." Journal of Propulsion and Power 19, no. 4 (2003): 538–46. http://dx.doi.org/10.2514/2.6164.

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14

Gupta, Sneha, and Devendra Sharma. "Plasma flow equilibria in 2D cylindrically symmetric expanding magnetic field." Physics of Plasmas 26, no. 9 (2019): 093501. http://dx.doi.org/10.1063/1.5090559.

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15

Timofeev, A. V. "Stability of the collisional plasma flow in a magnetic field." JETP Letters 97, no. 1 (2013): 5–9. http://dx.doi.org/10.1134/s0021364013010116.

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16

Hill, Jacqueline L., Amir Seyhoonzadeh, Hong-Young Chang, and Karl E. Lonngren. "On the flow of plasma around a dipole magnetic field." Radio Science 22, no. 7 (1987): 1211–18. http://dx.doi.org/10.1029/rs022i007p01211.

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17

Nakamura, R., D. N. Baker, D. H. Fairfield, D. G. Mitchell, and R. L. McPherron. "Plasma flow and magnetic field characteristics in the midtail region." Advances in Space Research 13, no. 4 (1993): 223–28. http://dx.doi.org/10.1016/0273-1177(93)90337-b.

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18

Frolova, Valeria P., Alexey G. Nikolaev, Efim M. Oks, et al. "Supersonic Flow of Vacuum Arc Plasma in a Magnetic Field." IEEE Transactions on Plasma Science 49, no. 9 (2021): 2478–89. http://dx.doi.org/10.1109/tps.2021.3088154.

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19

Dubinin, E. M., K. Sauer, and J. F. McKenzie. "Nonlinear 1-D stationary flows in multi-ion plasmas – sonic and critical loci – solitary and "oscillatory" waves." Annales Geophysicae 24, no. 11 (2006): 3041–57. http://dx.doi.org/10.5194/angeo-24-3041-2006.

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Abstract. One-dimensional stationary flows of a plasma consisting of two ion populations and electrons streaming against a heavy ion cloud are studied. The flow structure is critically governed by the position of sonic and critical points, at which the flow is shocked or choked. The concept of sonic and critical points is suitably generalized to the case of multi-ion plasmas to include a differential ion streaming. For magnetic field free flows, the sonic and critical loci in the (upx, uhx) space coincide. Amongst the different flow patterns for the protons and heavy ions, there is a possible

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20

Gus'kov, S. Yu, V. B. Rozanov, and T. Pisarczyk. "Magnetic control of the plasma flows in laser targets." Laser and Particle Beams 12, no. 3 (1994): 371–77. http://dx.doi.org/10.1017/s0263034600008223.

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The idea of controlling the plasma flows in laser targets by action of a strong external magnetic field (H ≥ 1 MG) is presented. The magnetic control of plasma flows for the keeping of a transparency of entrance holes of indirect-compression targets and other type targets operating at an introduction of the laser beams into the interior of the target is suggested. It is shown that the magnetic field, transverse versus the direction of the propagation of the plasma flow with an intensity of 2–4 MG, causes a decrease (1.5–3 times) of the closing speed of holes for the laser beam introduction int

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21

Mitrofanov, K. N., V. I. Krauz, V. V. Myalton, E. P. Velikhov, V. P. Vinogradov, and Yu V. Vinogradova. "Magnetic field distribution in the plasma flow generated by a plasma focus discharge." Journal of Experimental and Theoretical Physics 119, no. 5 (2014): 910–23. http://dx.doi.org/10.1134/s1063776114110168.

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22

IQBAL, M., and P. K. SHUKLA. "Beltrami fields in a hot electron–positron–ion plasma." Journal of Plasma Physics 78, no. 3 (2012): 207–10. http://dx.doi.org/10.1017/s0022377812000050.

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AbstractA possibility of relaxation of relativistically hot electron and positron (e − p) plasma with a small fraction of hot or cold ions has been investigated analytically. It is observed that a strong interaction of plasma flow and field leads to a non-force-free relaxed magnetic field configuration governed by the triple curl Beltrami (TCB) equation. The triple curl Beltrami (TCB) field composed of three different Beltrami fields gives rise to three multiscale relaxed structures. The results may have the strong relevance to some astrophysical and laboratory plasmas.

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23

Yahnin, A. G., I. V. Despirak, A. A. Lubchich, et al. "Indirect mapping of the source of the oppositely directed fast plasma flows in the plasma sheet onto the auroral display." Annales Geophysicae 24, no. 2 (2006): 679–87. http://dx.doi.org/10.5194/angeo-24-679-2006.

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Abstract. Data from Polar and Geotail spacecraft are combined to investigate the relationship between locations of active auroras and the magnetotail plasma sheet region where reversed fast plasma flows are generated during substorms. Using the magnetospheric magnetic field model, it is shown that at the beginning of the tailward fast flow the ionospheric footprint of the spacecraft measuring the flow tends to be located poleward of the auroral bulge. The spacecraft within the earthward flow is mapped equatorward of the poleward edge of the auroral bulge. We conclude that a source of the fast

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24

Campos Rozo, J. I., D. Utz, S. Vargas Domínguez, A. Veronig, and T. Van Doorsselaere. "Photospheric plasma and magnetic field dynamics during the formation of solar AR 11190." Astronomy & Astrophysics 622 (February 2019): A168. http://dx.doi.org/10.1051/0004-6361/201832760.

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Context. The Sun features on its surface typical flow patterns called the granulation, mesogranulation, and supergranulation. These patterns arise due to convective flows transporting energy from the interior of the Sun to its surface. The other well known elements structuring the solar photosphere are magnetic fields arranged from single, isolated, small-scale flux tubes to large and extended regions visible as sunspots and active regions. Aims. In this paper we will shed light on the interaction between the convective flows in large-scale cells as well as the large-scale magnetic fields in a

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25

Neubauer, F. M. "The Magnetic Field Structure of the Cometary Plasma Environment." International Astronomical Union Colloquium 116, no. 2 (1991): 1107–24. http://dx.doi.org/10.1017/s0252921100012847.

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AbstractThe plasma surrounding a comet has the interplanetary magnetic field frozen in. The geometric interpretation of this property is considered. The frozen-in character of the magnetic field leads to the draping of magnetic field lines around the inner coma, where, by exclusion of the inner purely cometary ionosphere, a magnetic cavity is formed inside a region of magnetic field pile-up. The consequences of these physical processes can nicely be diagnosed and tested by interplanetary tangential discontinuities serving as tracers of the magnetoplasma flow. The topology of the magnetic field

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26

Nishikawa, K. I., P. Hardee, B. Zhang, et al. "Magnetic field generation in a jet-sheath plasma via the kinetic Kelvin-Helmholtz instability." Annales Geophysicae 31, no. 9 (2013): 1535–41. http://dx.doi.org/10.5194/angeo-31-1535-2013.

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Abstract. We have investigated the generation of magnetic fields associated with velocity shear between an unmagnetized relativistic jet and an unmagnetized sheath plasma. We have examined the strong magnetic fields generated by kinetic shear (Kelvin–Helmholtz) instabilities. Compared to the previous studies using counter-streaming performed by Alves et al. (2012), the structure of the kinetic Kelvin–Helmholtz instability (KKHI) of our jet-sheath configuration is slightly different, even for the global evolution of the strong transverse magnetic field. In our simulations the major components o

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27

BOROVSKY, JOSEPH E., RICHARD C. ELPHIC, HERBERT O. FUNSTEN та MICHELLE F. THOMSEN. "The Earth's plasma sheet as a laboratory for flow turbulence in high-β MHD". Journal of Plasma Physics 57, № 1 (1997): 1–34. http://dx.doi.org/10.1017/s0022377896005259.

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The bulk flows and magnetic-field fluctuations of the plasma sheet are investigated using single-point measurements from the ISEE-2 Fast Plasma Experiment and fluxgate magnetometer. Ten several-hour-long intervals of continuous data (with 3 s and 12 s time resolution) are analysed. The plasma-sheet flow appears to be strongly ‘turbulent’ (i.e. the flow is dominated by fluctuations that are unpredictable, with rms velocities[Gt ]mean velocities and with field fluctuations≈mean fields). The flow velocities are typically sub-Alfvénic. The flow-velocity probability distribution P(v) is constructed

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28

Johansson, T., J. W. Bonnell, C. Cully, et al. "Observation of an inner magnetosphere electric field associated with a BBF-like flow and PBIs." Annales Geophysicae 27, no. 4 (2009): 1489–500. http://dx.doi.org/10.5194/angeo-27-1489-2009.

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Abstract. Themis E observed a perpendicular (to the magnetic field) electric field associated with an Earthward plasma flow at XGSM=−9.6 RE on 11 January 2008. The electric field observation resembles Cluster observations closer to Earth in the auroral region. The fast plasma flow shared some characteristics with bursty bulk flows (BBFs) but did not meet the usual criteria in maximum velocity and duration to qualify as one. Themis C observed the same flow further downtail but Themis D, separated by only 1 RE in azimuthal direction from Themis E, did not. At the time of the electric field and i

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29

Klimov, Aleksandr, and Aleksey Zenin. "Surface treatment by the ion flow from electron beam generated plasma in the forevacuum pressure range." MATEC Web of Conferences 143 (2018): 03008. http://dx.doi.org/10.1051/matecconf/201814303008.

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The paper presents research results of peculiarities of gas ion flows usage and their generation from large plasma formation (>50 sq.cm) obtained by electron beam ionization of gas in the forevacuum pressure range. An upgraded source was used for electron beam generation, which allowed obtaining ribbon electron beam with no transmitting magnetic field. Absence of magnetic field in the area of ion flow formation enables to obtain directed ion flows without distorting their trajectories. In this case, independent control of current and ion energy is possible. The influence of electron beam pa

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30

Timofeev, A. V. "Flow of a plasma of multielectron elements along a magnetic field." Plasma Physics Reports 37, no. 11 (2011): 978–87. http://dx.doi.org/10.1134/s1063780x11100072.

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31

Moritaka, Toseo, Yasuhiro Kuramitsu, Yao-Li Liu, and Shih-Hung Chen. "Spontaneous focusing of plasma flow in a weak perpendicular magnetic field." Physics of Plasmas 23, no. 3 (2016): 032110. http://dx.doi.org/10.1063/1.4942028.

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32

Nakamura, R., D. N. Baker, D. H. Fairfield, D. G. Mitchell, R. L. McPherron, and E. W. Hones. "Plasma flow and magnetic field characteristics near the midtail neutral sheet." Journal of Geophysical Research 99, A12 (1994): 23591. http://dx.doi.org/10.1029/94ja02082.

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33

Ebersohn, Frans H., J. P. Sheehan, Alec D. Gallimore, and John V. Shebalin. "Kinetic simulation technique for plasma flow in strong external magnetic field." Journal of Computational Physics 351 (December 2017): 358–75. http://dx.doi.org/10.1016/j.jcp.2017.09.021.

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34

Kozlov, A. N. "Numerical Model of Plasma Flow Injection in a Solenoid’s Magnetic Field." Mathematical Models and Computer Simulations 13, no. 1 (2021): 1–10. http://dx.doi.org/10.1134/s2070048221010129.

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35

Shukurov, A., and D. D. Sokoloff. "Hydromagnetic Dynamo in Astrophysical Jets." Symposium - International Astronomical Union 157 (1993): 367–71. http://dx.doi.org/10.1017/s0074180900174431.

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The origin of a regular magnetic field in astrophysical jets is discussed. It is shown that jet plasma flow can generate a magnetic field provided the streamlines are helical. The dynamo of this type, known as the screw dynamo, generates magnetic fields with the dominant azimuthal wave number m = 1 whose field lines also have a helical shape. The field concentrates into a relatively thin cylindrical shell and its configuration is favorable for the collimation and confinement of the jet plasma.

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36

Vörös, Z., W. Baumjohann, R. Nakamura, et al. "Multi-scale magnetic field intermittence in the plasma sheet." Annales Geophysicae 21, no. 9 (2003): 1955–64. http://dx.doi.org/10.5194/angeo-21-1955-2003.

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Abstract. This paper demonstrates that intermittent magnetic field fluctuations in the plasma sheet exhibit transitory, localized, and multi-scale features. We propose a multifractal-based algorithm, which quantifies intermittence on the basis of the statistical distribution of the "strength of burstiness", estimated within a sliding window. Interesting multi-scale phenomena observed by the Cluster spacecraft include large-scale motion of the current sheet and bursty bulk flow associated turbulence, interpreted as a cross-scale coupling (CSC) process.Key words. Magnetospheric physics (magnetot

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37

Mikhailenko, V. S., D. V. Chibisov, and V. V. Mikhailenko. "Shear-flow-driven ion cyclotron instabilities of magnetic field-aligned flow of inhomogeneous plasma." Physics of Plasmas 13, no. 10 (2006): 102105. http://dx.doi.org/10.1063/1.2354021.

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38

Phan, T. D., and B. U. Ö. Sonnerup. "MHD stagnation-point flows at a current sheet including viscous and resistive effects: general two-dimensional solutions." Journal of Plasma Physics 44, no. 3 (1990): 525–46. http://dx.doi.org/10.1017/s0022377800015361.

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Exact solutions are presented of two-dimensional steady-state incompressible stagnation point flows at a current sheet separating two colliding plasmas. They describe the process of resistive field annihilation (zero reconnection) where the magnetic field in each plasma is strictly parallel to the current sheet, but may have different magnitudes and direction on its two sides. The flow in the (x, y) plane toward the current sheet, located at x = 0, may have an arbitrary angle of incidence and an arbitrary amount of divergence from or convergence towards the stagnation point. We find the most g

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39

ONO, Norifumi, Kazuhiro MUSHA, and Kazuo KOIKE. "Control of Plasma Jet Using Strong Magnetic Field." JSME International Journal Series B 48, no. 3 (2005): 411–16. http://dx.doi.org/10.1299/jsmeb.48.411.

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40

Myshkin, Vyacheslav F., Dmitry A. Izhoykin, Ivan A. Ushakov, and Viktor F. Shvetsov. "Physical and Chemical Processes Research of Isotope Separation in Plasma under Magnetic Field." Advanced Materials Research 880 (January 2014): 128–33. http://dx.doi.org/10.4028/www.scientific.net/amr.880.128.

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It is known that chemical bonding is only possible when particles with antiparallel valence electrons spins orientation collide [1, 2]. In an external magnetic field unpaired electrons spins precession around the field lines is observed. Precession frequencies of valence electrons of magnetic and nonmagnetic nuclei differ, resulting in a different probability to collide in reactive state for different isotopes. The investigations results of magnetic field influence on the carbon isotopes redistribution between carbon dioxide and disperse carbon in plasmachemical processes are given. Argon-oxyg

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41

Janhunen, P. "Simulation study of the plasma-brake effect." Annales Geophysicae 32, no. 10 (2014): 1207–16. http://dx.doi.org/10.5194/angeo-32-1207-2014.

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Abstract. Plasma brake is a thin, negatively biased tether that has been proposed as an efficient concept for deorbiting satellites and debris objects from low Earth orbit. We simulate the interaction with the ionospheric plasma ram flow with the plasma-brake tether by a high-performance electrostatic particle in cell code to evaluate the thrust. The tether is assumed to be perpendicular to the flow. We perform runs for different tether voltage, magnetic-field orientation and plasma-ion mass. We show that a simple analytical thrust formula reproduces most of the simulation results well. The in

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42

Funaki, I., K. Ueno, H. Yamakawa, Y. Nakayama, T. Kimura, and H. Horisawa. "Interaction Between Plasma Flow and Magnetic Field in Scale Model Experiment of Magnetic Sail." Fusion Science and Technology 51, no. 2T (2007): 226–28. http://dx.doi.org/10.13182/fst07-a1357.

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43

Meng, Jian Bing, Xiao Juan Dong, and Chang Ning Ma. "Effects of External Transverse Alternating Magnetic Field on the Oscillating Amplitude of Atmospheric Pressure Plasma Arc." Advanced Materials Research 129-131 (August 2010): 692–96. http://dx.doi.org/10.4028/www.scientific.net/amr.129-131.692.

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A mathematical model was developed to describe the oscillating amplitude of the plasma arc injected transverse to an external transverse alternating magnetic field. The characteristic of plasma arc under the external transverse alternating magnetic field imposed perpendicular to the plasma current was discussed. The effect of processing parameters, such as flow rate of working gas, arc current, magnetic flux density and the standoff from the nozzle to the workpiece, on the oscillation of plasma arc were also analyzed. The results show that it is feasible to adjust the shape of the plasma arc b

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44

Sumner, Chloe, and Youra Taroyan. "Amplification of magnetic field twisting by a stagnation point flow." Astronomy & Astrophysics 642 (October 2020): A181. http://dx.doi.org/10.1051/0004-6361/202038761.

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Context. Flows are a common feature of many processes occurring in the solar atmosphere, such as the formation of prominences where evaporated plasma from the chromosphere condensates along thin prominence threads that are seen to twist and oscillate. Aim. We aim to investigate the twisting of these threads by plasma condensation during their formation. Methods. We introduce a simple model with fixed critical points where the flow speed matches the Alfvén speed. This allows us to study the problem separately in the sub-Alfvénic and super-Alfvénic regimes. The temporal and spatial evolution of

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45

Burman, Ron. "Distorted Dipole Magnetic Fields." International Astronomical Union Colloquium 160 (1996): 433–34. http://dx.doi.org/10.1017/s0252921100042044.

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Mestel et al. (1985; MRΩ2) introduced an axisymmetric pulsar magnetosphere model in which electrons leave the star with non-negligible speeds and flow with moderate acceleration, and with poloidal motion that is closely tied to poloidal magnetic field lines, before reachingSL, a limiting surface near which rapid acceleration occurs. As well as these Class I flows, there exist Class II flows which do not encounter a region of rapid acceleration (Burman 1984, 1985b). The formalism introduced by MRΩ2to describe the moderately accelerated flows can be interpreted in terms of a plasma drift across

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Iizuka, Satoru, Yasujiroh Minamitani, and Hiroshi Tanaca. "Particle and energy transport due to magnetic field-line reconnection in a tokamak." Journal of Plasma Physics 37, no. 3 (1987): 335–46. http://dx.doi.org/10.1017/s0022377800012228.

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Plasma behaviour during magnetic field-line reconnection which is driven by a rapid toroidal current reversal in a tokamak is investigated by calculating plasma flow speed from the magnetohydromatic equations with variables measured in the experiment. A strong plasma acceleration appears in the outside region of the X-type separatrix formed in the poloidal magnetic field lines. The induced electric field inside the plasma is evaluated directly from Ohm's law by using the fact that the toroidal current density vanishes during the current reversal. Then, plasma resistivity is estimated in the cr

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Longmore, M., S. J. Schwartz, and E. A. Lucek. "Rotation of the magnetic field in Earth's magnetosheath by bulk magnetosheath plasma flow." Annales Geophysicae 24, no. 1 (2006): 339–54. http://dx.doi.org/10.5194/angeo-24-339-2006.

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Abstract. Orientations of the observed magnetic field in Earth's dayside magnetosheath are compared with the predicted field line-draping pattern from the Kobel and Flückiger static magnetic field model. A rotation of the overall magnetosheath draping pattern with respect to the model prediction is observed. For an earthward Parker spiral, the sense of the rotation is typically clockwise for northward IMF and anticlockwise for southward IMF. The rotation is consistent with an interpretation which considers the twisting of the magnetic field lines by the bulk plasma flow in the magnetosheath. H

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De Keyser, J., M. Echim, and M. Roth. "Cross-field flow and electric potential in a plasma slab." Annales Geophysicae 31, no. 8 (2013): 1297–314. http://dx.doi.org/10.5194/angeo-31-1297-2013.

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Abstract. We consider cross-field plasma flow inside a field-aligned plasma slab embedded in a uniform background in a 1-dimensional geometry. This situation may arise, for instance, when long-lasting reconnection pulses inject plasma into the inner magnetosphere. The present paper presents a detailed analysis of the structure of the interfaces that separate the slab from the background plasma on either side; a fully kinetic model is used to do so. Since the velocity shear across both interfaces has opposite signs, and given the typical gyroradius differences between injected and background io

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Moawad, S. M. "Exact equilibria for nonlinear force-free magnetic fields with its applications to astrophysics and fusion plasmas." Journal of Plasma Physics 80, no. 2 (2014): 173–95. http://dx.doi.org/10.1017/s0022377813001050.

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AbstractKnowledge of the structure of coronal magnetic field originating from the photosphere is relevant to the understanding of many solar activity phenomena, e.g. flares, solar prominences, coronal loops, and coronal heating. In most of the existing literature, these loop-like magnetic structures are modeled as force-free magnetic fields (FFMF) without any plasma flow. In this paper, we present several exact solution classes for nonlinear FFMF, in both translational and axisymmetric geometries. The solutions are considered for their possible relevance to astrophysics and solar physics probl

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Potemra, T. A., M. J. Engebretson, L. J. Zanetti, R. E. Erlandson, and P. F. Bythrow. "Satellite observations of currents and waves in space plasmas." Laser and Particle Beams 6, no. 3 (1988): 503–11. http://dx.doi.org/10.1017/s0263034600005425.

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When viewed from outer space, the earth's magnetic field does not resemble a simple dipole, but is severely distorted into a comet-shaped configuration by the continuous flow of solar wind plasma. A complicated system of currents flows within this distorted magnetic field configuration called the ‘magnetosphere’ (See figure 1). For example, the compression of the geomagnetic field by the solar wind on the dayside of the earth is associated with a large-scale current flowing across the geomagnetic field lines, called the ‘Chapman-Ferraro’ or magnetopause current. The magnetospheric system inclu

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