Glow dynamics of the spark channel and detached shock wave at high gradients of the magnetic field pressure

2011 ◽  
Vol 37 (7) ◽  
pp. 638-642 ◽  
Author(s):  
O. A. Omarov ◽  
Sh. Sh. El’darov ◽  
M. Sh. El’darov
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Detached Shock Wave ◽  
High Gradients ◽  
Spark Channel ◽  
The Magnetic Field

scholarly journals Magnetorotational supernovae with different equations of state

2011 ◽  
Vol 7 (S279) ◽  
pp. 357-358
Author(s):  
Sergey G. Moiseenko ◽  
Gennady S. Bisnovatyi-Kogan
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Angular Momentum ◽  
Differential Rotation ◽  
Equations Of State ◽  
Supernova Explosion ◽  
Explosion Energy ◽  
Iron Core ◽  
Wave Forms ◽  
The Magnetic Field

AbstractWe present results of the simulation of a magneto-rotational supernova explosion. We show that, due to the differential rotation of the collapsing iron core, the magnetic field increases with time. The magnetic field transfers angular momentum and a MHD shock wave forms. This shock wave produces the supernova explosion. The explosion energy computed in our simulations is 0.5-2.5 ċ 1051erg. We used two different equations of state for the simulations. The results are rather similar.

Magneto-gasdynamic flow over a wedge

1966 ◽  
Vol 25 (1) ◽  
pp. 165-178 ◽  
Author(s):  
D. C. Pack ◽  
G. W. Swan
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Shock Waves ◽  
Wave Pattern ◽  
Ionized Gas ◽  
Current Sheets ◽  
Gasdynamic Flow ◽  
The Stability ◽  
The Magnetic Field ◽  
Insight Into

The solution for the flow of a fully ionized gas over a wedge of finite angle is known for the case when the applied magnetic field is aligned with the incident stream. In this flow there are current sheets on the surfaces of the wedge. When the magnetic field is allowed to deviate slightly from the stream, the current sheets may move into the gas and become shock waves. The magnetic fields adjacent to the wedge above and below it have to be matched. A perturbation method is introduced by means of which expressions for the unknown quantities in the different regions may be determined when there are four shocks attached to the wedge. The results give insight into the manner in which the shock-wave pattern develops as the obliquity of the magnetic field to the stream increases. The question of the stability of the shock waves is also examined.

Investigation of the magnetic field between the shock wave and the obstacle in the solar wind flow around a planet

1981 ◽  
Vol 1 (1) ◽  
pp. 101-104
Author(s):  
V.B. Boranov ◽  
E.G. Eroshenko ◽  
M.D. Kartalev ◽  
I.P. Mastikov
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Solar Wind ◽  
Wind Flow ◽  
Solar Wind Flow ◽  
The Magnetic Field

scholarly journals Particle Acceleration in the Process of Eruptive Opening and Reconnection of Magnetic Fields

1980 ◽  
Vol 91 ◽  
pp. 217-221 ◽  
Author(s):  
Z. Švestka ◽  
S. F. Martin ◽  
R. A. Kopp
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Particle Acceleration ◽  
Magnetic Fields ◽  
Magnetic Loop ◽  
Coronal Loops ◽  
X Rays ◽  
Flare Loops ◽  
Field Lines ◽  
The Magnetic Field

In a series of papers on the flare of 29 July 1973 (Nolte et al., 1979; Martin, 1979; Švestka et al., 1979) it has been shown that Hα “post-flare” loops are the cooled aftermath of previously hot coronal loops which were visible in x-rays in the same position earlier in the flare. Kopp and Pneuman (1976) have proposed that these post-flare loops are formed by a process of successive magnetic field reconnections of previously distended magnetic field lines as illustrated in Figure 1. Each successive reconnection of the magnetic field yields a closed magnetic loop that forms above and concentric with previously formed loops. A shock wave created during each sudden reconnection travels down both legs of each loop and provides energy for ionizing chromospheric mass at the footpoints of the loop. Subsequent condensation of the ionized mass at the tops of the loops renders them visible as this mass falls to the chromosphere.

scholarly journals Particle Acceleration and Radio Emission of the Supernovae Remnants at Different Stages of their Evolution

1983 ◽  
Vol 101 ◽  
pp. 183-186
Author(s):  
V. N. Fedorenko
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Particle Acceleration ◽  
Radio Emission ◽  
Temporal Evolution ◽  
Relativistic Electrons ◽  
List Type ◽  
Type Number ◽  
Physical Processes ◽  
The Magnetic Field

In this Paper, I consider physical processes, governing relativistic electrons in SNRs. a)SNRs at the age t > 102 yr. I argue that the shock wave acceleration faces some difficulties. Then I show that the temporal evolution of the SNRs radio emission can be accounted for without involving the acceleration.b)SNRs at the age t < 102 yr. I associate the lack of radio emission at this stage (Brown and Marscher, 1978) with the weakness of the magnetic field.c)I infer that the most efficient particle acceleration and radio emission of the SNRs should occur at the stage t ~ 102 yr.

The structure of the turbulent shock wave propagating in the solar atmosphere across the magnetic field

Solar Physics ◽  
1978 ◽  
Vol 60 (2) ◽  
pp. 279-291 ◽  
Author(s):  
V. V. Zaitsev ◽  
O. G. Parfenov ◽  
A. V. Stepanov
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Solar Atmosphere ◽  
The Magnetic Field

scholarly journals Probing the Interstellar Magnetic Field by Polarization Observations of Supernova Remnants

1990 ◽  
Vol 140 ◽  
pp. 73-75
Author(s):  
Ernst Fürst ◽  
Wolfgang Reich
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Linear Polarization ◽  
Supernova Remnants ◽  
Bilateral Symmetry ◽  
Galactic Magnetic Field ◽  
Polarization Measurements ◽  
The Magnetic Field

We present a comparison of the Galactic magnetic field and the magnetic field of three supernova remnants (SNRs) of bilateral symmetry derived from linear polarization measurements. These data are best explained if a quasi-perpendicular propagation of the SNR-shock wave is assumed.

scholarly journals Shock waves in gas and plasma

1996 ◽  
Vol 14 (2) ◽  
pp. 125-132 ◽  
Author(s):  
K. Niu
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Inertial Confinement Fusion ◽  
Magnetized Plasma ◽  
Irreversible Processes ◽  
Wave Flow ◽  
Discontinuous Surface ◽  
Neutral Gas ◽  
The Magnetic Field ◽  
Free Shock

A shock wave is a discontinuous surface that connects supersonic flow with subsonic flow. After a shock wave, flow velocity is reduced, and pressure and temperature increase; entropy especially increases across a shock wave. Therefore, flow is in nonequilibrium, and irreversible processes occur inside the shock layer. The thickness of a shock wave in neutral gas is of the order of the mean free path of the fluid particle. A shock wave also appears in magnetized plasma. Provided that when the plasma flow is parallel to the magnetic field, a shock wave appears if the governing equation for velocity potential is in hyperbolic type in relation with the Mach number and the Alfvén number. When the flow is perpendicular to the magnetic field, the Maxwell stress, in addition to the pressure, plays a role in the shock wave in plasma. When the plasma temperature is so high, as the plasma becomes collision-free, another type of shock wave appears. In a collision-free shock wave, gyromotions of electrons around the magnetic field lines cause the shock formation instead of collisions in a collision-dominant plasma or neutral gas. Regardless of a collision-dominant or collision-free shock wave, the fluid that passes through the shock wave is heated in addition to being compressed. In inertial confinement fusion, the fuel must be compressed. Really, implosion motion performs fuel compression. A shock wave, appearing in the process of implosion, compresses the fuel. The shock wave, however, heats the fuel more intensively, and it makes it difficult to compress the fuel further because high temperatures invite high pressure. Adiabatic compression of the fuel is the desired result during the implosion, without the formation of a shock wave.

scholarly journals Propagation of Shock Waves in a Polytrope with a Poloidal Magnetic Field

1968 ◽  
Vol 21 (5) ◽  
pp. 681
Author(s):  
Narendra K Sinha
Keyword(s):  
Magnetic Field ◽  
Shock Wave ◽  
Shock Waves ◽  
Poloidal Magnetic Field ◽  
The Magnetic Field

The propagation of a spherically developed shock wave in a poly trope with a poloida.l magnetic field has been studied using a generalization of Whitham's method. The effect of the magnetic field on the geometry of the front as well as on the effects brought about by the shock has been discussed.

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