Download Magnetic Reconnection: MHD Theory and Applications by Eric Priest, Terry Forbes PDF
By Eric Priest, Terry Forbes
Magnetic reconnection is on the center of many dynamic phenomena within the universe, comparable to sun flares, geomagnetic substorms and tokamak disruptions. Written through international leaders at the topic, this quantity offers a accomplished review of this basic technique. insurance offers either a pedagogical account of the fundamental thought and a wide-ranging evaluation of the actual phenomena created by way of reconnection--from laboratory machines, the Earth's magnetosphere, and the Sun's surroundings to flare stars and astrophysical accretion disks. it's also a succinct account of particle acceleration via electrical fields, stochastic fields and surprise waves, and the way reconnection will be very important in those mechanisms. essentially written and hugely available, this quantity serves as a vital advent for graduate scholars in sun physics, astrophysics, plasma physics and house technology. Researchers in those fields will also locate Magnetic Reconnection an authoritative reference.
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Magnetic Reconnection: MHD Theory and Applications
Magnetic reconnection is on the center of many dynamic phenomena within the universe, corresponding to sun flares, geomagnetic substorms and tokamak disruptions. Written via international leaders at the topic, this quantity presents a entire evaluation of this primary method. insurance provides either a pedagogical account of the fundamental concept and a wide-ranging assessment of the actual phenomena created by way of reconnection--from laboratory machines, the Earth's magnetosphere, and the Sun's surroundings to flare stars and astrophysical accretion disks.
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Additional info for Magnetic Reconnection: MHD Theory and Applications
Example text
There are at least a dozen different approximations that are commonly used for the MHD system of equations. Some of the well-known ones are: incompressibility (p constant or V • v = 0); a steady state (d/dt = 0 for all variables); the Boussinesq approximation (filtering out sound waves by including density variations only in the gravitational term in the equation of motion); an isothermal state (T = constant or n large); an ideal MHD state (Rm ^> 1); an inviscid state (i? e ^>l); an irrotational (potential) flow ( 9. Notation for (a) a perpendicular shock and (b) an oblique shock. faster than its trough, causing a progressive steepening. Ultimately, the gradients become so large that dissipation becomes important, and a steady acoustic shock-wave shape may be attained, with a balance between the steepening effect of the nonlinear convective term and the broadening effect of dissipation. The dissipation inside the shock front converts the energy being carried by the wave gradually into heat. The effect of the passage of the shock is to compress and heat the gas. 2b list various plasma parameters along with the characteristic scale-lengths for four different regions where reconnection is thought to occur. The parameter Le is the global (external) scale-size of the region, and the fundamental quantities from which all other parameters are derived are the density, temperature, and magnetic field. For convenience, we assume that the Alfven Mach number (M) is unity and that the electron and ion temperatures are roughly equal. 2 occur in the magnetosphere, which is completely collisionless, and in the solar interior, which is highly collisional.