Physics of Fully Ionized Gases

Spitzer, Lyman; Seeger, Raymond J.

doi:10.1119/1.1969155

Cited by 939 publications

(636 citation statements)

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“…Li and Petrasso [24] define a Coulomb logarithm in terms of the combination of classical and quantum cutoffs as described above, namely 27) where 28) in which m pb is the reduced mass of the projectile (p) -plasma particle (b) system, and…”

Section: B Quantum Correctionsmentioning

confidence: 99%

“…For the Coulomb potential 36 , 14) where the phase φ is independent of l, and η is the generic quantum parameter. For the specific p-b system that we consider, η → η pb , where…”

Section: B Full Quantum Correctionmentioning

confidence: 99%

“…The overall coefficient of the Coulomb logarithm in the energy transfer rate (12.12) was obtained long ago by Spitzer [35] as described in his book [36]. However, our determination, as always, gives not only this coefficient, but also a precise definition of the value of the Coulomb logarithm, the constant under the Coulomb logarithm.…”

Section: A Introduction and Summarymentioning

confidence: 99%

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Charged particle motion in a highly ionized plasma

2005

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A recently introduced method utilizing dimensional continuation is employed to compute the energy loss rate for a non-relativistic particle moving through a highly ionized plasma. No restriction is made on the charge, mass, or speed of this particle. It is, however, assumed that the plasma is not strongly coupled in the sense that the dimensionless plasma coupling parameter g = e 2 κ D /4πT is small, where κ D is the Debye wave number of the plasma. To leading and next-to-leading order in this coupling, dE/dx is of the generic form g 2 ln[Cg 2 ]. The precise numerical coefficient out in front of the logarithm is well known. We compute the constant C under the logarithm exactly for arbitrary particle speeds. Our exact results differ from approximations given in the literature. The differences are in the range of 20% for cases relevant to inertial confinement fusion experiments. The same method is also employed to compute the rate of momentum loss for a projectile moving in a plasma, and the rate at which two plasmas at different temperatures come into thermal equilibrium. Again these calculations are done precisely to the order given above. The loss rates of energy and momentum uniquely define a Fokker-Planck equation that describes particle motion in the plasma. The coefficients determined in this way are thus well-defined, contain no arbitrary parameters or cutoffs, and are accurate to the order described. This FokkerPlanck equation describes the straggling -the spreading in the longitudinal position of a group of particles with a common initial velocity and positionand the transverse diffusion of a beam of particles. It should be emphasized that our work does not involve a model, but rather it is a precisely defined evaluation of the leading terms in a well-defined perturbation theory.

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Section: B Quantum Correctionsmentioning

confidence: 99%

“…For the Coulomb potential 36 , 14) where the phase φ is independent of l, and η is the generic quantum parameter. For the specific p-b system that we consider, η → η pb , where…”

Section: B Full Quantum Correctionmentioning

confidence: 99%

Section: A Introduction and Summarymentioning

confidence: 99%

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Charged particle motion in a highly ionized plasma

2005

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“…where η is the plasma resistivity (a measure of the collisionality of the plasma, see Spitzer (1956)) and J is the electric current density vector. The effect of finite conductivity on the diffusion of magnetic fields was already investigated for several configurations by Parker & Krook (1956).…”

Section: Dissipation Processmentioning

confidence: 99%

Three-dimensional magnetic reconnection and its application to solar flares

Janvier

2017

J. Plasma Phys.

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Solar flares are powerful radiations occurring in the Sun's atmosphere. They are powered by magnetic reconnection, a phenomenon that can convert magnetic energy into other forms of energy such as heat and kinetic energy, and which is believed to be ubiquitous in the universe. With the ever increasing spatial and temporal resolutions of solar observations, as well as numerical simulations benefiting from increasing computer power, we can now probe into the nature and the characteristics of magnetic reconnection in three dimensions to better understand the phenomenon's consequences during eruptive flares in our star's atmosphere. We review in the following the efforts made on different fronts to approach the problem of magnetic reconnection. In particular, we will see how understanding the magnetic topology in three dimensions helps in locating the most probable regions for reconnection to occur, how the current layer evolves in three dimensions and how reconnection leads to the formation of flux ropes, plasmoids and flaring loops.

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“…Averaging over a Maxwellian velocity distribution, Spitzer derived a relation giving the relaxation time constant for equilibrating temperatures in a two-component plasma [8].…”

Section: Theoretical Framework For Electron Coolingmentioning

confidence: 99%