Elementary Plasma Physics

Longmire, C. L.; Payne, William T.

doi:10.1119/1.1969973

Cited by 119 publications

(97 citation statements)

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“…For nonrelativistic particles (for holes in a semiconductor crystal, the thermal velocity is much lower than the speed of light), it is equal to [1]: . Since during rotation the particle undergoes acceleration that is constant in magnitude and directed perpendicularly to the velocity, it is the source of radiation of electromagnetic waves at the frequency ω B [1][2][3]. Radiation of all charged carriers still determines the intensity of the cyclotron radiation of thermal plasma in a semiconductor crystal.…”

Section: Resultsmentioning

confidence: 99%

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High-frequency electromagnetic radiation of germanium crystals in magnetic fields

Milenin¹

2017

Semicond. Phys. Quantum Electron. Optoelectron.

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Section: Resultsmentioning

confidence: 99%

“…Plasma placed in a magnetic field radiates electromagnetic waves due to the rotation of charged carriers with a cyclotron frequency under the action of the Lorentz force [1][2][3]. The cyclotron radiation of semiconductor crystals is of interest for at least the following two reasons.…”

Section: Introductionmentioning

confidence: 99%

High-frequency electromagnetic radiation of germanium crystals in magnetic fields

Milenin¹

2017

Semicond. Phys. Quantum Electron. Optoelectron.

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“…It allows for separate ion, electron, and radiation tespcraturcs (a t'lanckian spectrun for he radiation Is assumed). (kJ/yg) , (12) [following Eq. …”

Section: Iktfioductiosmentioning

confidence: 99%

Thermonuclear burn characteristics of compressed deuterium-tritium microspheres

Fraley

Linnebur

Mason

et al. 1974

The Physics of Fluids

265

132

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The phenomenology of thermonuclear burn in deuterium-tritium microspheres at high densities is described, and numerical results characterizing the burn for a broad range of initial conditions are given. The fractional burnup, bootstrap-heating, and depletion of the DT fuel, its expansive disassembly, and thermonuclear ignition by propagating burn from central hot spots in the microspheres are discussed. Extensive numerical results from a 3 T Lagrangian simulation code are presented. The yields Y0 from uniform 10, 1, and 0.1 μg microspheres with densities ρ = 1 to 4 × 104 g/cm3 and temperatures Te = Ti = 1.8 to 100 keV are given. It is shown that Y0 ∼ ρR, ρR < 0.3 (R is the microsphere radius) or, equivalently, Y0 ∼ ρ2/3 for spheres of fixed mass m. The gain-factor G0 ≡ Y0/mI0 (I0 is the internal energy) is shown to measure burn efficiency in uniform microspheres. More than a four-fold increment in the gain factor is shown to derive from apportionment of the internal energy in a central hot spot. The limiting effects of electron degeneracy on the gain factor are outlined. As a guideline, the experimental observation of 1013 neutrons/kJ of input laser energy is established as proof of good absorption; 1015/kJ will imply yields exceeding break even.

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“…As has been discussed by Parker (1957) and Sweet (1958a), the magnetic configuration of sunspot groups is of the force-free type whenever the sunspot magnetic fields are stable, and so the magnetic lines of force extending into the solar atmosphere over the sunspot groups are necessarily twisted (Gold and Hoyle, 1960;Longmire, 1963;Sakurai, 1967). While accumulating magnetic energy within the magnetic flux tube through the twisting of magnetic lines of force, the magnetic configuration of sunspot groups gradually approach to an unstable state according to the discussion by Alfven (1950), Lundquist (1950) and Longmire (1963).…”

Section: Triggering Of Solar Proton Flares and The Acceleration Of Enmentioning

confidence: 99%

Magnetic Structure of Sunspot Groups which Produce Solar Proton Flares

Sakurai

1969

J. geomagn. geoelec

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Solar proton flares take place due to the release of magnetic energy accumulated within the sunspot magnetic flux tube of force lying in the chromosphere and the lower corona due to the twisting of it, which is seen from the rotational motion of sunspot groups on the photospheric surface. This rotational motion is counterclockwise (clockwise) in the northern (southern) hemisphere when viewed from the earth. The accumulation of magnetic energy within the flux tube due to this motion continues to proceed until some instability is induced along the flux tube. It is further shown that the magnetic configuration of sunspot groups is important for the triggering of a solar proton flare.

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Elementary Plasma Physics

Cited by 119 publications

References 0 publications

High-frequency electromagnetic radiation of germanium crystals in magnetic fields

High-frequency electromagnetic radiation of germanium crystals in magnetic fields

Thermonuclear burn characteristics of compressed deuterium-tritium microspheres

Magnetic Structure of Sunspot Groups which Produce Solar Proton Flares

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