Energy Loss of a Fast Ion in a Plasma

Butler, S. T.; Buckingham, Michael J.

doi:10.1103/physrev.126.1

Cited by 167 publications

(65 citation statements)

References 4 publications

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“…For ions, expressions for Λ are given in e.g. Butler and Buckingham (1962);Gould (1972a). For Λ ′ we used the Bethe-Bloch form (Olive and Particle Data Group, 2014), neglecting the correction for the polarisation of the medium which is negligible in the low-density conditions of the solar atmosphere.…”

Section: Discussionmentioning

confidence: 99%

Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT

et al. 2015

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Solar observations in the infrared domain can bring important clues on the response of the low solar atmosphere to primary energy released during flares. At present the infrared continuum has been detected at 30 THz (10 µm) in only a few flares. SOL2012-03-13 , which is one of these flares, has been presented and discussed in Kaufmann et al. (2013). No firm conclusions were drawn on the origin of the mid-infrared radiation. In this work we present a detailed multi-frequency analysis of the SOL2012-03-13 event, including observations at radio millimeter and sub-millimeter wavelengths, in hard X-rays (HXR), gamma-rays (GR), Hα, and white-light. HXR/GR spectral analysis shows that SOL2012-03-13 is a GR line flare and allows estimating the numbers of and energy contents in electrons, protons and α particles produced during the flare. The energy spectrum of the electrons producing the HXR/GR continuum is consistent with a broken power-law with an energy break at ∼ 800 keV. It is shown that the high-energy part (above ∼ 800 keV) of this distribution is responsible for the high-frequency radio emission (> 20 GHz) time-independent models of the quiet and flare atmospheres, we find that most (∼80%) of the observed 30 THz radiation can be attributed to thermal freefree emission of an optically-thin source. Using the F2 flare atmospheric model (Machado et al., 1980) this thin source is found to be at temperatures T ∼ 8000 K and is located well above the minimum temperature region. We argue that the chromospheric heating, which results in 80 % of the 30 THz excess radiation, can be due to energy deposition by non-thermal flare accelerated electrons, protons and α particles. The remaining 20% of the 30 THz excess emission is found to be radiated from an optically-thick atmospheric layer at T ∼ 5000 K, below the temperature minimum region, where direct heating by non-thermal particles is insufficient to account for the observed infrared radiation.

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Section: Discussionmentioning

confidence: 99%

Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT

et al. 2015

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“…We consider the test particle interaction only with the electron component of plasma, since it is this interaction that dominates the stopping of a test particle [19,20]. Besides, in contrast with the papers [10][11][12][13][14][15], Larmor rotation of a test particle in a magnetic field is taken into account.…”

Section: Introductionmentioning

confidence: 99%

Stopping of charged particles in a magnetized classical plasma

Nersisyan

1998

Phys. Rev. E

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The analytical and numerical investigations of the energy loss rate of the test particle in a magnetized electron plasma are developed on the basis of the Vlasov-Poisson equations, and the main results are presented. The Larmor rotation of a test particle in a magnetic field is taken into account. The analysis is based on the assumption that the energy variation of the test particle is much less than its kinetic energy. The obtained general expression for stopping power is analyzed for three cases: (i) the particle moves through a collisionless plasma in a strong homogeneous magnetic field; (ii) the fast particle moves through a magnetized collisionless plasma along the magnetic field; and (iii) the particle moves through a magnetized collisional plasma across a magnetic field. Calculations are carried out for the arbitrary test particle velocities in the first case, and for fast particles in the second and third cases. It is shown that the rate at which a fast test particle loses energy while moving across a magnetic field may be much higher than the loss in the case of motion through plasma without magnetic field.

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“…Simultaneously, in high density plasmas, "strong screening" [4] is also important, so we include its effect by Brysk's approximation for the Debye screening distance [5]. Besides S j is the same form as the Coulombic stopping power [6] while D j is the energy dispersion coefficient [7].…”

Section: Kinetic Model Equationmentioning

confidence: 99%

On the Ion Distribution Function in Degenerate Electron Plasmas

Sugita

Matsuura

Nakao

2013

Plasma and Fusion Research

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In highly-compressed plasmas as realized in inertial confinement fusion, the wave nature of electrons becomes noticeable and Pauli's exclusion principle restricts the energy transition of electrons remarkably. Such a state is called "electron degeneracy". In addition, the electron degeneracy may affect the energy distribution and temperature of coexisting ions through Coulombic ion-electron interaction. In order to evaluate these effects, we developed and solved the model equation for the distribution function of ions in degenerate electron plasmas. As a result, it is shown that the ion distribution function maintains a Maxwellian form at a temperature equal to that of degenerate electrons in thermal equilibrium because two effects of electron degeneracy-spectral hardening and Pauli blocking-counteract each other. Furthermore the electron degeneracy slows temperature relaxation between ions and electrons in non-thermal equilibrium.

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Energy Loss of a Fast Ion in a Plasma

Cited by 167 publications

References 4 publications

Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT

Origin of the 30 THz Emission Detected During the Solar Flare on 2012 March 13 at 17:20 UT

Stopping of charged particles in a magnetized classical plasma

On the Ion Distribution Function in Degenerate Electron Plasmas

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