Relevant bibliographies by topics / Electron Clouds

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  1. Journal articles

Academic literature on the topic 'Electron Clouds'

Author: Grafiati
Published: 7 September 2023

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Journal articles on the topic "Electron Clouds"

1

Lehmann, Andrew, and Mark Wardle. "Diffusion of cosmic-ray electrons in the Galactic centre molecular cloud G0.13–0.13." Proceedings of the International Astronomical Union 9, S303 (2013): 434–38. http://dx.doi.org/10.1017/s1743921314001082.

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AbstractThe Galactic center (GC) molecular cloud G0.13–0.13 exhibits a shell morphology in CS J = (1 − 0), with ∼ 105 solar masses and expansion speed ∼ 20 km s−1, yielding a total kinetic energy ∼ 1051 erg. Its morphology is also suggestive of an interaction with the nonthermal filaments of the GC arc. 74 MHz emission indicates the presence of a substantial population of low energy electrons permeating the cloud, which could either be produced by the interaction with the arc or accelerated in the shock waves responsible for the cloud's expansion. These scenarios are explored using time dependent diffusion models.With these diffusion models, we determine the penetration of low-energy cosmic-ray electrons accelerated into G0.13–0.13 and calculate the spatial distribution of the cosmic-ray ionization and heating rates. We show that the 6.4 keV Fe Kα line emission associated with the electron population provides an observational diagnostic to distinguish these two acceleration scenarios.We discuss the implications of our results for understanding the distinct character of clouds in the central molecular zone compared to clouds in the Galactic disk, and how GC nonthermal filaments interact with molecular clouds.
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2

Bakhareva, O. A., V. Yu Sergeev, and I. A. Sharov. "On the Formation of a Plasma Cloud at the Ablation of a Pellet in a High-Temperature Magnetized Toroidal Plasma." JETP Letters 117, no. 3 (2023): 207–13. http://dx.doi.org/10.1134/s0021364022603190.

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The investigation of cold secondary plasma clouds near pellets ablating in the hot plasma of magnetic confinement devices (tokamaks and stellarators) provides valuable information on the physical characteristics of a pellet cloud. In this work, the characteristic sizes of emitting clouds around fusible polystyrene pellets and refractory carbon pellets have been analyzed. The calculation of the ionization length of C+ ions in both carbon and hydrocarbon clouds has shown that the contribution of only hot electrons is insufficient to ensure the experimentally observed decay lengths of the CII line intensity. Taking into account the strong shielding of the electron flux of the background plasma in the hydrocarbon pellet cloud, the ionization of C+ ions in this cloud is determined predominantly by electrons of the cold plasma of the cloud. Shielding near a refractory carbon pellet is weak because its ablation rate is lower. The contributions from hot electrons of the surrounding plasma and cold electrons of the pellet cloud to the ionization of C+ ions are comparable in the case of carbon pellets.
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3

Le Bars, G., J. Loizu, J. Ph Hogge, et al. "First self-consistent simulations of trapped electron clouds in a gyrotron gun and comparison with experiments." Physics of Plasmas 30, no. 3 (2023): 030702. http://dx.doi.org/10.1063/5.0136340.

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We report on the initial validation of the novel code FENNECS, which simulates the spontaneous formation of trapped electron clouds in coaxial geometries with strong externally applied azimuthal flows and in the presence of a residual neutral gas. For this purpose, a realistic gyrotron electron gun geometry is used in the code, and a self-consistent electron cloud build-up is simulated. The predicted electronic current resulting from these clouds that is collected on the gun electrodes is simulated and successfully compared with the previous experimental results for configurations with different externally applied electric and magnetic fields. These different configurations effectively modify the size and depth of the trapping potential wells responsible for the confinement of the electron clouds. This investigation also provides further insight into the link between potential well depth and resulting electronic current.
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4

John, P. I. "Physics of toroidal electron clouds." Plasma Physics and Controlled Fusion 34, no. 13 (1992): 2053–59. http://dx.doi.org/10.1088/0741-3335/34/13/039.

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5

Tkachev, A. N., and S. I. Yakovlenko. "Electron clouds around charged particulates." Technical Physics 44, no. 1 (1999): 48–52. http://dx.doi.org/10.1134/1.1259250.

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6

Dimant, Y. S., and M. M. Oppenheim. "Interaction of plasma cloud with external electric field in lower ionosphere." Annales Geophysicae 28, no. 3 (2010): 719–36. http://dx.doi.org/10.5194/angeo-28-719-2010.

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Abstract. In the auroral lower-E and upper-D region of the ionosphere, plasma clouds, such as sporadic-E layers and meteor plasma trails, occur daily. Large-scale electric fields, created by the magnetospheric dynamo, will polarize these highly conducting clouds, redistributing the electrostatic potential and generating anisotropic currents both within and around the cloud. Using a simplified model of the cloud and the background ionosphere, we develop the first self-consistent three-dimensional analytical theory of these phenomena. For dense clouds, this theory predicts highly amplified electric fields around the cloud, along with strong currents collected from the ionosphere and circulated through the cloud. This has implications for the generation of plasma instabilities, electron heating, and global MHD modeling of magnetosphere-ionosphere coupling via modifications of conductances induced by sporadic-E clouds.
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7

Zhang, Tao. "Average value of the shape and direction factor in the equation of refractive index." Modern Physics Letters B 31, no. 29 (2017): 1750263. http://dx.doi.org/10.1142/s0217984917502633.

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The theoretical calculation of the refractive indices is of great significance for the developments of new optical materials. The calculation method of refractive index, which was deduced from the electron-cloud-conductor model, contains the shape and direction factor [Formula: see text]. [Formula: see text] affects the electromagnetic-induction energy absorbed by the electron clouds, thereby influencing the refractive indices. It is not yet known how to calculate [Formula: see text] value of non-spherical electron clouds. In this paper, [Formula: see text] value is derived by imaginatively dividing the electron cloud into numerous little volume elements and then regrouping them. This paper proves that [Formula: see text] when molecules’ spatial orientations distribute randomly. The calculations of the refractive indices of several substances validate this equation. This result will help to promote the application of the calculation method of refractive index.
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8

del Valle, Maria V. "Gamma-rays from reaccelerated cosmic rays in high-velocity clouds colliding with the Galactic disc." Monthly Notices of the Royal Astronomical Society 509, no. 3 (2021): 4448–56. http://dx.doi.org/10.1093/mnras/stab3206.

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ABSTRACT High-velocity clouds moving towards the disc will reach the Galactic plane and will inevitably collide with the disc. In these collisions, a system of two shocks is produced, one propagating through the disc and the other develops within the cloud. The shocks produced within the clouds in these interactions have velocities of hundreds of kilometres per second. When these shocks are radiative they may be inefficient in accelerating fresh particles; however, they can reaccelerate and compress Galactic cosmic rays from the background. In this work, we investigate the interactions of Galactic cosmic rays within a shocked high-velocity cloud, when the shock is induced by the collision with the disc. This study is focused in the case of radiative shocks. We aim to establish under which conditions these interactions lead to significant non-thermal emission, especially gamma-rays. We model the interaction of cosmic ray protons and electrons reaccelerated and further energized by compression in shocks within the clouds, under very general assumptions. We also consider secondary electron–positron pairs produced by the cosmic ray protons when colliding with the material of the cloud. We conclude that nearby clouds reaccelerating Galactic cosmic rays in local shocks can produce high-energy radiation that might be detectable with existing and future gamma-ray detectors. The emission produced by electrons and secondary pairs is important at radio wavelengths, and in some cases it may be relevant at hard X-rays. Concerning higher energies, the leptonic contribution to the spectral energy distribution is significant at soft gamma-rays.
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9

Stein, Benjamin P. "An “orbital glass” of electron clouds." Physics Today 58, no. 3 (2005): 9. http://dx.doi.org/10.1063/1.4796921.

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10

Zharkova, Valentina V., and Taras Siversky. "Formation of electron clouds during particle acceleration in a 3D current sheet." Proceedings of the International Astronomical Union 6, S274 (2010): 453–57. http://dx.doi.org/10.1017/s1743921311007472.

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AbstractAcceleration of protons and electrons in a reconnecting current sheet (RCS) is investigated with the test particle and particle-in-cell (PIC) approaches in the 3D magnetic configuration including the guiding field. PIC simulations confirm a spatial separation of electrons and protons towards the midplane and reveal that this separation occur as long as protons are getting accelerated. During this time electrons are ejected into their semispace of the current sheet moving away from the midplane to distances up to a factor of 103 – 104 of the RCS thickness and returning back to the RCS. This process of electron circulation around the current sheet midplane creates a cloud of high energy electrons around the current sheet which exists as long as protons are accelerated. Only after protons gain sufficient energy to break from the magnetic field of the RCS, they are ejected to the opposite semispace dragging accelerated electrons with them. These clouds can be the reason of hard X-ray emission in coronal sources observed by RHESSI.
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