A database on electron‐solid interactions

Joy, David C.

doi:10.1002/sca.4950170501

Cited by 239 publications

(211 citation statements)

References 10 publications

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“…To estimate the energy E e tr obtained from an electron, one needs to calculate the Mott cross section [67], which is a laborious task. It was proposed in [35] to use the experimental approximation from [68], obtained for graphite, for this cross section. We used the algorithm of [35] to compute E e tr , which is taken to be the difference between the initial energy of the electron E e 0 and its energy after it has passed through a PAH, E e 1 , which is found taking into account the traversed distance.…”

Section: Interactions With Gasmentioning

confidence: 99%

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Murga¹,

Khoperskov²,

Wiebe³

2016

Astron. Rep.

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A model of key processes influencing the evolution of a hydrocarbon grain of an arbitrary size under astrophysical conditions corresponding to ionized hydrogen regions (HII regions) and supernova remnants is presented. The considered processes include aromatization and photodestruction, sputtering by electrons and ions, and shattering due to collisions between grains. The model can be used to simulate the grain size distribution and the aromatization degree during the evolution of HII regions and supernova remnants for a specified radiation field, relative velocity of gas and dust, etc. The contribution of various processes to the evolution of hydrocarbon dust grains for parameters typical for the interstellar medium of our Galaxy is pre-

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Section: Interactions With Gasmentioning

confidence: 99%

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Murga¹,

Khoperskov²,

Wiebe³

2016

Astron. Rep.

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“…One of the candidates was the secondary electron emission due to electrons hitting the antenna box walls. We have implemented the secondary electron emission into our model using the yield dependency on the incoming energy from [8]. The secondary electron yield (SEY) depends strongly on the surface properties (roughness, cleanness, etc.)…”

Section: Plasma Initiation At F = 42 Mhzmentioning

confidence: 99%

Discharge initiation by ICRF antenna in IShTAR

Tripský

Wauters²,

D’Incà

et al. 2017

EPJ Web Conf.

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Abstract. IShTAR is a linear magnetized plasma test facility dedicated to the investigation of RF wave/plasma interaction. The IShTAR ICRF system consists of a single strap RF antenna. When using the antenna for plasma production without an external plasma source, it is shown that the plasma is either produced in front of the antenna strap or inside the antenna box depending on the antenna parameters. Here, we present experimental and numerical investigation of the plasma initiation parametric dependencies. Detailed pressure and RF power scans were performed in helium at f = 5.22 MHz and f = 42.06 MHz. The experiment shows the parameter ranges for which the plasma is produced in front of the strap, or inside the antenna box. These ranges are validated by simulations with the RFdinity model, and by theoretical predictions.

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“…They derive the electron energy loss (for E = 10 eV−2 keV) in carbon from measurements of dE/dx for solid carbon (Joy 1995). The data points are well fit by the following function:…”

Section: Electron Collisional Heatingmentioning

confidence: 99%

Dust heating

Bocchio

Jones

Verstraete

et al. 2013

A&A

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Aims. We investigate and quantify the effects of the electron collisional heating of dust in a hot gas and compare this with photon heating by the interstellar radiation field. Methods. We compare the rate of energy absorption by dust due to electron collisional and photon heating as a function of the physical conditions of the gas and the ambient radiation field. We calculate the resulting dust spectral energy distributions (SEDs) for different environments.Results. We find that electron collisions and grain charging effects in a hot gas (10 6 −10 7 K) rapidly destroy small carbonaceous particles and result in a minimum particle size of the order of a few nm. The charging due to the emission of secondary electrons is important and leads to high electric potentials, which quickly destroy the small grains by field ion emission. In the case of weak interstellar radiation fields (G 0 ∼ 0.1), electron collisional heating can be the dominant heating process and therefore makes an important contribution to the dust thermal emission. Conclusions. Collisions of electrons with dust grains, in a hot gas, lead to important changes in the dust SED, as a result of their high energy input. We find that grain charge effects and accompanying erosion need to be taken into account in the calculation of the dust SED. The power absorbed by the dust as a result of electron collisions in a hot tenuous gas can be larger than that due to photon absorption in the intergalactic medium close to a galaxy where the radiation field is weak (G 0 < ∼ 0.1).

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A database on electron‐solid interactions

Cited by 239 publications

References 10 publications

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Discharge initiation by ICRF antenna in IShTAR

Dust heating

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