Influence of emissivity on behavior of metallic dust particles in plasmas

Tanaka, Yasunori; Smirnov, R.D.; Pigarov, A. Yu.; Rosenberg, M.

doi:10.1063/1.2946435

Cited by 11 publications

(4 citation statements)

References 41 publications

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“…In this processing, " was taken as equal to Q a [28,29], which we based on comparison to a least-squares fit over 0:55-0:9 m. These absolute emissivity levels increase toward unity near 3500 K, which is an expected trend. We also attempted to calculate emissivity based on " 2:31Q a =Q s 0:5 [30,31] because the scattering coefficient was so much larger than the absorption coefficient, however, the fits were even poorer because the assumption of a semi-infinite medium was invalid.…”

Section: Experimental Methodsmentioning

confidence: 98%

Emissivity of Aluminum-Oxide Particle Clouds: Application to Pyrometry of Explosive Fireballs

Lynch

Krier

Glumac

2010

Journal of Thermophysics and Heat Transfer

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Pyrometry measurements of clouds of high-temperature particles require an estimate of the spectral dependence of the particle emissivity. Common assumptions for this dependence range from " 2 to " constant. Depending upon the assumption used, there is uncertainty in the temperature of 100 s to a 1000 K in hightemperature clouds. Such errors are not apparent in goodness of fit of spectral data. A heterogeneous shock tube was used to measure the emissivity of aluminum oxide in an inert environment as a function of temperature (2000-3500 K), wavelength (0:55-0:95 m), and particle diameter (50 nm-10 m). In micro-sized alumina particles, the spectral dependence upon temperature transitions from decreasing with wavelength to increasing with wavelength with the dependence being roughly gray at about 3000 K. Because of local minima in the " vs curve, a power-law ( n ) dependence is insufficient to describe the emissivity. However, if such a dependence is assumed, n transitions from 1:4 to 0.5 as temperature increases from 2500-3500 K. Nano-sized alumina particles exhibit an even stronger spectral dependence. At 2678 K, n is approximately 1:2 but reaches as high as 2.1 at 3052 K. Considering optical depth issues, there is merit in gray emissivity approximations for high-temperature (3000-3300 K) particles typical of aluminum particle combustion. Nomenclature C = power-law coefficient c n = third-order law coefficients, n 0, 1, 2, 3 I = spectral intensity, W m 2 m 1 n = power-law exponent Q a = spectral absorption efficiency Q s = spectral scattering efficiency T = temperature, K t L = optical depth " = spectral emissivity = wavelength, m 0 = reference wavelength, 1 m Subscripts bb = Planck blackbody cal = calibration source exp = experimental p = particle

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Section: Experimental Methodsmentioning

confidence: 98%

Emissivity of Aluminum-Oxide Particle Clouds: Application to Pyrometry of Explosive Fireballs

Lynch

Krier

Glumac

2010

Journal of Thermophysics and Heat Transfer

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“…where σ SB is the Stefan-Boltzmann constant, ε d (R d , T d ) is the emissivity of the dust particle and T wall is the wall temperature. The computation of ε d from Mie theory is detailed in [62].…”

Section: Thermal Radiationmentioning

confidence: 99%

Dust–wall and dust–plasma interaction in the MIGRAINe code

Vignitchouk

Tolias

Ratynskaia

2014

Plasma Phys. Control. Fusion

106

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The physical models implemented in the recently developed dust dynamics code MIGRAINe are described. A major update of the treatment of secondary electron emission, stemming from models adapted to typical scrape-off layer temperatures, is reported. Sputtering and plasma species backscattering are introduced from fits of available experimental data and their relative importance to dust charging and heating is assessed in fusion-relevant scenarios. Moreover, the description of collisions between dust particles and plasma-facing components, based on the approximation of elastic-perfectly plastic adhesive spheres, has been upgraded to take into account the effects of particle size and temperature.

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“…The dust particle is heated by electron and ion fluxes and their recombination on the surface, as well as by emission processes, and cooled by radiation and evaporation. The equation describing the energy flux on the dust particle surface reads: 28) ( ) is the dust entalphy, other terms in the right hand side of Eq. ( 7) are described below.…”

Section: Dust Particle Heating and Mass Evolutionmentioning

confidence: 99%

Destruction of a dust particle in the white dwarf atmosphere

Kenzhebekova

Bastykova

Kodanova

et al. 2020

Jpn. J. Appl. Phys.

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Dusty white dwarfs are natural objects for studying the properties of cosmic dusty plasmas. We present the results of computation of the charge, radius, and temperature of a carbon dust particle in the atmosphere of dusty white dwarf G29-38, which is a typical example of a dusty white dwarf. The calculation results show that dust particles life-time in the atmospheres of dusty white dwarfs is of the order of microsecond. Therefore, dust particles cannot be sustained in a typical white dwarf atmosphere.

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Influence of emissivity on behavior of metallic dust particles in plasmas

Cited by 11 publications

References 41 publications

Emissivity of Aluminum-Oxide Particle Clouds: Application to Pyrometry of Explosive Fireballs

Emissivity of Aluminum-Oxide Particle Clouds: Application to Pyrometry of Explosive Fireballs

Dust–wall and dust–plasma interaction in the MIGRAINe code

Destruction of a dust particle in the white dwarf atmosphere

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