Dusty plasma at the surface of the moon

Popel, S. I.; Kopnin, S. I.; Голуб, А. П.; Dolnikov, Gennady; Захаров, А. В.; Zelenyǐ, L. M.; Izvekova, Yu. N.

doi:10.1134/s0038094613060063

Cited by 96 publications

(16 citation statements)

References 24 publications

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“…In a recent work, Popel and coworkers 23 have analyzed the size and elevation distribution of the charged dust particles on the lunar surface. However, the analysis is based on an intuitive formalism considering half Maxwellian distribution of electrons and uses an inappropriate expression for the photoemission current from the dust particle, for determining the dust particle charge.…”

Section: Resultsmentioning

confidence: 99%

“…(20)) with appropriate physical parameters viz. radiation/solar wind plasma flux; the specific parameters has been taken from Popel et al 23 and mentioned in Sec. V C. For a given electric potential V 0 (or t 0 ) of the moon surface, Eq.…”

Section: B Scheme Of Computationmentioning

confidence: 99%

“…Later analyses [17][18][19][20][21][22][23] are also based on the assumed arbitrary half Maxwellian distribution of emitted photoelectron energy and an inapplicable expression for electron accretion on the dust particles. In this paper, considering the balance of photoemission emission flux from the sunlit moon surface and solar wind flux, the steady state potential of the lunar surface has been estimated.…”

Section: Introductionmentioning

confidence: 99%

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Lunar photoelectron sheath and levitation of dust

Sodha

Mishra

2014

Physics of Plasmas

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The decision to launch Luna Glob and Luna Resus satellites, carrying instrumentation to investigate the structure of photoelectron sheath and levitation of dust particles in the sheath, adjacent to the surface of the moon has intensified interest in this exciting area. The present analysis incorporates the following novel features: (i) In contrast to intuitive half Maxwellian (M) distribution of velocities of the photoelectrons, emitted from the surface of the moon, which corresponds to an arbitrary temperature, a well-established half Fermi Dirac (F-D) distribution [R. H. Fowler, Phys. Rev. 38, 45 (1931)] has been used, (ii) the profiles for electric potential, electric field, and electron density have been derived (not a priori assumed), (iii) an expression for the rate of electron accretion on a positively charged dust particle, which takes account of the anisotropic flux of electrons has been derived and used in the analysis, and (iv) a derived (rather than intuitive) expression for the rate of photoelectron emission from a positively charged dust particle has been used for the first time in such analyses. The profiles of the electric potential, electric field, and electron density in the photoelectric sheath have been evaluated for typical lunar environment and used to obtain the profile of the radius of a dust particle for levitation. The dependence of the electric potential on the surface of the moon on the parameters of the solar wind and photo-efficiency of the material of moon's surface has also been discussed. It is seen that the results based on half F-D distribution are significantly different from those obtained on the basis of M-distribution. V C 2014 AIP Publishing LLC. [http://dx.

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Section: Resultsmentioning

confidence: 99%

Section: B Scheme Of Computationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Lunar photoelectron sheath and levitation of dust

Sodha

Mishra

2014

Physics of Plasmas

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“…A possibility of rising charged dust particles with the sizes of the order of 100 nm over the surface of the Moon in the entire range of the subsolar angles was demonstrated (Popel et al 2013a;Popel and Zelenyi 2013). This explains the lack of the so-called 'dead zone" [where dust particles, as it was previously believed (Stubbs et al 2006), do not rise off the surface] at lunar latitudes of about 80 • was demonstrated.…”

Section: Recent Lunar Dusty Plasma Studies In Russiamentioning

confidence: 89%

“…We emphasize that the considerations (Popel et al 2013a;Popel and Zelenyi 2013) showed the difference in the parameters of the dusty plasma system over the Moon for the work functions and the quantum yields inherent in typical and hydrogen-rich lunar regolith areas. This indicates the variability of the dusty plasma properties together with those of the lunar regolith depending on location.…”

Section: Recent Lunar Dusty Plasma Studies In Russiamentioning

confidence: 99%

Dusty plasmas over the Moon

Popel

Zelenyǐ

2014

J. Plasma Phys.

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Granular avalanches on the Moon: Mass‐wasting conditions, processes, and features

et al. 2017

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Seven lunar crater sites of granular avalanches are studied utilizing high‐resolution images (0.42–1.3 m/pixel) from the Lunar Reconnaissance Orbiter Camera; one, in Kepler crater, is examined in detail. All the sites are slopes of debris extensively aggraded by frictional freezing at their dynamic angle of repose, four in craters formed in basaltic mare and three in the anorthositic highlands. Diverse styles of mass wasting occur, and three types of dry‐debris flow deposit are recognized: (1) multiple channel‐and‐lobe type, with coarse‐grained levees and lobate terminations that impound finer debris, (2) single‐surge polylobate type, with subparallel arrays of lobes and fingers with segregated coarse‐grained margins, and (3) multiple‐ribbon type, with tracks reflecting reworked substrate, minor levees, and no coarse terminations. The latter type results from propagation of granular erosion‐deposition waves down slopes dominantly of fine regolith, and it is the first recognized natural example. Dimensions, architectures, and granular segregation styles of the two coarse‐grained deposit types are like those formed in natural and experimental avalanches on Earth, although the timescale of motion differs due to the reduced gravity. Influences of reduced gravity and fine‐grained regolith on dynamics of granular flow and deposition appear slight, but we distinguish, for the first time, extensive remobilization of coarse talus by inundation with finer debris. The (few) sites show no clear difference attributable to the contrasting mare basalt and highland megaregolith host rocks and their fragmentation. This lunar study offers a benchmarking of deposit types that can be attributed to formation without influence of liquid or gas.

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Dusty plasma at the surface of the moon

Cited by 96 publications

References 24 publications

Lunar photoelectron sheath and levitation of dust

Lunar photoelectron sheath and levitation of dust

Dusty plasmas over the Moon

Granular avalanches on the Moon: Mass‐wasting conditions, processes, and features

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