Photoemission and Secondary Electron Emission from Lunar Surface Material

Willis, R. F.; Anderegg, M.; Feuerbacher, B.; Fitton, B.

doi:10.1007/978-94-010-2647-5_25

Cited by 72 publications

(63 citation statements)

References 5 publications

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“…The dayside lunar surface also provides a source of low energy photoelectrons produced by solar photons and secondary electrons produced by both electron and ion impact, as well as reflected and backscattered primary electrons (Feuerbacher et al, 1972;Willis et al, 1973;Whipple, 1981;Horányi et al, 1998).…”

Section: Introductionmentioning

confidence: 99%

Solar wind electron interaction with the dayside lunar surface and crustal magnetic fields: Evidence for precursor effects

et al. 2012

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Electron distributions measured by Lunar Prospector above the dayside lunar surface in the solar wind often have an energy dependent loss cone, inconsistent with adiabatic magnetic reflection. Energy dependent reflection suggests the presence of downward parallel electric fields below the spacecraft, possibly indicating the presence of a standing electrostatic structure. Many electron distributions contain apparent low energy (<100 eV) upwardgoing conics (58% of the time) and beams (12% of the time), primarily in regions with non-zero crustal magnetic fields, implying the presence of parallel electric fields and/or wave-particle interactions below the spacecraft. Some, but not all, of the observed energy dependence comes from the energy gained during reflection from a moving obstacle; correctly characterizing electron reflection requires the use of the proper reference frame. Nonadiabatic reflection may also play a role, but cannot fully explain observations. In cases with upward-going beams, we observe partial isotropization of incoming solar wind electrons, possibly indicating streaming and/or whistler instabilities. The Moon may therefore influence solar wind plasma well upstream from its surface. Magnetic anomaly interactions and/or non-monotonic near surface potentials provide the most likely candidates to produce the observed precursor effects, which may help ensure quasi-neutrality upstream from the Moon.

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Section: Introductionmentioning

confidence: 99%

Solar wind electron interaction with the dayside lunar surface and crustal magnetic fields: Evidence for precursor effects

et al. 2012

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“…Halekas et al (2009) reported the first in situ measurements of secondary electron emission efficiency of a lunar regolith. They found that the secondary emission yield from this material is a factor of ≈3 lower than that measured under laboratory conditions (Willis et al 1973;Horányi et al 1998;Němeček et al 2011). The authors discussed the discrepancy between their observations and laboratory measurements and concluded that it might result from the roughness and irregular shape of the lunar regolith, which likely affect the escape of secondary electrons from the surface.…”

Section: Introductionmentioning

confidence: 87%

Secondary Emission From Non-Spherical Dust Grains With Rough Surfaces: Application to Lunar Dust

Richterová

Němeček

Beránek

et al. 2012

ApJ

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Electrons impinging on a target can release secondary electrons and/or they can be scattered out of the target. It is well established that the number of escaping electrons per primary electron depends on the target composition and dimensions, the energy, and incidence angle of the primary electrons, but there are suggestions that the target's shape and surface roughness also influence the secondary emission. We present a further modification of the model of secondary electron emission from dust grains which is applied to non-spherical grains and grains with defined surface roughness. It is shown that the non-spherical grains give rise to a larger secondary electron yield, whereas the surface roughness leads to a decrease in the yield. Moreover, these effects can be distinguished: the shape effect is prominent for high primary energies, whereas the surface roughness predominantly affects the yield at the low-energy range. The calculations use the Lunar Highlands Type NU-LHT-2M simulant as a grain material and the results are compared with previously published laboratory and in situ measurements.

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“…The lunar material current density at normal sunlight incidence angle is J p0 = 4.5 µA/m 2 at 1 AU for lunar dust [12]. The secondary emission from particle impact [12] is assumed to be low at the surface, but the secondary emission model of [13] is implemented for the emission induced by electron impact in the volume.…”

Section: B Lander Insertionmentioning

confidence: 99%

“…The secondary emission from particle impact [12] is assumed to be low at the surface, but the secondary emission model of [13] is implemented for the emission induced by electron impact in the volume. This model depends on the inverse of the energy required to excite a single secondary electron (K = 0.01 eV -1 ), the inverse of the absorption length for secondary electrons (α =10 8 m -1 ), and the Whiddington constant for the rate loss with distance (a = 10 14 V 2 .m -1 ).…”

Section: B Lander Insertionmentioning

confidence: 99%

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New SPIS Capabilities to Simulate Dust Electrostatic Charging, Transport, and Contamination of Lunar Probes

Hess

Sarrailh

Matéo‐Vélez

et al. 2015

IEEE Trans. Plasma Sci.

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Abstract-The Spacecraft Plasma interaction Software (SPIS) has been improved to allow for the simulation of lunar and asteroid dust emission, transport, deposition and interaction with a spacecraft on or close to the lunar surface. The physics of dust charging and of the forces that they are subject to has been carefully implemented in the code. It is both a tool to address the risks faced by lunar probes on the surface, and a tool to study the dust transport physics. We hereby present the details of the physics that has been implemented in the code, as well as the interface improvements that allow for a user friendly insertion of the lunar topology and of the lander in the simulation domain. A realistic case is presented that highlights the capabilities of the code as well as some general results about the interaction between a probe and a dusty environment.

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Photoemission and Secondary Electron Emission from Lunar Surface Material

Cited by 72 publications

References 5 publications

Solar wind electron interaction with the dayside lunar surface and crustal magnetic fields: Evidence for precursor effects

Solar wind electron interaction with the dayside lunar surface and crustal magnetic fields: Evidence for precursor effects

Secondary Emission From Non-Spherical Dust Grains With Rough Surfaces: Application to Lunar Dust

New SPIS Capabilities to Simulate Dust Electrostatic Charging, Transport, and Contamination of Lunar Probes

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