Physics
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsm23b..03s&link_type=abstract
American Geophysical Union, Spring Meeting 2007, abstract #SM23B-03
Physics
5421 Interactions With Particles And Fields, 6025 Interactions With Solar Wind Plasma And Fields, 6250 Moon (1221), 7855 Spacecraft Sheaths, Wakes, Charging
Scientific paper
The surface of the Moon is electrically charged by solar ultraviolet radiation incident on its dayside and the highly variable plasma environment that surrounds it. Lunar surface charging and the associated transport of charged dust could present hazards to future explorers, so developing a predictive capability for this environment will be a high priority. The main electric current sources come from the photoemission of electrons, plasma electrons, plasma ions, and the secondary emission of electrons. All four current sources can be very dynamic, which in turn results in a highly variable electrostatic potential and electric field at the lunar surface, both temporally and spatially. We present predictions for lunar surface potentials and electric fields for a variety of steady-state solar wind conditions. In addition, we also consider what happens when the Moon enters the hotter and more tenuous lobe and plasma sheet regions in the Earth's magnetotail. The main assumptions in deriving these predictions are that all the charged particle populations have a Maxwellian velocity distribution, and that as far as these populations are concerned the Moon's surface is an infinite plane. Since we focus mainly on the solar wind-lunar interaction, we initially neglect the effects of secondary electron emission, since this is often not a significant current source. The intention of this work is to develop a basic theoretical approach to making lunar surface charging predictions, which can be augmented by improvements in (1) our understanding of the current sources, (2) observational constraints, and (3) laboratory measurements. These initial predictions establish a "baseline" against which future theoretical and observational results may be compared, not just for the lunar case, but for all airless bodies such as Mercury and asteroids.
Burchill J. K.
Delory Gregory T.
Farrell William M.
Halekas Jasper S.
Pfaff Robert F.
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