Exosphere generation of the Moon investigated through a high-energy neutral detector

Milillo, A.; Mangano, V.; Mura, A.; Orsini, S.; Angelis, E. De; Lellis, A. M. Di; Massetti, S.; Plainaki, C.; Rispoli, Rosanna; Selci, S.; Vertolli, N.

doi:10.1007/s10686-010-9196-z

Cited by 3 publications

(1 citation statement)

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“…Sputter yields and elemental abundances consistent with Wurz et al [2007] were assumed. At 50 km where a possible orbiter could be located, all the IS species (mainly O and Si) have densities of the order of 4 cm −3 in agreement with the estimation of Milillo et al [2011]. This flux might increase following the exposure of the lunar surface to Earth's plasma sheet ions, which impart approximately three times higher energy than SW ions.…”

Section: A2 the Moonsupporting

confidence: 81%

Observing planets and small bodies in sputtered high-energy atom fluxes

et al. 2011

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[1] The evolution of the surfaces of bodies unprotected by either strong magnetic fields or thick atmospheres in the solar system is caused by various processes, induced by photons, energetic ions, and micrometeoroids. Among these processes, the continuous bombardment of the solar wind or energetic magnetospheric ions onto the bodies may significantly affect their surfaces, with implications for their evolution. Ion precipitation produces neutral atom releases into the exosphere through ion sputtering, with velocity distribution extending well above the particle escape limits. We refer to this component of the surface ejecta as sputtered high-energy atoms (SHEA). The use of ion sputtering emission for studying the interaction of exposed bodies (EB) with ion environments is described here. Remote sensing in SHEA in the vicinity of EB can provide mapping of the bodies exposed to ion sputtering action with temporal and mass resolution. This paper speculates on the possibility of performing remote sensing of exposed bodies using SHEA and suggests the need for quantitative results from laboratory simulations and molecular physic modeling in order to understand SHEA data from planetary missions. In Appendix A, referenced computer simulations using existing sputtering data are reviewed.

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Section: A2 the Moonsupporting

confidence: 81%

Observing planets and small bodies in sputtered high-energy atom fluxes

et al. 2011

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Kinetic modeling of sodium in the lunar exosphere

Tenishev

Rubin

Tucker

et al. 2013

Icarus

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Modeling exospheres: analytical and numerical methods with application examples

Tenishev,

Shou,

Lee

et al. 2024

Front. Astron. Space Sci.

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Exospheres, the tenuous gas environments surrounding planets, planetary satellites, and cometary comae, play a significant role in mediating the interactions of these astronomical bodies with their surrounding space environments. This paper presents a comprehensive review of both analytical and numerical methods employed in modeling exospheres. The paper explores analytical models, including the Chamberlain and Haser models, which have significantly contributed to our understanding of exospheres of planets, planetary satellites, and cometary comae. Despite their simplicity, these models provide baselines for more complex simulations. Numerical methods, particularly the Direct Simulation Monte Carlo (DSMC) method, have proven to be highly effective in capturing the detailed dynamics of exospheres under non-equilibrium conditions. The DSMC method’s capacity to incorporate a wide range of physical processes, such as particle collisions, chemical reactions, and surface interactions, makes it an indispensable tool in planetary science. The Adaptive Mesh Particle Simulator (AMPS), which employs the DSMC method, has demonstrated its versatility and effectiveness in simulating gases in planetary and satellite exospheres and dusty gas cometary comae. It provides a detailed characterization of the physical processes that govern these environments. Additionally, the multi-fluid model BATSRUS has been effective in modeling neutral gases in cometary comae, as discussed in the paper. The paper presents methodologies of exosphere modeling and illustrates them with specific examples, including the modeling of the Enceladus plume, the sodium exosphere of the Moon, the coma of comet 67P/Churyumov-Gerasimenko, and the hot oxygen corona of Mars and Venus.

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Exosphere generation of the Moon investigated through a high-energy neutral detector

Cited by 3 publications

References 42 publications

Observing planets and small bodies in sputtered high-energy atom fluxes

Observing planets and small bodies in sputtered high-energy atom fluxes

Kinetic modeling of sodium in the lunar exosphere

Modeling exospheres: analytical and numerical methods with application examples

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