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Monte-Carlo simulation of Callisto’s exosphere
Icarus, 2015We model Callisto's exosphere based on its ice as well as non-ice surface via the use of a Monte-Carlo exosphere model. For the ice component we implement two putative compositions that have been computed from two possible extreme formation scenarios of the satellite.
Vorburger, A. +4 more
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Detection of SO in Io's Exosphere
Science, 2000The Galileo orbiter's close pass by Io in 1995 produced evidence for extensive mass loading of the plasma torus through the ionization of SO 2 . On 11 October 1999, Galileo passed even closer to Io, this time across the upstream side relative to the flow of magnetospheric plasma that corotates with Jupiter.
C T, Russell, M G, Kivelson
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Lorentzian ion exosphere model
Journal of Geophysical Research: Space Physics, 1996Since observed velocity distributions of particles in the magnetosphere generally have a suprathermal tail instead of an exponential one, we propose to recalculate the density and temperature distributions in a nonrotating ion exosphere with a Lorentzian velocity distribution function (VDF) instead of a Maxwellian.
V. Pierrard, J. Lemaire
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Model of the polar ion-exosphere
Planetary and Space Science, 1970A model of a polar ion-exosphere in which the geomagnetic field lines are open is developed. The electrostatic field in this region has been calculated by taking into account two fundamental conditions: (1) quasi-neutrality has to be satisfied everywhere in the exosphere; (2) escape fluxes of electrons and ions have to be equal.
Lemaire, J., Scherer, M.
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The Exospheric Systems of Saturn's Rings
Icarus, 1995Abstract Because of collisional interaction with interplanetary meteoroids, the ring system of Saturn is supposedly a major source of neutral gas cloud in the inner saturnian system. We consider some new features brought about by the asymmetric impact geometry of the ring-meteoroid interaction.
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A model of rotating exospheres
Journal of Geophysical Research: Space Physics, 1993Using a truncated Boltzmann distribution, we analyze the neutral density profile of an isothermal planetary exosphere. In the absence of rotation, the classical result obtained by Chamberlain is recovered. When rotation exists, a latitude‐dependent limit appears and the total bound mass presents a logarithmic divergence.
M. Membrado, A. F. Pacheco, J. Sañudo
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2020
In this chapter, we turn away from giant impacts themselves to study a particular feature hosted by the most famous outcome of a giant impact, the Moon; specifically the lunar argon exosphere with its links to the Moon’s interior. This is just one example of a connection between the consequences of giant impacts and their role in planet formation to ...
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In this chapter, we turn away from giant impacts themselves to study a particular feature hosted by the most famous outcome of a giant impact, the Moon; specifically the lunar argon exosphere with its links to the Moon’s interior. This is just one example of a connection between the consequences of giant impacts and their role in planet formation to ...
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Exospheric escape: A parametrical study
Advances in Space Research, 2018Abstract The study of exospheres can help us understand the long-term loss of volatiles from planetary bodies due to interactions of planets, satellites, and small bodies with the interplanetary medium, solar radiation, and internal forces including diffusion and outgassing.
Rosemary M. Killen +2 more
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1966
The relative smallness of the mass of the Moon and the low velocity of escape from its gravitational field, together with the probable chemical composition of its globe as discussed in the preceding chapter, entail several further important consequences; and perhaps the most important one for an understanding of lunar surface features is the well-nigh ...
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The relative smallness of the mass of the Moon and the low velocity of escape from its gravitational field, together with the probable chemical composition of its globe as discussed in the preceding chapter, entail several further important consequences; and perhaps the most important one for an understanding of lunar surface features is the well-nigh ...
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The calcium exosphere of Mercury
Icarus, 2005Abstract A tenuous calcium atmosphere at Mercury, principally seen in the polar regions, was first observed in July, 1998, using the High Resolution Echelle Spectrograph (HIRES) at the W.M. Keck I telescope (Bida et al., Nature 404, 159, 2000). We report four years of observations of the calcium exosphere of Mercury, confirming the initial findings ...
R KILLEN, T BIDA, T MORGAN
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