Near-lunar proton velocity distribution explained by electrostatic acceleration

The observation of parallel ion velocity in the near-lunar wake approximately equal to external solar wind velocity can be explained within uncertainties by an analytic electrostatic expansion model. The one-dimensional model frequently used is inadequate because it does not account for the moon...

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Main Author: Hutchinson, Ian Horner
Other Authors: Massachusetts Institute of Technology. Department of Nuclear Science and Engineering
Format: Article
Language:en_US
Published: American Geophysical Union (AGU) 2015
Online Access:http://hdl.handle.net/1721.1/95829
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author Hutchinson, Ian Horner
author2 Massachusetts Institute of Technology. Department of Nuclear Science and Engineering
author_facet Massachusetts Institute of Technology. Department of Nuclear Science and Engineering
Hutchinson, Ian Horner
author_sort Hutchinson, Ian Horner
collection MIT
description The observation of parallel ion velocity in the near-lunar wake approximately equal to external solar wind velocity can be explained within uncertainties by an analytic electrostatic expansion model. The one-dimensional model frequently used is inadequate because it does not account for the moon's spherical shape. However, application of a more recent generalization to three dimensions of the solution along characteristics predicts higher velocities and is probably sufficient to account for the SARA observations on the Chandrayaan-1 spacecraft.
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spelling mit-1721.1/958292023-02-26T03:29:39Z Near-lunar proton velocity distribution explained by electrostatic acceleration Hutchinson, Ian Horner Massachusetts Institute of Technology. Department of Nuclear Science and Engineering Massachusetts Institute of Technology. Plasma Science and Fusion Center Hutchinson, Ian H. The observation of parallel ion velocity in the near-lunar wake approximately equal to external solar wind velocity can be explained within uncertainties by an analytic electrostatic expansion model. The one-dimensional model frequently used is inadequate because it does not account for the moon's spherical shape. However, application of a more recent generalization to three dimensions of the solution along characteristics predicts higher velocities and is probably sufficient to account for the SARA observations on the Chandrayaan-1 spacecraft. 2015-03-04T20:51:50Z 2015-03-04T20:51:50Z 2013-05 2013-03 Article http://purl.org/eprint/type/JournalArticle 21699380 2169-9402 http://hdl.handle.net/1721.1/95829 Hutchinson, I. H. “Near-Lunar Proton Velocity Distribution Explained by Electrostatic Acceleration.” Journal of Geophysical Research: Space Physics 118, no. 5 (May 2013): 1825–1827. en_US http://dx.doi.org/10.1002/jgra.50277 Journal of Geophysical Research: Space Physics Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf American Geophysical Union (AGU) arXiv
spellingShingle Hutchinson, Ian Horner
Near-lunar proton velocity distribution explained by electrostatic acceleration
title Near-lunar proton velocity distribution explained by electrostatic acceleration
title_full Near-lunar proton velocity distribution explained by electrostatic acceleration
title_fullStr Near-lunar proton velocity distribution explained by electrostatic acceleration
title_full_unstemmed Near-lunar proton velocity distribution explained by electrostatic acceleration
title_short Near-lunar proton velocity distribution explained by electrostatic acceleration
title_sort near lunar proton velocity distribution explained by electrostatic acceleration
url http://hdl.handle.net/1721.1/95829
work_keys_str_mv AT hutchinsonianhorner nearlunarprotonvelocitydistributionexplainedbyelectrostaticacceleration