Lunar Plasma Environment in Cases with Extreme Solar Wind Conditions: First Results from 3-D Hybrid Kinetic Modeling and Comparison with ARTEMIS Observations
| dc.contributor.author | Lipatov, Alexander | |
| dc.contributor.author | Sarantos, Menelaos | |
| dc.contributor.author | Cooper, John | |
| dc.contributor.author | Halekas, Jasper | |
| dc.date.accessioned | 2022-08-17T14:47:47Z | |
| dc.date.available | 2022-08-17T14:47:47Z | |
| dc.date.issued | 2020-12-04 | |
| dc.description | Fall 2020 AGU Meeting, Dec. 1 - 17, 2020 | en_US |
| dc.description.abstract | The study of lunar plasma environment's response to the extreme solar wind condition is the main subject of our investigation in this report. The computational model includes the self-consistent dynamics of the light (H_2+) and (He+), and heavy (Na^+}) pickup ions. The electrons are considered as a fluid. The lunar interior is considered as a weakly conducting body. The input parameters are taken from the ARTEMIS observations. The modeling demonstrates a formation of the various plasma structures near the Moon: (a) bow shock wave with split shock transition in case of extreme solar wind density and standard bulk velocity; (b) hyper-sonic/Alfvenic Mach cone in case of extreme solar wind bulk velocity and moderate solar wind density. The modeling shows a strong asymmetry in the solar wind ion VDF which connected with a plasma compression and ion reflection at the bow shock wave/Mach cone front. | en_US |
| dc.description.sponsorship | This work was supported by NASA Grant(80NSSC20K0146) “Hybrid Fluid-Kinetic Model of the Processes in the Moon’s Plasma Environment” from Solar System Workings Pro-gram (NNH18ZDA001N-C.3 SSW2018). Computational resources were provided by the NASA High-End Supercomputing Facilities (Pleiades/Electra/Aitken-Ames, Discover-Goddard, Project HEC SMD 20-02357875). | en_US |
| dc.description.uri | https://www.essoar.org/doi/10.1002/essoar.10505143.1 | en_US |
| dc.format.extent | 23 pages | en_US |
| dc.genre | presentations (communicative events) | en_US |
| dc.genre | conference papers and proceedings | en_US |
| dc.identifier | doi:10.13016/m2isky-6f3v | |
| dc.identifier.uri | https://doi.org/10.1002/essoar.10505143.1 | |
| dc.identifier.uri | http://hdl.handle.net/11603/25420 | |
| dc.language.iso | en_US | en_US |
| dc.relation.isAvailableAt | The University of Maryland, Baltimore County (UMBC) | |
| dc.relation.ispartof | UMBC Goddard Planetary Heliophysics Institute (GPHI) | |
| dc.relation.ispartof | UMBC Faculty Collection | |
| dc.rights | This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law. | en_US |
| dc.rights | Public Domain Mark 1.0 | * |
| dc.rights.uri | http://creativecommons.org/publicdomain/mark/1.0/ | * |
| dc.title | Lunar Plasma Environment in Cases with Extreme Solar Wind Conditions: First Results from 3-D Hybrid Kinetic Modeling and Comparison with ARTEMIS Observations | en_US |
| dc.type | Text | en_US |
| dcterms.creator | https://orcid.org/0000-0001-5026-8214 | en_US |