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Rosetta and Mars Express observations of the influence of high solar wind pressure on the Martian plasma environment
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.
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2009 (English)In: Annales Geophysicae, ISSN 0992-7689, E-ISSN 1432-0576, Vol. 27, no 12, 4533-4545 p.Article in journal (Refereed) Published
Abstract [en]

We report on new simultaneous in-situ observations at Mars from Rosetta and Mars Express (MEX) on how the Martian plasma environment is affected by high pressure solar wind. A significant sharp increase in solar wind density, magnetic field strength and turbulence followed by a gradual increase in solar wind velocity is observed during similar to 24 h in the combined data set from both spacecraft after Rosetta's closest approach to Mars on 25 February 2007. The bow shock and magnetic pileup boundary are coincidently observed by MEX to become asymmetric in their shapes. The fortunate orbit of MEX at this time allows a study of the inbound boundary crossings on one side of the planet and the outbound crossings on almost the opposite side, both very close to the terminator plane. The solar wind and interplanetary magnetic field (IMF) downstream of Mars are monitored through simultaneous measurements provided by Rosetta. Possible explanations for the asymmetries are discussed, such as crustal magnetic fields and IMF direction. In the same interval, during the high solar wind pressure pulse, MEX observations show an increased amount of escaping planetary ions from the polar region of Mars. We link the high pressure solar wind with the observed simultaneous ion outflow and discuss how the pressure pulse could also be associated with the observed boundary shape asymmetry.

Place, publisher, year, edition, pages
2009. Vol. 27, no 12, 4533-4545 p.
Keyword [en]
Interplanetary physics, Planetary bow shocks, Magnetospheric physics, Magnetosheath, Solar wind interactions with unmagnetized bodies
National Category
Physical Sciences
URN: urn:nbn:se:uu:diva-148212DOI: 10.5194/angeo-27-4533-2009ISI: 000273060300014OAI: oai:DiVA.org:uu-148212DiVA: diva2:401640
Available from: 2011-03-03 Created: 2011-03-03 Last updated: 2011-03-03Bibliographically approved

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