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Solar wind plasma protrusion into the martian magnetosphere: ASPERA-3 observations |
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| Authors: | E Dubinin D Winningham J Woch S Barabash R Frahm AJ Coates J-A Sauvaud H Andersson A Grigoriev K Asamura KS Hsieh H Koskinen P Riihelä T Säles J Luhmann R Cerulli-Irelli M Maggi D Williams P Wurz C Dierker M Carter |
| Institution: | a MPI für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany b Southwest Research Institute, San Antonio, TX 7228-0510, USA c Swedish Institute of Space Physics, Box 812, S-98 128 Kiruna, Sweden d Centre d'Etude Spatiale des Rayonnements, BP-4346, F-31028 Toulouse, France e Mullard Space Science Laboratory, University College London, Surrey RH5 6NT, UK f Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamichara, Japan g University of Arizona, Tucson, AZ 85721, USA h Department of Physical Sciences, University of Helsinki, P.O. Box 64, 00014 Helsinki, Finland i Finnish Meteorological Institute, Box 503, FIN-00101 Helsinki, Finland j Space Physics Research Laboratory, University of Michigan, Ann Arbor, MI 48109-2143, USA k Space Science Laboratory, University of California in Berkeley, Berkeley, CA 94720-7450, USA l Space Technology Ireland, National University of Ireland, Maynooth, Co. Kildare, Ireland m Istituto di Fisica dello Spazio Interplanetari, I-00133 Rome, Italy n Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723-6099, USA o Physikalisches Institut, University of Bern, CH-3012 Bern, Switzerland p Technical University of Braunschweig, Hans-Sommer-Strasse 66, D-38106 Braunschweig, Germany q Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK |
| Abstract: | The ASPERA-3 experiment onboard the Mars Express spacecraft revealed, near the wake boundary of Mars, a spatially narrow, strip-like plasma structure composed of magnetosheath-like electrons and planetary ions. The peak electron energy often exceeds the peak energy at the bow shock that indicates a significant heating (acceleration) during the structure formation. It is shown that this structure is formed during efficient plasma penetration into the martian magnetosphere in the region near the terminator. The penetration of sheath electrons and their gradual heating (acceleration) is accompanied by a change of the ion composition from a solar wind plasma to a planetary plasma dominated by oxygen ions. A possible mechanism of plasma inflow to the magnetosphere is discussed. |
| Keywords: | Mars Magnetospheres |
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