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Carbon dioxide photoelectron energy peaks at Mars |
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| Authors: | RA Frahm JD Winningham JR Scherrer AJ Coates DO Kataria S Barabash H Andersson A Grigoriev T Säles W Schmidt JU Kozyra EC Roelof S Livi KC Hsieh M Grande J-A Sauvaud J-J Thocaven S Orsini M Maggi P Bochsler J Woch K Asamura |
| Institution: | a Southwest Research Institute, PO Drawer 28510, San Antonio, TX 78228-0510, USA b Mullard Space Science Laboratory, University College London, Surrey RH5 6NT, UK c Swedish Institute of Space Physics, Box 812, S-98 128 Kiruna, Sweden d Finnish Meteorological Institute, Box 503, FIN-00101 Helsinki, Finland e Department of Physical Sciences, University of Helsinki, P.O. Box 64, FIN-00014 Helsinki, Finland f Space Physics Research Laboratory, University of Michigan, Ann Arbor, MI 48109-2143, USA g Space Science Laboratory, University of California in Berkeley, Berkeley, CA 94720-7450, USA h Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723-6099, USA i University of Arizona, Tucson, AZ 85721, USA j Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK k Centre d'Etude Spatiale des Rayonnements, BP-4346, F-31028 Toulouse, France l Space Technology Ireland, National University of Ireland, Maynooth, Co. Kildare, Ireland m Istituto di Fisica dello Spazio Interplanetari, I-00133 Rome, Italy n Physikalisches Institut, University of Bern, CH-3012 Bern, Switzerland o Max-Planck-Institut für Aeronomie, D-37191 Katlenburg-Lindau, Germany p Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamichara, Japan q Technical University of Braunschweig, Hans-Sommer-Strasse 66, D-38106 Braunschweig, Germany |
| Abstract: | The ELectron Spectrometer (ELS) from the Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) flown on the Mars Express spacecraft has an 8% energy resolution, combined with the capability to oversample the martian electron distribution. This makes possible the resolution and identification of electrons generated as a result of the He 304 Å ionization of CO2 at the martian exobase on the dayside of the planet. Ionospheric photoelectrons were observed during almost every pass into the ionosphere and CO2 photoelectron peaks were identified near the terminator. Atmospherically generated CO2 photoelectrons are also observed at 10,000 km altitude in the martian tail near the inner magnetospheric boundary. Observations over a wide range of spacecraft orbits showed a consistent presence of photoelectrons at locations along the inner magnetospheric boundary and in the ionosphere, from an altitude of 250 to 10,000 km. |
| Keywords: | Mars Ionospheres Atmospheres Magnetospheres |
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