Chemical interactions of solar wind with cometary nuclei and comae |
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| Institution: | 1. Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany;2. Institut für Theoretische Physik, Technische Universität Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany;3. DLR-Institut für Planetenforschung, Rutherfordstr. 2, 12489 Berlin, Germany;1. Southwest Research Institute, 6220 Culebra Road, San Antonio, TX, 78238, USA;2. Swedish Institute of Space Physics, Uppsala, Sweden;3. Department of Physics and Astronomy, University of Kansas, Lawrence, KS, USA;4. Department of Physics, Imperial College London, Prince Consort Road, London, UK;5. Wigner Research Centre for Physics, Budapest, Hungary;6. Institut für Geophysik und Extraterrestrische Physik, TU Braunschweig, Braunschweig, Germany;7. Physikalisches Institut, University of Bern, Bern, Switzerland;1. Mullard Space Science Laboratory, University College London, Dorking, UK;2. Centre for Planetary Sciences at UCL/Birkbeck, University College London, London, UK;3. Department of Physics and Astronomy, University of Iowa, Iowa City, IA, USA;4. Max Planck Institute for Solar System Research, Göttingen, Germany;1. Belgian Institute for Space Aeronomy, Avenue Circulaire 3, Brussels, Belgium;3. Physics Department, Umeå University, Umeå, Sweden;4. Aalto University, School of Electrical Engineering, Department of Radio Science and Engineering, Espoo, Finland;5. Swedish Institute of Space Physics, Kiruna, Sweden |
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| Abstract: | Solar wind particles, especially H, C, N, O, S, and P-ions, may undergo specific chemical reactions with gaseous or solid matter of comets when in the energy region of a few 10 to some eV. Each component of the solar wind, even if not chemically reactive itself, creates a multiplicity of energetic secondary particles by knock-on processes with the cometary matter. These are responsible for the majority of the so called “hot” chemical processes. Endothermic reactions with high activation energy and atom molecule interactions are possible and may add to the classical exothermic ion-molecule or radical reactions. Other sources of hot atoms or ions in comets are: cosmic rays, acceleration or pick-up processes and turbulences in comae and gas or dust tails, and photon absorption induced dissociation. The products of hot chemical reactions, short period comets experience on their orbits, add to those formed in the individual component ice or dust grains by strong fluxes of energetic particles in times prior to the accretion to a comet. |
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