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Evolution of the ion environment of comet 67P during the Rosetta mission as seen by RPC-ICA

Nilsson, Hans (författare)
Luleå tekniska universitet,Rymdteknik,Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden,Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden;Luleå Univ Technol, Dept Comp Sci Elect & Space Engn, SE-98128 Kiruna, Sweden
Stenberg Wieser, Gabriella (författare)
Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden,Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden
Behar, Etienne (författare)
Luleå tekniska universitet,Rymdteknik,Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden,Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden;Luleå Univ Technol, Dept Comp Sci Elect & Space Engn, SE-98128 Kiruna, Sweden
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Gunell, Herbert (författare)
Umeå universitet,Institutionen för fysik,Royal Belgian Institute for Space Aeronomy, Avenue Circulaire 3, B-1180 Brussels, Belgium; Department of Physics, Umeå University, SE-901 87 Umeå, Sweden,Royal Belgian Inst Space Aeron, Ave Circulaire 3, B-1180 Brussels, Belgium;Umeå Univ, Dept Phys, SE-90187 Umeå, Sweden
Wieser, Martin (författare)
Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden,Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden
Galand, Marina (författare)
Department of Physics, Imperial College London, Prince Consort Road, London SW7 2AZ, UK,Imperial Coll London, Dept Phys, Prince Consort Rd, London SW7 2AZ, England
Simon Wedlund, Cyril (författare)
Department of Physics, University of Oslo, PO Box 1048 Blindern, N-0316 Oslo, Norway,Univ Oslo, Dept Phys, POB 1048 Blindern, N-0316 Oslo, Norway
Alho, Markku (författare)
Department of Electronics and Nanoengineering, School of Electrical Engineering, Aalto University, PO Box 15500, FI-00076 Aalto, Finland,Aalto Univ, Sch Elect Engn, Dept Elect & Nanoengn, POB 15500, FI-00076 Aalto, Finland
Goetz, Charlotte (författare)
Institut für Geophysik und extraterrestrische Physik, Technische Universität Braunschweig, Mendelssohnstr 3, D-38106 Braunschweig, Germany,Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany
Yamauchi, Masatoshi (författare)
Swedish Institute of Space Physics, Box 812, SE-981 28 Kiruna, Sweden,Swedish Inst Space Phys, Box 812, SE-98128 Kiruna, Sweden
Henri, Pierre (författare)
LPC2E-CNRS, 3A avenue de la Recherche Scientifique, F-45071 Orléans, Cedex, 2, Orléans, France,CNRS, LPC2E, 3A Ave Rech Sci, F-45071 Orleans 2, France
Odelstad, Elias (författare)
Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen
Vigren, Erik (författare)
Uppsala universitet,Institutet för rymdfysik, Uppsalaavdelningen
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 (creator_code:org_t)
2017-06-21
2017
Engelska.
Ingår i: Monthly notices of the Royal Astronomical Society. - : Oxford University Press. - 0035-8711 .- 1365-2966. ; 469:Suppl_2, s. S252-S261
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  • Tidskriftsartikel (refereegranskat)
Abstract Ämnesord
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  • Rosetta has followed comet 67P from low activity at more than 3.6 au heliocentric distance to high activity at perihelion (1.24 au) and then out again. We provide a general overview of the evolution of the dynamic ion environment using data from the RPC-ICA ion spectrometer. We discuss where Rosetta was located within the evolving comet magnetosphere. For the initial observations, the solar wind permeated all of the coma. In 2015 mid-April, the solar wind started to disappear from the observation region, to re-appear again in 2015 December. Low-energy cometary ions were seen at first when Rosetta was about 100 km from the nucleus at 3.6 au, and soon after consistently throughout the mission except during the excursions to farther distances from the comet. The observed flux of low-energy ions was relatively constant due to Rosetta's orbit changing with comet activity. Accelerated cometary ions, moving mainly in the antisunward direction gradually became more common as comet activity increased. These accelerated cometary ions kept being observed also after the solar wind disappeared from the location of Rosetta, with somewhat higher fluxes further away from the nucleus. Around perihelion, when Rosetta was relatively deep within the comet magnetosphere, the fluxes of accelerated cometary ions decreased, as did their maximum energy. The disappearance of more energetic cometary ions at close distance during high activity is suggested to be due to a flow pattern where these ions flow around the obstacle of the denser coma or due to charge exchange losses.

Ämnesord

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

Nyckelord

plasmas
methods: data analysis
comets: individual: 67P
Atmosfärsvetenskap
Atmospheric Science

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