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- Hans Nilsson
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Gabriella Stenberg Wieser
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Etienne Behar
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Cyril Simon Wedlund
- Aalto University, School of Electrical Engineering, Department of Radio Science and Engineering, Post Office Box 13000, FI-00076 Aalto, Finland.
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- Herbert Gunell
- Belgian Institute for Space Aeronomy, Avenue Circulaire 3, 1180 Brussels, Belgium.
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- Masatoshi Yamauchi
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Rickard Lundin
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Stas Barabash
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Martin Wieser
- Swedish Institute of Space Physics, Post Office Box 812, 981 28 Kiruna, Sweden.
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- Chris Carr
- Imperial College London, Exhibition Road, London SW7 2AZ, UK.
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- Emanuele Cupido
- Imperial College London, Exhibition Road, London SW7 2AZ, UK.
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- James L. Burch
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA.
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- Andrei Fedorov
- Institut de Recherche en Astrophysique et Planétologie, Toulouse, France.
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- Jean-André Sauvaud
- Institut de Recherche en Astrophysique et Planétologie, Toulouse, France.
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- Hannu Koskinen
- Department of Physics, University of Helsinki, Post Office Box 64, FI-00014 Helsinki, Finland.
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- Esa Kallio
- Aalto University, School of Electrical Engineering, Department of Radio Science and Engineering, Post Office Box 13000, FI-00076 Aalto, Finland.
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- Jean-Pierre Lebreton
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E), UMR 7328 CNRS–Université d’Orléans, France.
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- Anders Eriksson
- Swedish Institute of Space Physics, Ångström Laboratory, Lägerhyddsvägen 1, Uppsala, Sweden.
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- Niklas Edberg
- Swedish Institute of Space Physics, Ångström Laboratory, Lägerhyddsvägen 1, Uppsala, Sweden.
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- Raymond Goldstein
- Belgian Institute for Space Aeronomy, Avenue Circulaire 3, 1180 Brussels, Belgium.
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- Pierre Henri
- Laboratoire de Physique et Chimie de l’Environnement et de l’Espace (LPC2E), UMR 7328 CNRS–Université d’Orléans, France.
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- Christoph Koenders
- Technicsche Universität–Braunschweig, Institute for Geophysics and Extraterrestrial Physics, Mendelssohnstraße 3, D-38106 Braunschweig, Germany.
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- Prachet Mokashi
- Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, USA.
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- Zoltan Nemeth
- Wigner Research Centre for Physics, 1121 Konkoly Thege Street 29-33, Budapest, Hungary.
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- Ingo Richter
- Technicsche Universität–Braunschweig, Institute for Geophysics and Extraterrestrial Physics, Mendelssohnstraße 3, D-38106 Braunschweig, Germany.
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- Karoly Szego
- Wigner Research Centre for Physics, 1121 Konkoly Thege Street 29-33, Budapest, Hungary.
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- Martin Volwerk
- Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, 8042 Graz, Austria.
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- Claire Vallat
- Rosetta Science Ground Segment, Science and Robotic Exploration (SRE-OOR), Office A006, European Space Astronomy Centre, Post Office Box 78, 28691 Villanueva de la Cañada, Madrid, Spain.
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- Martin Rubin
- Physikalisches Institut, University of Bern, Sidlerstraße 5, CH-3012 Bern, Switzerland.
書誌事項
- 公開日
- 2015-01-23
- 権利情報
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- http://www.sciencemag.org/about/science-licenses-journal-article-reuse
- DOI
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- 10.1126/science.aaa0571
- 公開者
- American Association for the Advancement of Science (AAAS)
この論文をさがす
説明
<jats:p>The Rosetta mission shall accompany comet 67P/Churyumov-Gerasimenko from a heliocentric distance of >3.6 astronomical units through perihelion passage at 1.25 astronomical units, spanning low and maximum activity levels. Initially, the solar wind permeates the thin comet atmosphere formed from sublimation, until the size and plasma pressure of the ionized atmosphere define its boundaries: A magnetosphere is born. Using the Rosetta Plasma Consortium ion composition analyzer, we trace the evolution from the first detection of water ions to when the atmosphere begins repelling the solar wind (~3.3 astronomical units), and we report the spatial structure of this early interaction. The near-comet water population comprises accelerated ions (<800 electron volts), produced upstream of Rosetta, and lower energy locally produced ions; we estimate the fluxes of both ion species and energetic neutral atoms.</jats:p>
収録刊行物
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- Science
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Science 347 (6220), aaa0571-, 2015-01-23
American Association for the Advancement of Science (AAAS)
