期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 462, 期 -, 页码 S9-S22出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw1736
关键词
plasmas; solar wind; comets: general
资金
- NASA [1345493, 1496541]
- Jet Propulsion Laboratory, California Institute of Technology
- German Ministerium fur Wirtschaft und Energie
- Deutsches Zentrum fur Luft- und Raumfahrt [50QP 1401]
- State of Bern
- European Space Agency PRODEX Programme
- Research Council of Norway [240000]
- CNRS
- UK Space Agency
- Swiss National Science Foundation
- CNES
- Observatoire de Paris
- Universite Paul Sabatier, Toulouse
- STFC [ST/K001051/1, ST/N000722/1, ST/K000977/1, ST/N000692/1, ST/H002383/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/N000722/1, ST/H002383/1, ST/K001051/1, ST/N000692/1] Funding Source: researchfish
- UK Space Agency [ST/P002250/1, ST/K001698/1] Funding Source: researchfish
One of the primary objectives of the Rosetta Plasma Consortium, a suite of five plasma instruments on-board the Rosetta spacecraft, is to observe the formation and evolution of plasma interaction regions at the comet 67P/Churyumov-Gerasimenko (67P/CG). Observations made between 2015 April and 2016 February show that solar wind-cometary plasma interaction boundaries and regions formed around 2015 mid-April and lasted through early 2016 January. At least two regions were observed, separated by an ion-neutral collisionopause boundary. The inner region was located on the nucleus side of the boundary and was characterized by low-energy water-group ions, reduced magnetic field pileup and enhanced electron densities. The outer region was located outside of the boundary and was characterized by reduced electron densities, water-group ions that are accelerated to energies above 100 eV and enhanced magnetic field pileup compared to the inner region. The boundary discussed here is outside of the diamagnetic cavity and shows characteristics similar to observations made on-board the Giotto spacecraft in the ion pileup region at 1P/Halley. We find that the boundary is likely to be related to ion-neutral collisions and that its location is influenced by variability in the neutral density and the solar wind dynamic pressure.
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