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Vertical structure of the near-surface expanding ionosphere of comet 67P probed by Rosetta
Imperial Coll London, Dept Phys, Prince Consort Rd, London SW7 2AZ, England.
Univ Orleans, CNRS, LPC2E, F-45100 Orleans, France.
Univ Orleans, CNRS, LPC2E, F-45100 Orleans, France.
Imperial Coll London, Dept Phys, Prince Consort Rd, London SW7 2AZ, England.
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2017 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 469, p. S118-S129Article in journal (Refereed) Published
Abstract [en]

The plasma environment has been measured for the first time near the surface of a comet. This unique data set has been acquired at 67P/Churyumov-Gerasimenko during ESA/Rosetta spacecraft's final descent on 2016 September 30. The heliocentric distance was 3.8 au and the comet was weakly outgassing. Electron density was continuously measured with Rosetta Plasma Consortium (RPC)-Mutual Impedance Probe (MIP) and RPC-LAngmuir Probe (LAP) during the descent from a cometocentric distance of 20 km down to the surface. Data set from both instruments have been cross-calibrated for redundancy and accuracy. To analyse this data set, we have developed a model driven by Rosetta Orbiter Spectrometer for Ion and Neutral Analysis-COmetary Pressure Sensor total neutral density. The two ionization sources considered are solar extreme ultraviolet radiation and energetic electrons. The latter are estimated from the RPC-Ion and Electron Sensor (IES) and corrected for the spacecraft potential probed by RPC-LAP. We have compared the results of the model to the electron densities measured by RPC-MIP and RPC-LAP at the location of the spacecraft. We find good agreement between observed and modelled electron densities. The energetic electrons have access to the surface of the nucleus and contribute as the main ionization source. As predicted, the measurements exhibit a peak in the ionospheric density close to the surface. The location and magnitude of the peak are estimated analytically. The measured ionospheric densities cannot be explained with a constant outflow velocity model. The use of a neutral model with an expanding outflow is critical to explain the plasma observations.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2017. Vol. 469, p. S118-S129
Keywords [en]
plasmas, methods: data analysis, Sun: UV radiation, comets: individual: 67P
National Category
Astronomy, Astrophysics and Cosmology Fusion, Plasma and Space Physics
Identifiers
URN: urn:nbn:se:uu:diva-376693DOI: 10.1093/mnras/stx1459ISI: 000443940500012OAI: oai:DiVA.org:uu-376693DiVA, id: diva2:1288504
Conference
International Conference on Cometary Science - Comets - A New Vision after Rosetta and Philae, NOV 14-18, 2016, Toulouse, FRANCE
Available from: 2019-02-13 Created: 2019-02-13 Last updated: 2019-02-13Bibliographically approved

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Odelstad, EliasEriksson, Anders I.Vigren, Erik

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Swedish Institute of Space Physics, Uppsala Division
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Monthly notices of the Royal Astronomical Society
Astronomy, Astrophysics and CosmologyFusion, Plasma and Space Physics

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