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Observations of a Solar Energetic Particle Event from Inside and Outside the Coma of Comet 67P
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT UK; The Centre for Planetary Science at UCL/Birkbeck, Gower Street, London, WC1E 6BT UK.ORCID iD: 0000-0002-2861-7999
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT UK; The Centre for Planetary Science at UCL/Birkbeck, Gower Street, London, WC1E 6BT UK.ORCID iD: 0000-0002-5859-1136
Department of Physics and Astronomy, Turku Collegium for Science, Medicine and Technology, University of Turku, Turku, Finland.ORCID iD: 0000-0003-3903-4649
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT UK; The Centre for Planetary Science at UCL/Birkbeck, Gower Street, London, WC1E 6BT UK.ORCID iD: 0000-0002-6185-3125
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2022 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 127, no 12Article in journal (Refereed) Published
Abstract [en]

We analyze observations of an SEP event at Rosetta’s target comet 67P/Churyumov-Gerasimenko during March 6th-10th 2015. The comet was 2.15AU from the Sun, with the Rosetta spacecraft approximately 70km from the nucleus placing it deep inside the comet’s coma and allowing us to study its response. The Eastern flank of an ICME also encountered Rosetta on March 6th and 7th. Rosetta’s RPC data indicate increases in ionization rates, and cometary water group pickup ions exceeding 1keV. Increased charge exchange reactions between solar wind ions and cometary neutrals also indicate increased upstream neutral populations consistent with enhanced SEP induced surface activity. In addition, the most intense parts of the event coincide with observations interpreted as an infant cometary bow shock, indicating that the SEPs may have enhanced the formation and/or intensified the observations. These solar transient events may also have pushed the cometopause closer to the nucleus.We track and discuss characteristics of the SEP event using remote observations by SOHO, WIND and GOES at the Sun, in-situ measurements at STEREO A, Mars and Rosetta, and ENLIL modeling. Based on its relatively prolonged duration, gradual and anisotropic nature and broad angular spread in the heliosphere, we determine the main particle acceleration source to be a distant ICME which emerged from the Sun on March 6th 2015 and was detected locally in the Martian ionosphere but was never encountered by 67P directly. The ICME’s shock produced SEPs for several days which traveled to the in-situ observation sites via magnetic field line connections.

Place, publisher, year, edition, pages
John Wiley & Sons, 2022. Vol. 127, no 12
National Category
Astronomy, Astrophysics and Cosmology
Research subject
Atmospheric science
Identifiers
URN: urn:nbn:se:ltu:diva-94256DOI: 10.1029/2022ja030398ISI: 000924527100001PubMedID: 37032655Scopus ID: 2-s2.0-85146127974OAI: oai:DiVA.org:ltu-94256DiVA, id: diva2:1713263
Note

Godkänd;2022;Nivå 0;2022-12-02 (sofila);

Funder: STFC consolidated Grants (grant nos. ST/N000722/1, ST/S000240/1, ST/W001004/1 and ST/W00089X/1); University of Turku, Finland;  Austrian Science Fund (FWF) (grant no. P32035-N36); UK-STFC Ernest Rutherford Fellowship (grant no. ST/V004115/1); NASA O2R Grant (no. 80NSSC20K0285); Academy of Finland (grant no. 322544); CNES; ANR (grant no. ANR-15-CE31-0009-01); ESA

Available from: 2022-11-24 Created: 2022-11-24 Last updated: 2024-11-20Bibliographically approved

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Nilsson, Hans

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Wellbrock, A.Jones, G. H.Dresing, N.Coates, A. J.Wedlund, C. SimonNilsson, HansPalmerio, E.Turc, L.Henri, P.Mandt, K.
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