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Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection
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SYSNO ASEP 0501832 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Statistical analysis of mirror mode waves in sheath regions driven by interplanetary coronal mass ejection Author(s) Ala-Lahti, M.M. (FI)
Kilpua, E. K. J. (FI)
Dimmock, A.P. (FI)
Osmane, A. (FI)
Pulkkinen, T. (FI)
Souček, Jan (UFA-U) RID, ORCIDNumber of authors 6 Source Title Annales Geophysicae. - : Copernicus - ISSN 0992-7689
Roč. 36, č. 3 (2018), s. 793-808Number of pages 16 s. Language eng - English Country DE - Germany Keywords interplanetary physics ; plasma waves and turbulence ; solar wind plasma ; space plasma physics ; waves and instabilities Subject RIV BL - Plasma and Gas Discharge Physics OECD category Fluids and plasma physics (including surface physics) R&D Projects GA17-08772S GA ČR - Czech Science Foundation (CSF) Institutional support UFA-U - RVO:68378289 UT WOS 000433126600001 EID SCOPUS 85047483420 DOI 10.5194/angeo-36-793-2018 Annotation We present a comprehensive statistical analysis of mirror mode waves and the properties of their plasma surroundings in sheath regions driven by interplanetary coronal mass ejection (ICME). We have constructed a semi-automated method to identify mirror modes from the magnetic field data. We analyze 91 ICME sheath regions from January 1997 to April 2015 using data from the Wind spacecraft. The results imply that similarly to planetary magnetosheaths, mirror modes are also common structures in ICME sheaths. However, they occur almost exclusively as dip-like structures and in mirror stable plasma. We observe mirror modes throughout the sheath, from the bow shock to the ICME leading edge, but their amplitudes are largest closest to the shock. We also find that the shock strength (measured by Alfven Mach number) is the most important parameter in controlling the occurrence of mirror modes. Our findings suggest that in ICME sheaths the dominant source of free energy for mirror mode generation is the shock compression. We also suggest that mirror modes that are found deeper in the sheath are remnants from earlier times of the sheath evolution, generated also in the vicinity of the shock. Workplace Institute of Atmospheric Physics Contact Kateřina Adamovičová, adamovicova@ufa.cas.cz, Tel.: 272 016 012 ; Kateřina Potužníková, kaca@ufa.cas.cz, Tel.: 272 016 019 Year of Publishing 2019
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