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Non-stationarity of the quasi-perpendicular bow shock: comparison between Cluster observations and simulations
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SYSNO ASEP 0360928 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Non-stationarity of the quasi-perpendicular bow shock: comparison between Cluster observations and simulations Author(s) Comisel, H. (RO)
Scholer, M. (DE)
Souček, Jan (UFA-U) RID, ORCID
Matsukiyo, S. (JP)Source Title Annales Geophysicae. - : Copernicus - ISSN 0992-7689
Roč. 29, č. 2 (2011), s. 263-274Number of pages 12 s. Language eng - English Country DE - Germany Keywords bow shock ; Cluster ; plasma waves ; shock waves Subject RIV BL - Plasma and Gas Discharge Physics CEZ AV0Z30420517 - UFA-U, BC-A (2005-2011) UT WOS 000287800700005 DOI 10.5194/angeo-29-263-2011 Annotation We performed full particle electromagnetic simulations of a quasi-perpendicular shock with parameters corresponding to the Earth's bow shock observed by Cluster on 24 January 2001. In run 1, modified two-stream instability (MTSI) is excited by the reflected solar wind ions. The waves due to the MTSI are on the whistler mode branch and have downstream directed phase velocities in the shock frame. The Poynting flux far upstream in the foot is also directed downstream. However, in the density and magnetic field compression region of the overshoot the waves are refracted and the Poynting flux in the shock frame points upstream. The MTSI is suppressed in the low mass ratio run 2, where significant reformation (“breathing”) is observed. It is suggested that the high frequency upstream waves are due to the MTSI and are not related to a nonlinear phase standing whistler. Different profiles observed by different Cluster spacecraft are due to the non-stationary behavior on a larger time scale. 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 2012 Electronic address http://www.ann-geophys.net/29/263/2011/angeo-29-263-2011.pdf
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