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Observations of EMIC waves in the distant cusp region and in the nearby magnetosheath
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SYSNO ASEP 0442502 Druh ASEP A - Abstrakt Zařazení RIV Záznam nebyl označen do RIV Zařazení RIV Není vybrán druh dokumentu Název Observations of EMIC waves in the distant cusp region and in the nearby magnetosheath Tvůrce(i) Grison, Benjamin (UFA-U) RID, ORCID
Escoubet, C. P. (NL)
Santolík, Ondřej (UFA-U) RID, ORCID
Lavraud, B. (FR)
Cornilleau-Wehrlin, N. (FR)Zdroj.dok. AGU Fall Meeting. - s. l : American Geophysical Union, 2014
SM13F-4220Akce AGU Fall Meeting Datum konání 15.12.2014-19.12.2014 Místo konání San Francisco Země US - Spojené státy americké Typ akce WRD Jazyk dok. eng - angličtina Země vyd. US - Spojené státy americké Institucionální podpora UFA-U - RVO:68378289 Anotace In the early years (2000-2004) of the mission, Cluster crossed the most distant part of the polar cusps. On 05/01/2002, Cluster enters the distant cusp region on the duskside of the southern hemisphere (inbound). The spacecraft are successively crossing the magnetopause between 19:50 UT (SC4) and 20:15 UT (SC3). The interplanetary conditions during the crossing were stable with a dominant negative By. The magnetometer (FGM) data indicates that the entry into the cusp takes place in a region where the magnetic field lines in the magnetosheath are anti-parallel with the field lines in the magnetosphere. Despite this clear picture, the global encounter is rather complex: one can notice partial magnetopause crossings, magnetic null points, and intense monochromatic waves on both sides of the magnetopause. We investigate electromagnetic ion cyclotron (EMIC) waves observed in the cusp and in the nearby magnetosheath, just before the magnetopause crossing by the spacecraft. Left-handed monochromatic waves observed in the cusp display different duration and frequency (below and above the local proton gyrofrequency) on each spacecraft. Both the Poynting flux of these emissions and the simultaneously recorded ion flows propagate in the same direction - toward the Earth. The wavenumber are determined in two ways: considering the Doppler shift and from direct measurements of the refractive index. We analyze these wave parameters and the local plasma conditions to explain the wave generation process on each side of the magnetopause. Pracoviště Ústav fyziky atmosféry Kontakt Kateřina Adamovičová, adamovicova@ufa.cas.cz, Tel.: 272 016 012 ; Kateřina Potužníková, kaca@ufa.cas.cz, Tel.: 272 016 019 Rok sběru 2015
Počet záznamů: 1