. "457559" . "14"^^ . . "RIV/68378289:_____/07:00091880!RIV08-GA0-68378289" . . "Variations of the flank LLBL thickness as response to the solar wind dynamic pressure and IMF orientation"@en . "Low-latitude boundary layer; solar wind-magnetosphere interaction; reconnection"@en . "Variations of the flank LLBL thickness as response to the solar wind dynamic pressure and IMF orientation"@en . "P(GA205/05/0170), P(GA205/06/0875), Z(AV0Z30420517), Z(MSM0021620860)" . "[BD6024B6B4F2]" . "Several mechanisms have been discussed as candidates for a formation of the low-latitude boundary layer (LLBL) magnetic reconnection between the magnetospheric and magnetosheath magnetic fields, impulsive penetration of magnetosheath plasma, and viscous/diffusive mixing of plasma populations at the magnetopause. The observed fluctuations of plasma parameters inside the LLBL are attributed either to transient nature of the phenomena forming the layer or to sweeping of deformations of the magnetopause or an inner edge of the LLBL surface along the spacecraft. We are using the Interball-1/Magion-4 satellite pair separated by several thousands of kilometers in order to distinguish between spatial and temporal changes of the LLBL plasma population. Observations of LLBL crossings invoked by sudden changes of upstream conditions show that even during a strongly northward interplanetary magnetic field (IMF), the LLBL is relatively thin and follows the compression of the magnetopause induced by changes of the" . . "P\u0159ech, L." . "\u0160im\u016Fnek, Ji\u0159\u00ED" . . . . "6"^^ . "\u0160afr\u00E1nkov\u00E1, J." . . . . "Variations of the flank LLBL thickness as response to the solar wind dynamic pressure and IMF orientation" . "US - Spojen\u00E9 st\u00E1ty americk\u00E9" . "A07201/1;A07201/14" . "Kol\u00EDs\u00E1n\u00ED tlou\u0161\u0165ky LLBL v z\u00E1vislosti na dynamick\u00E9m tlaku slune\u010Dn\u00EDho v\u011Btru a na orientaci meziplanet\u00E1rn\u00EDho magnetick\u00E9ho pole"@cs . . . . "1"^^ . . "RIV/68378289:_____/07:00091880" . . "Variations of the flank LLBL thickness as response to the solar wind dynamic pressure and IMF orientation" . "Journal of Geophysical Research" . "Several mechanisms have been discussed as candidates for a formation of the low-latitude boundary layer (LLBL) magnetic reconnection between the magnetospheric and magnetosheath magnetic fields, impulsive penetration of magnetosheath plasma, and viscous/diffusive mixing of plasma populations at the magnetopause. The observed fluctuations of plasma parameters inside the LLBL are attributed either to transient nature of the phenomena forming the layer or to sweeping of deformations of the magnetopause or an inner edge of the LLBL surface along the spacecraft. We are using the Interball-1/Magion-4 satellite pair separated by several thousands of kilometers in order to distinguish between spatial and temporal changes of the LLBL plasma population. Observations of LLBL crossings invoked by sudden changes of upstream conditions show that even during a strongly northward interplanetary magnetic field (IMF), the LLBL is relatively thin and follows the compression of the magnetopause induced by changes of the"@en . "Sibeck, D." . . "112" . . "N\u011Bme\u010Dek, Z." . "A7" . . "Formov\u00E1n\u00ED \u010Deln\u00ED hrani\u010Dn\u00ED vrstvy (LLBL) je vysv\u011Btlov\u00E1no n\u011Bkolika mechanizmy, p\u0159epojen\u00ED magnetick\u00FDch silo\u010Dar mezi magnetosf\u00E9rou a magnetick\u00FDm polem v p\u0159echodov\u00E9 vrstv\u011B, spont\u00E1nn\u00EDm pronik\u00E1n\u00EDm plazmatu p\u0159echodov\u00E9 vrstvy a visk\u00F3zn\u00EDm/difusivn\u00EDm m\u00EDch\u00E1n\u00EDm populac\u00ED plazmatu na magnetopauze. Pozorovan\u00E9 fluktuace parametr\u016F plazmatu jsou vysv\u011Btlov\u00E1ny bu\u010F do\u010Dasnosti vlastn\u00EDho jevu formuj\u00EDc\u00EDho tuto vrstvu nebo deforma\u010Dn\u00EDm pohybem magnetopauzy nebo vnit\u0159n\u00EDho kraje LLBL v bl\u00EDzkosti dru\u017Eice. Vyu\u017Eili jsme dvojici dru\u017Eic Interball-1/Magion-4, kter\u00E9 byly vz\u00E1jemn\u011B vzd\u00E1leny n\u011Bkolik tis\u00EDc kilometr\u016F, k tomu, abychom rozli\u0161ili prostorov\u00E9 a \u010Dasov\u00E9 zm\u011Bny vlastnost\u00ED plazmatu v LLBL. Pozorov\u00E1n\u00ED p\u0159echod\u016F LLBL vyvolan\u00FDch n\u00E1hl\u00FDmi zm\u011Bnami vlastnost\u00ED slune\u010Dn\u00EDho v\u011Btru ukazuj\u00ED, \u017Ee i v obdob\u00ED, kdy je sm\u011Br meziplanet\u00E1rn\u00EDho magnetick\u00E9ho pole (IMF) v\u00FDrazn\u011B severn\u00ED, LLBL je pom\u011Brn\u011B tenk\u00E1 a sleduje stla\u010Dov\u00E1n\u00ED magnetopauzy vyvolan\u00E9 zm\u011Bnou dynamick\u00E9ho tlaku slune\u010Dn\u00EDho v\u011Btru. Tlou\u0161\u0165ka vrstvy se znateln\u011B zvy\u0161uje (od zlomk\u016F Re a\u017E na v\u00EDc ne\u017E 1,4 R"@cs . "Kol\u00EDs\u00E1n\u00ED tlou\u0161\u0165ky LLBL v z\u00E1vislosti na dynamick\u00E9m tlaku slune\u010Dn\u00EDho v\u011Btru a na orientaci meziplanet\u00E1rn\u00EDho magnetick\u00E9ho pole"@cs . "0148-0227" . "Sauvaud, J. A." . .