"P(GA205/09/0170), P(ME09056), S, Z(MSM0021620860)" . "10.1016/j.pss.2011.03.016" . "N\u011Bme\u010Dek, Zden\u011Bk" . . . "8"^^ . "Richardson, J. D." . "http://dx.doi.org/10.1016/j.pss.2011.03.016" . "9" . . . . "NL - Nizozemsko" . "Deformation of ICMEs/MCs along their path" . "Deformation of ICMEs/MCs along their path"@en . . "000292722100004" . "Deformation of ICMEs/MCs along their path"@en . "Lynnyk, Andrii" . . . . "\u0160afr\u00E1nkov\u00E1, Jana" . . "[75EB0A8F65B1]" . "193141" . . . . "0032-0633" . "3"^^ . "Planetary and Space Science" . "Interplanetary coronal mass ejections (ICMEs) and their subset, magnetic clouds (MCs), are important manifestations of solar activity which have substantial impact on the geomagnetic field. We re-analyze events already identified in Wind and Voyager 2 data and estimate changes of their geometry along the path from the Sun. The analysis is based on the thickness of the sheath between a shock and a particular ICME or MC which is proportional to the apparent curvature radius of ICMEs/MCs. We have found that this apparent radius of curvature increases with the Mach number and this effect is attributed to the larger deformation of the fast ICME/MC. Further, the relative sheath thickness that is proportional to the flux rope oblateness decreases with the magnetic field intensity inside the ICME/MC and increases with the heliospheric distance." . . "11320" . "Deformation of ICMEs/MCs along their path" . . . . "Interplanetary coronal mass ejections (ICMEs) and their subset, magnetic clouds (MCs), are important manifestations of solar activity which have substantial impact on the geomagnetic field. We re-analyze events already identified in Wind and Voyager 2 data and estimate changes of their geometry along the path from the Sun. The analysis is based on the thickness of the sheath between a shock and a particular ICME or MC which is proportional to the apparent curvature radius of ICMEs/MCs. We have found that this apparent radius of curvature increases with the Mach number and this effect is attributed to the larger deformation of the fast ICME/MC. Further, the relative sheath thickness that is proportional to the flux rope oblateness decreases with the magnetic field intensity inside the ICME/MC and increases with the heliospheric distance."@en . "4"^^ . . "RIV/00216208:11320/11:10108220" . . "RIV/00216208:11320/11:10108220!RIV12-GA0-11320___" . "59" . . . "Interplanetary coronal mass ejections; Deformation"@en .