<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="6.x">Drupal-Biblio</source-app><ref-type>10</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Poedts, S.</style></author><author><style face="normal" font="default" size="100%">Jacobs, C.</style></author><author><style face="normal" font="default" size="100%">van der Holst, B.</style></author><author><style face="normal" font="default" size="100%">Chane, E.</style></author><author><style face="normal" font="default" size="100%">Keppens, R.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Numerical simulations of the solar corona and Coronal Mass Ejections</style></title></titles><keywords><keyword><style  face="normal" font="default" size="100%">coronal mass ejections</style></keyword><keyword><style  face="normal" font="default" size="100%">Magnetohydrodynamics</style></keyword><keyword><style  face="normal" font="default" size="100%">numerical</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2009</style></year></dates><urls><web-urls><url><style face="normal" font="default" size="100%">&lt;Go to ISI&gt;://000268745500012 </style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">Terra Scientific Publ Co</style></publisher><pages><style face="normal" font="default" size="100%">599-602</style></pages><language><style face="normal" font="default" size="100%">English</style></language><abstract><style face="normal" font="default" size="100%">Numerical simulations Of Coronal Mass Ejections (CMEs) call provide a deeper Insight ill the Structure and propagation of these impressive solar events. lit this work, we present our latest results Of numerical simulations of the initial evolution Of a fast CME. For this purpose, the equations Of ideal MagnetoHydroDynamics (MHD) have been solved on a three-dimensional (3D) mesh by means of an explicit, finite volume solver, where the simulation domain ranges front the lower solar corona Up to 30R(circle dot). In order to simulate the propagation of a CME throughout the heliosphere, a magnetic flux rope is superposed oil top of a stationary background solar (MHD) wind with extra density added to the flux rope. The flux rope is launched by giving it all extra initial velocity in order to get a fast CME forming, a 3D shock wave. The magnetic field inside the initial flux rope is described in terms of Bessel functions and possesses a high amount of twist.</style></abstract><accession-num><style face="normal" font="default" size="100%">ISI:000268745500012</style></accession-num><notes><style face="normal" font="default" size="100%">ISI Document Delivery No.: 480OLTimes Cited: 0Cited Reference Count: 22</style></notes><custom1><style face="normal" font="default" size="100%">Fusion Physics</style></custom1></record></records></xml>