{"id":138,"date":"2018-06-05T20:00:53","date_gmt":"2018-06-05T18:00:53","guid":{"rendered":"https:\/\/sites-lira.obspm.fr\/lea-griton\/?p=138"},"modified":"2019-04-04T11:52:08","modified_gmt":"2019-04-04T09:52:08","slug":"three%e2%80%90dimensional-magnetohydrodynamic-simulations-of-the-solar-wind-interaction-with-a-hyperfast%e2%80%90rotating-uranus","status":"publish","type":"post","link":"https:\/\/sites-lira.obspm.fr\/lea-griton\/2018\/06\/05\/three%e2%80%90dimensional-magnetohydrodynamic-simulations-of-the-solar-wind-interaction-with-a-hyperfast%e2%80%90rotating-uranus\/","title":{"rendered":"Three\u2010Dimensional Magnetohydrodynamic Simulations of the Solar Wind Interaction With a Hyperfast\u2010Rotating Uranus"},"content":{"rendered":"\n<table class=\"wp-block-table\"><tbody><tr><td><strong>Authors:<\/strong><\/td><td><a href=\"http:\/\/adsabs.harvard.edu\/cgi-bin\/author_form?author=Griton,+L&amp;fullauthor=Griton,%20L.&amp;charset=UTF-8&amp;db_key=AST\">Griton,&nbsp;L.<\/a>;&nbsp;<a href=\"http:\/\/adsabs.harvard.edu\/cgi-bin\/author_form?author=Pantellini,+F&amp;fullauthor=Pantellini,%20F.&amp;charset=UTF-8&amp;db_key=AST\">Pantellini,&nbsp;F.<\/a>;&nbsp;<a href=\"http:\/\/adsabs.harvard.edu\/cgi-bin\/author_form?author=Meliani,+Z&amp;fullauthor=Meliani,%20Z.&amp;charset=UTF-8&amp;db_key=AST\">Meliani,&nbsp;Z.<\/a><\/td><\/tr><\/tbody><\/table>\n\n\n\n<figure class=\"wp-block-image\"><img loading=\"lazy\" decoding=\"async\" width=\"1024\" height=\"719\" src=\"https:\/\/sites-lira.obspm.fr\/lea-griton\/files\/2019\/04\/fast_uranus_fig6-1024x719.png\" alt=\"\" class=\"wp-image-139\" srcset=\"https:\/\/sites-lira.obspm.fr\/lea-griton\/files\/2019\/04\/fast_uranus_fig6-1024x719.png 1024w, https:\/\/sites-lira.obspm.fr\/lea-griton\/files\/2019\/04\/fast_uranus_fig6-300x211.png 300w, https:\/\/sites-lira.obspm.fr\/lea-griton\/files\/2019\/04\/fast_uranus_fig6-768x539.png 768w, https:\/\/sites-lira.obspm.fr\/lea-griton\/files\/2019\/04\/fast_uranus_fig6.png 1364w\" sizes=\"auto, (max-width: 1024px) 100vw, 1024px\" \/><figcaption>Figure from the paper. \u00a92018. American Geophysical Union. All Rights Reserved.<\/figcaption><\/figure>\n\n\n\n<p class=\"wp-block-paragraph\"><strong>Abstract: <\/strong>We present magnetohydrodynamic simulations of a fast-rotating planetary magnetosphere reminiscent of the planet Uranus at solstice, that is, with the spin axis pointing to the Sun. We impose a 10 times faster rotation than for Uranus, in order to emphasize the effects of rotation on the magnetospheric tail without the need of an excessively large simulation domain while keeping the qualitative aspects of a supersonic magnetized solar wind interacting with a fast-rotating magnetosphere. We find that a complex helical Alfv\u00e9nic structure propagates downstream at a velocity exceeding the plasma velocity in the magnetosheath. Similarly, the reconnection regions, which mediate the interaction of the planetary magnetic field and the interplanetary magnetic field, do also form a helical structure with the same downstream velocity but a 2 times larger pitch. We speculate that the magnetic field of the helical structure connected to the interplanetary magnetic field asymptotically reduces the phase velocity of the helical structure toward the tailward velocity in the magnetosheath. For our simulations we use the MPI-AMRVAC code which we enhanced with a time-dependent background magnetic field in the splitting of the magnetic field.<\/p>\n\n\n\n<p class=\"wp-block-paragraph\">\u00a92018. American Geophysical Union. All Rights Reserved.<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Authors: Griton,&nbsp;L.;&nbsp;Pantellini,&nbsp;F.;&nbsp;Meliani,&nbsp;Z. Abstract: We present magnetohydrodynamic simulations of a fast-rotating planetary magnetosphere reminiscent of the planet Uranus at solstice, that is, with the spin axis pointing to the Sun. We impose a 10 times faster rotation than for Uranus, in &hellip; <a href=\"https:\/\/sites-lira.obspm.fr\/lea-griton\/2018\/06\/05\/three%e2%80%90dimensional-magnetohydrodynamic-simulations-of-the-solar-wind-interaction-with-a-hyperfast%e2%80%90rotating-uranus\/\">Continuer la lecture <span class=\"meta-nav\">&rarr;<\/span><\/a><\/p>\n","protected":false},"author":52,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[2],"tags":[],"class_list":["post-138","post","type-post","status-publish","format-standard","hentry","category-publications"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v28.3 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>Three\u2010Dimensional Magnetohydrodynamic Simulations of the Solar Wind Interaction With a Hyperfast\u2010Rotating Uranus - L\u00e9a Griton<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/sites-lira.obspm.fr\/lea-griton\/2018\/06\/05\/three\u2010dimensional-magnetohydrodynamic-simulations-of-the-solar-wind-interaction-with-a-hyperfast\u2010rotating-uranus\/\" \/>\n<meta property=\"og:locale\" content=\"fr_FR\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"Three\u2010Dimensional Magnetohydrodynamic Simulations of the Solar Wind Interaction With a Hyperfast\u2010Rotating Uranus - L\u00e9a Griton\" \/>\n<meta property=\"og:description\" content=\"Authors: Griton,&nbsp;L.;&nbsp;Pantellini,&nbsp;F.;&nbsp;Meliani,&nbsp;Z. Abstract: We present magnetohydrodynamic simulations of a fast-rotating planetary magnetosphere reminiscent of the planet Uranus at solstice, that is, with the spin axis pointing to the Sun. 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Abstract: We present magnetohydrodynamic simulations of a fast-rotating planetary magnetosphere reminiscent of the planet Uranus at solstice, that is, with the spin axis pointing to the Sun. 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