{"id":5363,"date":"2021-06-24T14:58:25","date_gmt":"2021-06-24T12:58:25","guid":{"rendered":"https:\/\/www.mi.uni-koeln.de\/NumSim\/?p=5363"},"modified":"2021-06-24T15:03:41","modified_gmt":"2021-06-24T13:03:41","slug":"snapshot-evolution-of-a-magnetized-torus-differentially-rotating-around-a-static-point-mass","status":"publish","type":"post","link":"https:\/\/www.mi.uni-koeln.de\/NumSim\/2021\/06\/24\/snapshot-evolution-of-a-magnetized-torus-differentially-rotating-around-a-static-point-mass\/","title":{"rendered":"Snapshot: Evolution of a magnetized torus differentially rotating around a static point mass"},"content":{"rendered":"\r\n
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Evolution of a magnetized torus differentially rotating around a static point mass. [1] The torus gradually forms into an accretion disk with expanding filaments into the surrounding space due to magneto-rotational instabilities similar to the rich structure of the corona of our sun. The simulation was done with a new Discontinuous-Galerkin based MHD solver [2] in FLASH [3]. Fig. 1 and Fig. 2 show the log. scale density cross section in the x-y and x-z plane. Fig 3 highlights the rich structure of the magnetic field (white stream lines) overlayed on top of the log. scale magnetic pressure in the x-z plane.<\/p>\r\n<\/div>\r\n<\/div>\r\n\r\n\r\n\r\n

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