Open AccessMHD simulation of an interaction of a shock wave with a magnetic cloud
Author(s) -
Vandas M.,
Fischer S.,
Dryer M.,
Smith Z.,
Detman T.,
Geranios A.
Publication year - 1997
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/97ja01675
Subject(s) - physics , magnetic cloud , heliosphere , magnetohydrodynamics , ejecta , coronal mass ejection , shock wave , solar wind , interplanetary spaceflight , coronal cloud , shock (circulatory) , rope , corona (planetary geology) , mechanics , magnetic field , computational physics , geophysics , astrophysics , astrobiology , supernova , medicine , structural engineering , quantum mechanics , engineering , venus
Interplanetary shock waves, propagating in the heliosphere faster than earlier‐emitted coronal ejecta, penetrate them and modify their parameters during this interaction. Using two and one half dimensional MHD simulations, we show how a magnetic cloud (flux rope) propagating with a speed 3 times higher than the ambient solar wind is affected by an even faster traveling shock wave overtaking the cloud. The magnetic field increases inside the cloud during the interaction as it is compressed in the radial direction and becomes very oblate. The cloud is also accelerated and moves faster, as a whole, while both shocks (driven by the cloud and the faster interplanetary shock) merge upstream of the cloud. This interaction may be a rather common phenomenon due to the frequency of coronal mass ejections and occurrence of shock waves during periods of high solar activity.