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Interplanetary magnetic clouds: Topology and driving mechanism
Author(s) -
Chen James,
Garren David A.
Publication year - 1993
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/93gl02426
Subject(s) - plasma , interplanetary magnetic field , physics , magnetic cloud , magnetic field , solar wind , loop (graph theory) , corona (planetary geology) , magnetic reconnection , mercury's magnetic field , computational physics , interplanetary spaceflight , astrobiology , nuclear physics , quantum mechanics , mathematics , combinatorics , venus
A model is developed to study the origin and propagation of magnetic clouds. Starting with an equilibrium current loop embedded in an ambient plasma consistent with the solar corona, magnetic energy is injected by increasing the loop current. This causes the loop to rise, propelling plasma and magnetic field away from the Sun. Using a simple model of the interplanetary medium, the subsequent dynamics of the loop is calculated to 1 AU and beyond. The macroscopic properties of the resulting structures at 1 AU closely resemble those of observed magnetic clouds. Thermal effects indicate that clouds remain magnetically connected to the Sun in order to yield observed temperatures near 1 AU.