Three‐dimensional MHD simulation of a loop‐like magnetic cloud in the solar wind

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Abstract
A magnetic cloud ejected from the Sun is simulated as a part of a toroid. Its evolution and propagation through interplanetary space are studied using three‐dimensional magnetohydrodynamic self‐consistent numerical simulations. The flux rope deforms as it moves from the Sun, and this deformation causes a hypothetical spacecraft to observe the flux rope two times at some locations; that is, it could be crossed at its apex and a flank. Simulated observations at the apex give all three signatures of a magnetic cloud following from its definition. The apex is rather flat and can be approximated by a prolate (in latitude) cylinder. At the flanks of the flux rope the temperature drop is not pronounced, but the magnetic field increase has a double‐peak profile.

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