Expansion of magnetic clouds in the solar wind

Details Expansion of magnetic clouds in the solar wind Expansion of magnetic clouds in the solar wind

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1943v&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1943

Physics

[2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2134] Interplanetary Physics / Interplanetary Magnetic Fields, [2164] Interplanetary Physics / Solar Wind Plasma

Scientific paper

Magnetic clouds are supposed to be large interplanetary flux ropes propagating away from the Sun. Due to enhanced inner magnetic pressure, they expand during their travel. We analyze magnetic cloud observations using OMNI database and fit them by our models with cylindrical or toroidal geometry. Comparison of the time-dependent models with observations is shown for several cases with a detailed discussion. In addition to magnetic field vectors, also velocity vectors are modeled, and it is found that the radial velocity component behaves as expected. In some cases, analysis of velocity components helps up to determine, which model is more appropriate, cylindrical or toroidal one, that is, if curvature plays a role.

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