The Structure of Magnetic Clouds in the Inner Heliosphere: An Approach Through Grad-Shafranov Reconstruction

Details The Structure of Magnetic Clouds in the Inner Heliosphere: An Approach Through Grad-Shafranov Reconstruction The Structure of Magnetic Clouds in the Inner Heliosphere: An Approach Through Grad-Shafranov Reconstruction

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh42a..05h&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH42A-05

Physics

[2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds

Scientific paper

Magnetic Clouds (MCs), as a subset of Interplanetary Coronal Mass Ejections (ICMEs), are commonly observed in space. They have been extensively studied with respect to their origin at the Sun, their propagation, and their structures in the inner heliosphere between Sun and Earth. A method, based on the in-situ spacecraft measurements across such structures and the Grad-Shafranov (GS) equation, has been developed and widely used to derive their 2.5D cross-section from the single-spacecraft magnetic field and plasma data. We provide a brief review of the GS reconstruction of MC structures and its applications to various spacecraft mission data and Sun-Solar System Connection science. We then report the recent progress on the application of GS method to the MC structures by examining the effect of (1) inclusion of electron temperature (pressure), since Te is often >> Tp in these configurations, and (2) a locally torus-shape geometry of the MC flux rope, as opposed to the commonly assumed straight-cylinder geometry. Case studies will be presented to illustrate our results.

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