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| − | This page is a summary of the work by Working Group 5, dedicated to predicting the southern magnetic field component of CMEs.
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| − | =='''WG5 Statement'''==
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| − | The presence of southward magnetic fields in ICMEs are
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| − | the most important factor in producing geomagnetic storms.
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| − | The challenge is that direct observations of magnetic fields near the Sun
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| − | are extremely limited: currently possible only in the
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| − | photosphere/chromosphere
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| − | at the solar end and by in-situ observations at 1 AU.
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| − | WG5 aims to understand and reconstruct the possible flux
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| − | rope magnetic structure
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| − | of CMEs/ICMEs from observations and models. It also aims to
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| − | predict the intensity and the duration of of the Bs in ICMEs
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| − | upon arriving at the Earth.
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| − | =='''Methodology'''==
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| − | * Deduce near-Sun |B| of CMEs
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| − | * Deduce near-Sun orientation of CMEs
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| − | * Propagate near-Sun |B| to 1 AU
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| − | * Propagate near-Sun orientation to 1 AU
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| − | * Compare predictions with observations at 1 AU
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| − |
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| − | ===Preliminary Work Plan===
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| − | * Find suitable datasets for near-Sun |B| field calculations applicable
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| − | to as many of the available methods as possible --- start with events
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| − | already analyzed by the various team members ----coordinate w/ the
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| − | data and campaign WGs (yrs 1-2)
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