Difference between revisions of "User:Spatsour"
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===Preliminary Work Plan=== | ===Preliminary Work Plan=== | ||
| − | * Find suitable datasets for near-Sun |B| field calculations applicable to as many of the available methods as possible --- <b> start with events | + | * Find suitable datasets for near-Sun |B| field calculations applicable to as many of the available methods as possible --- <b> start with events already analysed </b> by the various team members ----coordinate w/ the data and campaign WGs (yrs 1-2) |
| − | already analysed </b> by the various team members ----coordinate w/ the data and campaign WGs (yrs 1-2) | ||
* Assess the pros & cons of the various methods of near-Sun |B| determination -- coordinate w/ the theory and modeling WGs (yrs 1-2) | * Assess the pros & cons of the various methods of near-Sun |B| determination -- coordinate w/ the theory and modeling WGs (yrs 1-2) | ||
* Apply methods (existing or improved) to a sample of CMEs and determine near-Sun |B| -> paper and list of events/data (yrs 2-3) | * Apply methods (existing or improved) to a sample of CMEs and determine near-Sun |B| -> paper and list of events/data (yrs 2-3) | ||
* Extrapolate near-Sun |B| & orientation to 1 AU and compare w/ in-situ measurements and MC fittings (Al-Haddad et al. 2013 | * Extrapolate near-Sun |B| & orientation to 1 AU and compare w/ in-situ measurements and MC fittings (Al-Haddad et al. 2013 | ||
for a benchmarking of available MC fitting methods) ->paper and tables of pertinent data (yrs 3-4) | for a benchmarking of available MC fitting methods) ->paper and tables of pertinent data (yrs 3-4) | ||
Revision as of 16:43, 28 November 2014
This page is a summary of the work by Working Group 5, dedicated to predicting the southern magnetic field component of CMEs.
WG5 Statement
The presence of southward magnetic fields in ICMEs are the most important factor in producing geomagnetic storms. The challenge is that direct observations of magnetic fields near the Sun are extremely limited: currently possible only in the photosphere/chromosphere at the solar end and by in-situ observations at 1 AU. WG5 aims to understand and reconstruct the possible flux rope magnetic structure of CMEs/ICMEs from observations and models. It also aims to predict the intensity and the duration of of the Bs in ICMEs upon arriving at the Earth.
Methodology
- Deduce near-Sun |B| of CMEs
- Deduce near-Sun orientation of CMEs
- Propagate near-Sun |B| to 1 AU
- Propagate near-Sun orientation to 1 AU
- Compare predictions with observations at 1 AU
Preliminary Work Plan
- Find suitable datasets for near-Sun |B| field calculations applicable to as many of the available methods as possible --- start with events already analysed by the various team members ----coordinate w/ the data and campaign WGs (yrs 1-2)
- Assess the pros & cons of the various methods of near-Sun |B| determination -- coordinate w/ the theory and modeling WGs (yrs 1-2)
- Apply methods (existing or improved) to a sample of CMEs and determine near-Sun |B| -> paper and list of events/data (yrs 2-3)
- Extrapolate near-Sun |B| & orientation to 1 AU and compare w/ in-situ measurements and MC fittings (Al-Haddad et al. 2013
for a benchmarking of available MC fitting methods) ->paper and tables of pertinent data (yrs 3-4)
