Difference between revisions of "Working Group 2"
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==Scientific Questions== | ==Scientific Questions== | ||
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===What mechanisms, processes, forces are governing the CME take-off and ICME propagation? === | ===What mechanisms, processes, forces are governing the CME take-off and ICME propagation? === | ||
| − | ====What is the role of reconnection==== | + | ====What is the role of the flare-associated reconnection?==== |
| + | ====What is the role of emerging flux and poloidal-flux injection?==== | ||
| + | ====How long the Lorentz force dominates over the aerodynamic drag==== | ||
| + | ====How the inductive effects affect the CME eruption and ICME propagation?==== | ||
| + | ====What is the role of the ICME/ambient-field reconnection ?==== | ||
===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?=== | ===How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?=== | ||
Revision as of 03:32, 30 May 2013
Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)
Contents
- 1 Scientific Objectives
- 2 Scientific Questions
- 2.1 What mechanisms, processes, forces are governing the CME take-off and ICME propagation?
- 2.1.1 What is the role of the flare-associated reconnection?
- 2.1.2 What is the role of emerging flux and poloidal-flux injection?
- 2.1.3 How long the Lorentz force dominates over the aerodynamic drag
- 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?
- 2.1.5 What is the role of the ICME/ambient-field reconnection ?
- 2.2 How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?
- 2.3 How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?
- 2.4 How to reconstruct the 3-D structure of ICMEs from in-situ observations?
- 2.5 What is the cause of "stealth" CMEs, i.e., CMEs without clear surface signature?
- 2.6 What is the cause of "problematic" ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?
- 2.7 Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?
- 2.8 What are event periods which need special attention for linking solar to in situ observations?
- 2.1 What mechanisms, processes, forces are governing the CME take-off and ICME propagation?
- 3 Future Plan
Scientific Objectives
- Initiation of CMEs and their take-off dynamics ("acceleration stage")
- Heliospheric dynamics of ICMEs and evolution of their structure
- Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects
- CME/ICME-associated phenomena (flares, shocks, etc.)
Scientific Questions
What mechanisms, processes, forces are governing the CME take-off and ICME propagation?
What is the role of the flare-associated reconnection?
What is the role of emerging flux and poloidal-flux injection?
How long the Lorentz force dominates over the aerodynamic drag
How the inductive effects affect the CME eruption and ICME propagation?
What is the role of the ICME/ambient-field reconnection ?
How to measure 3-D geometric and kinematic properties of CMEs in the corona, e.g., FOVs of COR1, COR2 and HI-1?
- croissant modeling a la Thernisien et al. (software available in IDL SolarSoft: "rtsccguicloud")
How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?
- Geometrical modeling, approximating the CME front with geometrical shapes (points, circles). The IDL SolarSoft SATPLOT software can be used to extract and model time-elongation tracks of CMEs from STEREO/COR2/HI1/HI2 Jmaps.
How to reconstruct the 3-D structure of ICMEs from in-situ observations?
- flux rope modeling:
- minimum variance analysis
- Grad-Shafranov method (non-force-free)
- force-free cylindrical flux ropes
What is the cause of "stealth" CMEs, i.e., CMEs without clear surface signature?
What is the cause of "problematic" ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?
Can we find examples of front-side full halo CMEs in C2, but have no ICME signatures at 1 AU? Does this kind of event exist or not?
What are event periods which need special attention for linking solar to in situ observations?
- interacting events, very fast or very slow CMEs, or other special properties
- late July to early August 2010
- February 2011
- early March 2012
- July 2012
