Difference between revisions of "Working Group 2"
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==== - How long the Lorentz force dominates over the aerodynamic drag==== | ==== - How long the Lorentz force dominates over the aerodynamic drag==== | ||
==== - How the inductive effects affect the CME eruption and ICME propagation?==== | ==== - How the inductive effects affect the CME eruption and ICME propagation?==== | ||
| − | ==== - What is the role of the ICME/ambient-field reconnection ?==== | + | ==== - What is the role of the ICME/ambient-field reconnection?==== |
| − | ===How variable ambient conditions affect ICMEs=== | + | ===How much variable ambient conditions affect ICMEs?=== |
==== - Which processes are involved in ICME-ICME interactions?==== | ==== - Which processes are involved in ICME-ICME interactions?==== | ||
==== - How ICME-ICME interactions affect the dynamics and evolution of ICMEs?==== | ==== - How ICME-ICME interactions affect the dynamics and evolution of ICMEs?==== | ||
| + | ==== - How high-speed solar wind streams (corotating interacting regions) affect ICMEs?==== | ||
| + | ==== - How the ICME-driven shock evolves in the decreasing Alfven-velocity environment?==== | ||
| + | |||
===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?=== | ===How to measure 3-D geometric and kinematic properties of CMEs far from the Sun, e.g., FOVs of HI-2?=== | ||
Revision as of 03:57, 30 May 2013
Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)
Contents
- 1 Scientific Objectives
- 2 Scientific Questions
- 2.1 Which 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 much variable ambient conditions affect ICMEs?
- 2.2.1 - Which processes are involved in ICME-ICME interactions?
- 2.2.2 - How ICME-ICME interactions affect the dynamics and evolution of ICMEs?
- 2.2.3 - How high-speed solar wind streams (corotating interacting regions) affect ICMEs?
- 2.2.4 - How the ICME-driven shock evolves in the decreasing Alfven-velocity environment?
- 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 Which 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
Which 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 much variable ambient conditions affect ICMEs?
- Which processes are involved in ICME-ICME interactions?
- How ICME-ICME interactions affect the dynamics and evolution of ICMEs?
- How high-speed solar wind streams (corotating interacting regions) affect ICMEs?
- How the ICME-driven shock evolves in the decreasing Alfven-velocity environment?
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
