Working Group 1
Data group led by Jie Zhang (USA) and Christian Mostl (Austria)
Contents
- 1 Scientific Objectives
- 2 Scientific Questions, Technique Approach/Methodology
- 2.1 What are the criteria of Earth-affecting CMEs?
- 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?
- 3 Future Plan
Scientific Objectives
- Identifying all Earth-Affecting ICMEs during the STEREO era (from 2007)
- Tracking these events from the Sun to the Earth, and fully measuring/characterizing/quantifying the properties/evolution from the Sun to the Earth
- Providing a comprehensive event database for statistical study, for creating empirical evolution/prediction model, for theoretical understanding, and for comparing/validating numerical models
Scientific Questions, Technique Approach/Methodology
What are the criteria of Earth-affecting CMEs?
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 CMEs, or other special properties
- late July to early August 2010
- February 2011
- early March 2012
- July 2012
