Difference between revisions of "Working Group 1"
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*Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models | *Provide a comprehensive event '''database''' for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models | ||
| − | ==Scientific Questions | + | ==Scientific Questions== |
===What are the criteria of Earth-affecting CMEs?=== | ===What are the criteria of Earth-affecting CMEs?=== | ||
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| + | ===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?=== | ||
| + | |||
| + | ===How reliably can we link solar to in situ CME observations?=== | ||
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| + | == Events == | ||
| + | |||
| + | === What are event periods which need special attention for linking solar to in situ observations?=== | ||
| + | *link to WG4 | ||
| + | *use simulation results from WG3 | ||
| + | *e.g. 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 | ||
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| + | |||
| + | == Techniques, Methodology == | ||
===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?=== | ||
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#force-free cylindrical flux ropes | #force-free cylindrical flux ropes | ||
#new models? | #new models? | ||
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==Future Plan== | ==Future Plan== | ||
Revision as of 04:52, 12 June 2013
Data group led by Jie Zhang (USA) and Christian Mostl (Austria)
Contents
- 1 Scientific Objectives
- 2 Scientific Questions
- 2.1 What are the criteria of Earth-affecting CMEs?
- 2.2 What is the cause of "stealth" CMEs, i.e., CMEs without clear surface signature?
- 2.3 What is the cause of "problematic" ICMEs, i.e., ICMEs without clear CME counterparts near the Sun?
- 2.4 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?
- 2.5 How reliably can we link solar to in situ CME observations?
- 3 Events
- 4 Techniques, Methodology
- 5 Future Plan
Scientific Objectives
- Identify all Earth-Affecting ICMEs during the STEREO era (2007-today)
- Track these events from the Sun to the Earth, and fully measure, characterize and quantify their properties and evolution from the Sun to the Earth
- Provide a comprehensive event database for statistical study, for creating empirical evolution and prediction models, for theoretical understanding, and for comparing and validating numerical models
Scientific Questions
What are the criteria of Earth-affecting CMEs?
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?
How reliably can we link solar to in situ CME observations?
Events
What are event periods which need special attention for linking solar to in situ observations?
- link to WG4
- use simulation results from WG3
- e.g. 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
Techniques, Methodology
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
- new models?
