Index of /~ptg/sipworkii/data

      Name                    Last modified       Size  Description


[DIR] Parent Directory        18-Apr-2006 11:01      -  
[DIR] bbso/                   01-Nov-2004 15:13      -  
[DIR] eit/                    14-Sep-2004 11:46      -  
[DIR] lasco/                  15-Sep-2004 10:31      -  
[DIR] mdi_continuum/          01-Nov-2004 14:36      -  
[DIR] mdi_magnetogram/        01-Nov-2004 14:45      -  
[DIR] rhessi/                 10-Sep-2004 12:20      -  
[DIR] trace/                  28-Oct-2004 10:10      -  

SIPWork II Data Archive Contents and Data Description
-----------------------------------------------------

There are 4 working groups, based on data type. These are
(1) Coronal feature - EIT, TRACE
(2) Coronagraphs -LASCO, MLSO, etc.
(3) Magnetic fields -MDI, BBSO, NSO, etc.
(4) Ground Based - H-alpha, G-band, etc..

There are obvious crossover between each group (e.g., Can you identify an
active region in various wavelengths), but because of time constraints 
it is probably best to keep to single wavelength studies. Obviously all these problems
will not be solved in an afternoon, but it will generate discussion.

There are several questions common to each group

what should we catalog and why?  
Should we number other features - active regions are numbered, why not other features?

What are the characteristics of the various features or regions on the 
Sun?
  - Active regions
  - coronal holes
  - solar wind source areas?
  - filaments

What features in the quiet Sun can we detect?

Can we identify newly emerging flux regions in the data?
How early can we detect newly emerging flux

What is an active region?
How do active regions evolve?

What special problems do solar images pose to the image processing community?
What makes solar data a challenge to the image processing community?

How much of an effect does the instrument have on the observation?  
For instance, there are multiple magnetogram/ h-alpha instruments - can two 
algorithms be made to produce the same results on data from different 
sources?

There are also several questions specific to each group

Coronal Features
-------------------
Can we count the loops in an active region, or measure the 
"connectivity" of an active region in some way?

EIT waves and EIT dimmings - what are the problems associated with 
detecting faint features on complex/structured backgrounds?

Can you detect and classify the flare, wave, and filament lift-off?

Can you detect and characterize the flare, the spines, and the faint ejection?

Can you detect and characterise bright points?
Can you detect and characterise Coronal hole boundaries?
What tools are best for faint feature identification?

Information on EIT can be found at http://umbra.nascom.nasa.gov/eit
See www.lmsal.com/TRACE for further information on the TRACE instrument.

Coronagraphs
--------------------
Can you detect and characterise the dynamics of the CME? 
What about it's geometry?
What are the best methods for faint-feature extraction?
How do coronagraph image pre-processing techniques compare?

Magnetograms
--------------------

Can you detect and classify the sunspot groups into their Mount Wilson / McIntosh class?
How do they evolve?
What are the possible characteristics of flaring activity?
How can we quantify 'complexity'?
Which algorithms are best for remapping data?

Information on the MDI instrument can be found at soi.stanford.edu


Ground-Based
--------------------

Can you detect filaments - what are there characteristics?
Can you detect filament liftoffs ?