Working Group A: Morphology of the 3-d corona

Members: D. Biesecker, S. Zidowitz, A Panasyuk, and D. Vibert.

Most of this derives from working with Working Group D and from D. Biesecker and S. Zidowitz. If anybody would like to add to this or make suggestions, they are more than welcome to contact D. Biesecker, the working group leader.

Our outline for a paper for Science follows.

1) Our `standard' view of the corona

• 1) Image of the corona
• 2) WSM synoptic map

Here we would discuss what we can and cannot learn from such a picture. In particular, we would address the shortcomings of observations which suffer from line of sight effects.

2) A 3-d view of the Sun
Figures:

• 1) An isosurface of density
• 2) Show the Ne in the plane of the sky that corresponds to the image of the corona shown in the first part
• 3) Show a synoptic map of Ne as in the first part.)

Here, we can bring out the way in which we may have been deceived by the old `standard' way of looking at the solar corona. Bring out the advantages of the 3-d modelling.

3) Densities in different structures
Figures:

• 1) Density v Height in different structures
• 2) Synoptic map of something else (C1 (Magnetic fields) or soemthing sensitive to T)

Here, we would show how the density in the corona relates to other observables and/or features in the photosphere.

There are a variety of other possibilities which can be explored with deconvolved data.

1) How do the complex structures low in the corona evolve into the simple streamer structures seen high up? Related to this is, What is the fine structure of the current sheet?

2) Volume measurements in the corona can be derived. These can be used to derive accurate temperatures.

3) We can look at the morphology of individual structures. For example, the `quiet-sun' streamer boundary or the boundary of the Elephant's trunk. `Stacked' synoptic maps may be useful for this.

4) Compare the LASCO C1 emission density (C1) to MkIII observations.

Doug Biesecker