Coronal Hole Boundary Working Group
To: E. Antonucci, J. Geiss, J. Raymond, P. Riley, R. von Steiger
CC: L.A. Fisk, G. Gloeckler, J. Kohl
From: Thomas Zurbuchen
Re: 1st meeting in Bern, June 26-28
Dear colleagues,
The time is coming closer when we will meet
at ISSI for our first meeting of the working group. This group should
facilitates a very natural combination of UVCS and SWICS data, comparing
composition in the corona and in interplanetary space.
During
the CME workshop in Elmau, where most of you participated, we finally decided
to attack this problem. The idea was to have a very small group starting in
mid-June and get much of the work done. ISSI seemed like the perfect place for
this. Many of us either work there or happen to be there differnent reasons.
Only Pete will not be able to join the first meeting of this core-group, he
will participate remotely.
I
was thinking during this weekend about how to perform this work. Here are my
first thoughts, questions and planning. Please add and comment as you like.
Ruedi and I will then sit together and include your comments and suggestions.
The enclosed program is meant to be a start point for discussions. Do not
over-interpret what is in there…
With best regards - see you in Bern !
Thomas
Zurbuchen
June ISSI Meeting
It is the purpose of this working group to
address the following questions:
1.
What is the nature of coronal hole boundaries and what is their
structure from the photosphere to the corona?
2.
Are these boundaries associated with tangential or rotational
discontinuities ?
3.
Are there non-ambiguous signatures of super-radial expansion ?
These questions will be addressed using a
combination of composition data in the corona and the solar wind. Coronal data
will be provided by UVCS, solar wind data by Ulysses (and ACE) SWICS. We will
use a 3D-MHD model of the corona to relate these two sets of data. The code
will also allow to "order" solar wind data according to their
distance from the coronal hole boundary. Over-expansion signatures should
therefore be detected using a super-posed epoch analysis.
This working group will meet June 26-28. The
work will contain the following three steps:
a)
define and specify scientific plan,
b)
know the details of the methods involved (UVCS, SWICS, MHD),
c)
perform one example of a combined data-analysis for CR 1914.
Note that c) implies the availability of data
on a portable computer or the WWW. Also, bring some information to perform
tasks a) and b).
Here
is a preliminary program (times are only to give order of magnitude estimates):
When |
Who |
What |
Day
1: |
|
|
9:00-9:30 |
All |
Coffee at ISSI |
9:30-9:45 |
Von Steiger |
Welcome, ISSI Specific information |
9:45-10:30 |
Geiss |
Scientific Introduction |
10:30-10:50 |
Raymond |
UVCS Point of view: Open issues |
10:50-11:10 |
Antonucci |
UVCS Point of view: Open issues |
10:50-11:10 |
Zurbuchen |
SWICS Work performed, open questions |
11:10-11:30 |
Von Steiger |
SWICS Work performed, open questions |
11:30-11:50 |
Riley (Zurbuchen) |
MHD Code: Performance and limitations |
13:30-16:00 |
All |
Discussion and definition of Tasks a), b) |
17:00-18:00 (8 am for Pete) |
All & Riley |
Telecon: Summary of the
day, |
|
|
|
Day
2: |
|
|
9:00-9:30 |
All |
Coffee at ISSI |
9:30-10:00 |
Zurbuchen, von Steiger |
Recap first day |
10:00-11:00 |
All |
Finalize tasks a) & b) |
11:00-12:00 |
All |
Agree on time-periods |
13:30-14:00 |
All |
Plot/Share data |
14:00-16:00 |
All |
Present, discuss data and
problems |
17:00-18:00 |
All & Pete |
Telecon: Summary of the
day, |
|
|
|