First ISSI Meeting on
“Coordinated Observations of the Gravitational Focusing Cone of the Local Interstellar Medium at 1 AU”
Space Science Center and Department of Physics, University of New Hampshire
John Raymond, SOHO UVCS
George Gloeckler, ACE and Ulysses SWICS
Daniel Rucinski, (Maciej Bzowski), Modeling
(Howard Ogawa, Darrell Judge), Don McMullin, SOHO CELIAS SEM
Rosine Lallement, EUV Absorption, SOHO SWAN
(William Thompson), SOHO CDS
Manfred Witte, Ulysses GAS
Hans Fahr, Modeling
Sergei Chalov, Modeling
Reinald Kallenbach, Ruedi von Steiger, ISSI
Eberhard Möbius, Chair
Invited: Toshio Terasawa, Hirotomo Noda, University of Tokyo, Japan, GEOTAIL, NOSOMI
______: Either confirmation to me about attendance or with ISSI about accomodations
( ): Won’t be able to attend.
In the following I will lay out the tentative structure of our meeting and related plans. Because we are a small group this is flexible, but the better we plan ahead the more effective our meeting will be. Please feel free to send me any comments, criticisms additions etc. that you might have. Titles and names are suggestions, of course, completely biased by my narrow view. I expect that the program and sequence will develop as we go. Also, please let me know of any specific presentations, important for our work, which you may want to contribute. However, please bear in mind that this should be a working meeting with detailed on-site work and not a meeting filled with presentations. We need to understand each other’s data and models though in order to get going. I still feel that the best way to do this is by some focused introductory talks.
For our detailed work we will need the main data sets on site, meaning one of the ISSI computers. I have talked about this with Ruedi. ISSI is prepared to assist us with their computers. In order to hit the ground running we will need the data ready before our meeting starts. I have already talked with some of you about contents and possible formats. The idea is not to shift any copies of raw data to ISSI. What we are interested in are the products of your work. However, the data need to be traceable, meaning:
- results should still contain any ancillary data inputs explicitly
- if models are used to derive final results, it would be better to include both the final result and the observable from which it has been derived (We would like to be able to explore, how the result changes with parameter modifications in the model and with the use of alternate models)
Also it would be a good idea to have some of the key models available, not necessarily the code, which may be very elaborate, but the results in a parameterized form.
Mulling over this, I think, both data and results from models would be best in a spreadsheet format. This will allow easy access and simple manipulations on site. Let me give you my first cut below.
- Pickup Ions: Suitable time averages (1 day?) of normalized energy flux or phase space density spectra over the interesting time period will a reasonable data set. Other information?
- EUV Lines (UVCS and EUVE): A set of calibrated absolute intensities with the viewing directions in GSE coordinates and heliospheric (ecliptic) coordinates along with spacecraft position will be needed. Other information?
- He Density Models: Density as a function of distance from the sun and distance from the inflow vector (with the inflow vector given in heliospheric coordinates. Sets of densities should be available parameterized according to ionization rate, inflow speed, LISM temperature. A normalized density would be preferable, so that we can adjust the absolute density as a simple parameter. Other parameters?
- Neutral Densities: Manfred, I have not come up with a good idea yet, how to implement your data. Do you have a feasible idea?
- Solar EUV Monitor Data: Integral fluxes and fluxes in the 304 Å band as a function of time (I believe 5 minute averages are readily available) along with the calibration factor between flux and ionization rate of He.
- CDS Full Sun Scans: Bill, thank you for your data set. This will be great for a comparison with the SEM data, which we have for the entire time periods.
- Ancillary Data: Solar wind proton, alpha fluxes, proton densities and speeds as a function of time (from ACE and/or SOHO); cross-sections for charge exchange. Daniel, how do we treat electron ionization without too much hassle?
- Anything else?
Structure of the meeting (Draft)
Welcome, overview, logistics, plan for the week (Möbius, von Steiger)
Local Interstellar Parameters, benchmark values for a
local sample of cosmic matter
– Where are we and where are we going? (Möbius)
Multi-fluid character of the interaction between the heliosphere and the interstellar medium (Fahr)
of the interstellar neutral gas in the heliosphere and its temporal variations
and velocity distribution of He pickup ions in the cone region
– Related transport and acceleration processes (Chalov)
Helium parameters from EUV absorption observations (Lallement)
Diagnostics of the focusing cone close to the sun (Raymond)
Scan of the focusing cone in the anti-sunward direction (Vallerga)
Interstellar parameters from pickup ion measurements at 1 AU and from Ulysses (Gloeckler)
Instrumentation for He pickup on Geotail and the Nosomi Mars Probe (Terasawa)
He pickup ion observations with Geotail and Nosomi (Noda)
Interstellar parameters from neutral gas measurements (Witte)
Determination of the photoionization rate for He (McMullin)
General discussion of our approach, response by modelers, split into WGs (all)
Work on data and interpretation in WGs
a) Remote sensing group (Lallement, Raymond, Vallerga + some modelers + 1 ISSI)
b) In-situ group (Gloeckler, Möbius, Witte, McMullin, Terasawa, Noda + some modelers + 1 ISSI)
Use plenary meetings as needed, but at least every morning and after lunch.
Presentation of WG results and open questions WGs
Plans for work at home, publication plans, next meeting (all)
Executive Meeting (subgroup including Möbius, von Steiger, Kallenbach + others)