Model Challenge

Concept
We would like to have as many of the simulation groups as possible run their global Mars models using identical input conditions so that the results of each different modeling approach (MHD, Hall MHD, multi-fluid, hybrid) and implementation can be compared at the Chapman conference.

Participating Global Simulationists


Boesswetter / Motschmann	Hybrid
Brecht / Ledvina	Hybrid
Fang / Liemohn	MHD + test particles
Harnett	Multi-fluid
Kallio	Hybrid
Ma / Nagy	MHD / Hall MHD
Modolo / Chanteur	Hybrid
Schoendorf	MHD
Terada / Shinagawa	Hybrid


Model Inputs
IMF:      3 nT, Parker spiral orientation (57^o), oriented in +y and -x directions (MSO)
Solar Wind:      400 km/s, 3 cm^-3 protons (only), T_ions = 5x10⁴ K, T_electrons = 3x10⁵ K
Atmosphere / EUV:      Bougher MTGCM results (click here)
Mars:      no crustal fields
If it is impossible to implement all of these inputs in your models then please incorporate as many as is feasible for you. It is more important to participate in the activity then it is to use all of the inputs. However, the most meaningful comparisons can be made between simulations that incorporate similar input conditions.

Data Products

1. 1-D cut along the Mars-Sun line of dynamic pressure of solar wind H+, total thermal pressure of all particles, and total magnetic pressure. Please provide ASCII files containing cuts ranging at least from +2 to -2 R_M (in units of R_M) at your model resolution. Files should have only 4 columns if possible: location, dynamic pressure, thermal pressure, and magnetic pressure. Pressures may be expressed in any units (please tell us which you are using) - we'll convert to a common unit on our end.
   
   
2. 2-D cut through the center of Mars in the noon-midnight plane of densities of solar wind H+ and planetary O+. Please provide ASCII files containing 2-D cuts of particle number densities at your model resolution. Files should have only 4 columns if possible: MSO x location, MSO z location, solar wind H+ density, planetary O+ density. Preferred units are R_M and #/cm³ (please specify if different units are used).
   
   
3. 1-D cut along a single Mars Express orbit trajectory of MEX of the total flux (number density times velocity) of H+, O+, and e-. An ASCII file containing the MEX trajectory is available here. Please provide ASCII files containing your model results for these quantities, interpolated to the spacecraft locations in the trajectory text file. Please use a Martian radius of 3390 km to convert between your model grid and the trajectory file. Files should have only 4 columns if possible: time (taken directly from the trajectory file), and number fluxes of H+, O+, and e-. Preferred units are #/cm²/s (please specify if different units are used).
   
   
4. Global escape rate of planetary O+, in #/s. Please email me (Dave) with your escape rate.
   
   
These data products should be sent to Dave Brain so that they can be displayed in the same manner for all models. Please send him your inputs ASAP!!!

Contact
Dave Brain - brain@ssl.berkeley.edu - (510) 642-0743