Physical Parameters to be Passed Between Models

Space Environment Modeling Workshop:"Towards Compatibility"
April 9-10, 2002

Community Survey
"Physical Parameters to be Passed Between Models"

Results

Physical Parameters to be passed from Solar Interior to Solar Atmosphere

Parameters:
Plasma Density
Temperature/Pressure
Velocity (vector)
Magnetic Field (vector)

Comments:
Pass time step information

Location of transition region
- On the adjoining numerical grids (face centered or cell centered)
- Overlapping grids for gradient information and data passing

Probably best thing here given state of the art is some observation-based photospheric boundary condition "data base." In particular, radial B fields given for Carrington Rotations.

Physical Parameters to be passed from Solar Atmosphere to Solar Wind

Parameters: Plasma Density Temperature/Pressure Velocity (vector) Magnetic Fields (vector)	Comments: Pass time step information Location of the transition region - Beyond the outer most critical points (approx. 20-30 solar radii) - On the adjoining numerical grids (face centered or cell centered) - Overlapping grids for gradient information and data passing

Physical Parameters to be passed from Solar Wind to Magnetosphere

Parameters:
Required by present models
- Density
- Pressure
- Velocity (vector)
- Magnetic Field (vector)

Future possibilities
- Minore species (e.g. He)
- Energetic Particles
- Wave Spectra: important for SW driving of ULF waves in magnetosphere

Comments:
"What and Where" can be as important as "what".

Interpolation of 3D data from one grid to another

Need to allow for possibility of 3D description of solar wind input to magnetospheric models

Differen variable description (i.e., cell-centered and face centered)

Extensibility of variables is important for future extensions of models

Physical Parameters to be passed from Solar Atmosphere to Ionosphere

Parameters: 10.7 cm Flux (for now) Spectra of EUV (ideal) Average Energy of Precipitating Electrons	Comments:

Physical Parameters to be passed from Solar Atmosphere to Ionoshpere Electrodynamic

Parameters: 10.7 cm Flux (for now) Spectra of EUV (ideal) Average Energy of Precipitating Electrons	Comments:

Physical Parameters to be passed from Solar Wind to Inner Magnetosphere

Parameters: SW Density N SW Velocity V	Comments:

Physical Parameters to be passed from Magnetosphere to Inner Magnetosphere

Parameters: 3D magnetic field Inner plasma sheet density Inner plasma sheet temperature Field line volume (for RCM)	Comments: What drives Ring Current and Radiation Belt Models -Magnetic field model -Convection electric field model -Particle distribution at model boundary -Radial diffusion model -Models of wave-particle interaction

Physical Parameters to be passed from Inner Magnetosphere to Magnetosphere

Parameters: Pressure in Inner Magnetosphere Subauroral Electric Potential Ionospheric Potential at MHD Equatorward Boundary	Comments:

Physical Parameters to be passed from Magnetosphere to Plasmasphere

Parameters: Estimated auroral particle precipitation	Comments:

Physical Parameters to be passed from Magnetosphere to Ionosphere Electrodynamic

Parameters: Field-Aligned currents Estimated auroral particle preciptation	Comments:

Physical Parameters to be passed from Ionosphere Electrodynamic to Magnetosphere

Parameters: Convection electric field	Comments:

Physical Parameters to be passed from Ionosphere to Magnetosphere

Parameters: Perpendicular velocity Outgoing density Temperature Field-aligned velocity of different species	Comments:

Physical Parameters to be passed from Magnetosphere to Ionosphere

Parameters:
Field Aligned Currents

Precipitating electron total and average energy flux

More Complex
- Precipitation electron distribution function and ion distribution function with some indication of pitch angels
- Interhemispheric transport on closed field lines through the magnetosphere

Comments:

Physical Parameters to be passed from Ionosphere Electrodynamic to Ionosphere

Parameters: Convection Electric Field	Comments:

Physical Parameters to be passed from Ionosphere to Ionosphere Electrodynamics

Parameters: Height integrated diffusion of neutral wind Height integrated conductances	Comments:

Physical Parameters to be passed from Ionosphere Electrodynamic to Inner Magnetosphere

Parameters: Ionosphereic potential distribution Height integrated conductances	Comments:

Physical Parameters to be passed from Inner Magnetosphere to Ionosphere Electrodynamic

Parameters: Field-aligned currents Ions and Electrons Precipitation in sub-auroral region	Comments:

Physical Parameters to be passed from Plasmasphere to Ionosphere

Parameters: Downward flux of ions on the nightside Interhemispheric transport on closed field lines through magnetosphere	Comments:

Physical Parameters to be passed from Plasmasphere4 to Inner Magnetosphere

Parameters: Models of wave-particle interatction Geocorona of different species to calculate loss rate of ions and electrons	Comments:

Physical Parameters to be passed from Neutral Atmosphere to Ionosphere

Parameters:
Neutral parameters in spherical, geophysical coordinates every 15 minutes
- Neutral density
- Neutral temperature
- Neutral wind

Electric Field
- Empirical model
- Self-consistent (need the neutral wind for low-to-mid latitude ionosphere)

Plasma dynamics
- Magnetic coordinate system, decoupled parallel and perpendicular plasma dynamics
- Tilted diople, offset tilted diople, IGRF

Comments:
Ionosphere models keep track on both coordinate systems

Physical Parameters to be passed from Ionosphere to Neutral Atmosphere

Parameters: Species Density Species velocity Species temperature Precipitation electron and ion distribution function to calculate ionoization rates and heating rates	Comments: Ionosphere and Neutral Atmosphere are not easily decoupled. Almost every parameter for different models at each grid cell. Photoionization requires that you know the local density for all of the atom/molecules which are going to be photoionized and Chapman integral for all neutral constituents.