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ESS 265 Simulation Results: OpenGGCM code. UCLA2 Ljiljana Vasic, Lan Jian, Hanying Wei, David Galvan. Solve the MHD equations on a stretched Cartesian grid using second order explicit time integration with conservative and flux-limited spatial finite differences.
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ESS 265 Simulation Results:OpenGGCM code UCLA2 Ljiljana Vasic, Lan Jian, Hanying Wei, David Galvan
Solve the MHD equations on a stretched Cartesian grid using second order explicit time integration with conservative and flux-limited spatial finite differences. Adaptable numerical grid can have from a few times 10^5 to more than 10^8 cells. Thus, the resolution in the MHD grid near the sub-solar magnetopause can be as small as 100 km or as large as 0.5 Re. A Yee grid is used to preserve the magnetic field divergence to round-off error. Does not include the energetic particle drift and ring current physics. No plasmasphere. Wave propagation through the inner magnetosphere is affected. Wave propagation in the inner magnetosphere is artificially slowed due to a `Boris correction' to keep time steps manageable. The developers do not provide any guarantee for the correctness of model results. Properties and Limitations of OpenGGCM (Open Geospace General Circulation Model)
3D MHD Model: OpenGGCM Simulation With Modeled Conditions Inflow Boundary Conditions: Time-Dependent Start Time: 2000/01/01 00:00 End Time: 2000/01/01 04:00 Dipole Tilt at Start in X-Z Plane: 0.0 deg. Dipole Tilt in Y-Z GSE Plane: 0.0 deg. Dipole Update With Time: noIonospheric Conductance: auroral No Corotation Velocity is Applied at The Inner Boundary.Radio Flux 10.7 cm: 150.Coordinate System for the Output: GSE Initial Solar Wind (SW) Parameters in GSM Coordinates: SW Density: 5. n/ccSW Temperature [Kelvin]: 100000 Kelvin X Component of SW Velocity: -400. km/sec Y Component of SW Velocity: 0. km/sec Z Component of SW Velocity: 0. km/sec IMF Bx: 0. nT IMF By: 0. nT IMF Bz: -5. nT IMF |B|: 5.00 nT IMF Clock Angle: 180.0 deg. Initial conditions