2.2.6 spase://CNES/SimulationRun/CDPP-AMDA/TAO/Cassini Tao Model SW propagated from Earth to Cassini (cruise) 2014-07-08T14:48:29Z These data sets are the simulation outputs of solar wind variations observed near the Earth and propagated to the different destinations using a 1-dimensional 2-component (radial and azimuthal) magnetohydrodynamic (MHD) model.The model code is based on the Coordinated Astronomical Numerical Software (CANS) by JST. Model details, evaluations compared with observation data, and limitations are described in Tao et al. 2005, J. Geophys. Res., 110, A11208, doi:10.1029/2004JA010959 The radial magnetic field along parker spirals is computed using : br = cass_input_b*cass_input_v(0)*1000./(2*pi/25.38/86400)/(2.5*Rsun-r_cass*AU) spase://CNES/Person/Chihiro.Tao PrincipalInvestigator spase://CNES/SimulationModel/CDPP-AMDA/Tao Cassini Cartesian RTN 2 AU Density Proton Velocity Proton Tangential Field Component Magnetic