Data of 3D PPMLR-MHD model Simulation for manuscript "Open Magnetic Field Lines Segregate Auroral Oval Segments to Form Transpolar Arcs"

Data of 3D PPMLR-MHD model Simulation for manuscript "Open Magnetic Field Lines Segregate Auroral Oval Segments to Form Transpolar Arcs" These data come from a fully run of a 3D MHD Simulation model that is named PPMLR-MHD model (detailed descriptions below). There are 2 types of data files: 1) 20150317_XXXXsimulation_data.mat is saved parameters of simulation result. 2) 20150317_XXXX_OCBoundary.fig is saved 3D open close filed lines boundary XXXX is the Universal Time of simulation result. The first type files of data include the following parameters: time, x, y, z, logrho, Vx, Vy, Vz, Bx, By, Bz, T Where, time is simulation time, which need to plus the start time to transfer them to universal time: time+16:00. (x,y,z) are the three components of the position of simulation point in GSM coordinates; logrho is the plasma density at the simulation point; (Vx, Vy,Vz) are the three components of plasma velocity at the simulation point in GSM coordinates; (Bx, By,Bz) are the three components of magnetic field at the simulation point in GSM coordinates; T is the plasma temperature at the simulation point; PPMLR-MHD model The PPMLR-MHD model is on the basis of an extension of the piecewise parabolic method (1) with a Lagrangian remap to magnetohydrodynamics (MHD) (2, 3). It is a three-dimensional MHD model, designed specially for the solar wind–magnetosphere–ionosphere system (4-6). The model possesses a high resolution in capturing MHD shocks and discontinuities and a low numerical dissipation in examining possible instabilities inherent in the system (4). The model uses a Cartesian coordinate system with the Earth’s center at the origin and X, Y, and Z axes pointing towards the Sun, the dawn-dusk direction, and the north, respectively. The size of the numerical box extends from 25 RE to –100 RE along the Sun-Earth line and from –50 RE to 50 RE in Y and Z directions, with 240×240×240 grid points and a minimum grid spacing of 0.2 RE. An inner boundary of radius 3 RE is set for the magnetosphere to avoid the complexities associated with the plasmasphere and large MHD characteristic velocity from the strong magnetic field (6). An electrostatic ionosphere shell with height-integrated conductance is imbedded, allowing an electrostatic coupling process introduced between the ionosphere and the magnetospheric inner boundary. The Earth’s magnetic field is approximated by a dipole field with a dipole moment of 8.06×1022 A/m in magnitude. The model is run to solve the whole system by inputting the real interplanetary conditions for the current event.