Data of 3D MHD Simulation for manuscript "Multiple transpolar auroral arcs reveal insight about coupling processes in the Earth’s magnetotail" These data come from a fully run of a 3D MHD Simulation model that named by PPMLR-MHD model (detailed descriptions below). There are 3 types of data files: 1) RSW_0378d.dms, which is full 3D Simulation data at 16:10 UT; 2) RSWE_EQU_S1RE_ALL_FAC_0000-0900_NEW_SAV. mat, which is saved time series data for the extracted parameters at about Z=-1 Re plane. 3) FAC mapping.rar, in which we compressed the data with a file name of rsw_xxxx_ZS1Re_T2SRPM.dat. These data are the parametters in the plane of about Z=-1 Re, which were mapped to the modeled inner boundary RPM (about 3 Re), along the magnetic field lines. All of these data include the following parameters: time, x, y, z, logrho, Vx, Vy, Vz, Bx, By, Bz, Pr, Jx, Jy, Jz, Edj Where, time is simulation time, which need to plus the start time to transfer them to universal time: time+14:04; (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; Pr is the plasma dynamic presure at the simulation point; (Jx, Jy,Jz) are the three components of plasma electric current at the simulation point in GSM coordinates; Edj is the electric field E dot electric current J, E dot J. 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 30 RE to –100 RE along the Sun-Earth line and from –50 RE to 50 RE in Y and Z directions, with 320×320×320 grid points and a minimum grid spacing of 0.15 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. Reference P. Colella, P. R. Woodward, The piecewise parabolic method (PPM) for gas-dynamical simulations. J. Comput. Phys. 54, 174– 201 (1984). Y. Q. Hu, X. C. Guo, C. Wang, On the ionospheric and reconnection potentials of the Earth: Results from global MHD simulations. J. Geophys. Res. 112, A07215 (2007). B. B. Tang, C. Wang, Large scale current systems developed from substorm onset: Global MHD results. SCIENCE CHINA Technological Sciences, 61(3): 389-396(2018). C. Wang et al. Magnetohydrodynamics (MHD) numerical simulations on the interaction of the solar wind with the magnetosphere: A review. Sci. China, Ser. D Earth Sci., 56(7), 1141–1157 (2013). X. Guo, C. Wang, Y. Hu,Global MHD simulation of the Kelvin-Helmholtz instability at the magnetopause for northward interplanetary magnetic field. J. Geophys. Res. 115, A10218 (2010). W. Li, C. Wang, B. Tang, X. Guo, D. Lin, Global features of Kelvin-Helmholtz waves at the magnetopause for northward interplanetary magnetic field. J. Geophys. Res. Space Physics. 118, 5118–5126 (2013).

{"references": ["P. Colella, P. R. Woodward, The piecewise parabolic method (PPM) for gas-dynamical simulations. J. Comput. Phys. 54, 174\u2013 201 (1984).", "Y. Q. Hu, X. C. Guo, C. Wang, On the ionospheric and reconnection potentials of the Earth: Results from global MHD simulations. J. Geophys. Res. 112, A07215 (2007).", "B. B. Tang, C. Wang, Large scale current systems developed from substorm onset: Global MHD results. SCIENCE CHINA Technological Sciences, 61(3): 389-396(2018).", "C. Wang et al. Magnetohydrodynamics (MHD) numerical simulations on the interaction of the solar wind with the magnetosphere: A review. Sci. China, Ser. D Earth Sci., 56(7), 1141\u20131157 (2013).", "X. Guo, C. Wang, Y. Hu,Global MHD simulation of the Kelvin-Helmholtz instability at the magnetopause for northward interplanetary magnetic field. J. Geophys. Res. 115, A10218 (2010).", "W. Li, C. Wang, B. Tang, X. Guo, D. Lin, Global features of Kelvin-Helmholtz waves at the magnetopause for northward interplanetary magnetic field. J. Geophys. Res. Space Physics. 118, 5118\u20135126 (2013)."]}