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This dataset contains outputs generated using the Gorgon Magnetohydrodynamic (MHD) code, for simulations of the magnetosphereionosphere system during impact by a series of interplanetary shocks with different solar wind conditions and dipole magnetic field orientations. The MHD equations were solved in the magnetosphere on a regular 3D cartesian grid of resolution 0.25 RE (Earth radii), covering a domain of dimensions (30,90) RE in X, (40,40) RE in Y and (40,40) RE in Z with an inner boundary at 3 RE. In this coordinate system the Sun lies in the negative Xdirection, the Z axis is aligned to the dipole in the 0 degree tilt case (where positive tilt points the north magnetic pole towards the Sun), and Y completes the righthanded set. The ionospheric variables were calculated on a separate 2D spherical grid of dimensions 128x256 in latitude and longitude (with the north pole at 90 degrees latitude and the Sun at 180 degrees longitude), coupled to the magnetospheric domain at the inner boundary. 5 different shocks were simulated in total, with the following solar wind jump conditions injected at the sunward edge at 7200s simulation time: Shocks 14: n = 5 /cm^3 > 10 /cm^3 (number density) v = 400 km/s > 600 km/s (velocity) T = 5 eV > 417 eV (temperature) B = 2 nT > 4 nT (interplanetary magnetic field) Shock 5: n = 5 /cm^3 > 20 /cm^3 (number density) v = 400 km/s > 1000 km/s (velocity) T = 5 eV > 1250 eV (temperature) B = 2 nT > 4 nT (interplanetary magnetic field) Shocks 1, 3 and 5 had an interplanetary magnetic field (IMF) clock angle of 180 degrees, i.e. B = Bz = 2 nT, whereas Shocks 2 and 3 had IMF clock angles of 135 degrees and 90 degrees, respectively. In addition, Shocks 1, 2, 3 and 5 had zero dipole tilt, whereas Shock 4 had a tilt angle of 30 degrees. These simulations employed zero electrical resistivity. The simulations of Shocks 1, 3 and 5 were then repeated utilising an explicit resistivity eta with value of eta/mu_0 = 5e10 m^2/s. The full set of 8 simulations are labelled 'Shock1', 'Shock2', 'Shock3', 'Shock4', 'Shock5' for the zero resistivity runs and 'Shock1_res', 'Shock3_res' and 'Shock5_res' for those with explicit resistivity. Output grid data are timestamped in seconds and are defined at the centre of the grid cells, stored as .hdf5 files for each timestep. Output timeseries data are for a single variable over a simulation time range, stored in .csv files. The simulation data corresponding to each shock are stored in separate directories, according to the simulation labels listed above. The magnetospheric variables are stored in the files 'Gorgon_[YYYYMMDD]_[RUN]_MS_params_[XXXX]s.hdf5' where RUN is the simulation label and XXXX is the simulation time in seconds. The magnetospheric data are in SI units and include the magnetic field vector ('Bvec_c'), electric current density vector ('jvec') and ion thermal pressure ('P') for multiple timesteps following initialisation at 7200s of simulation time. The dataset for each magnetospheric variable is of shape (480,320,320,3) for vectors and (480,320,320) for scalars, where the first 3 dimensions are the grid indices in (X,Y,Z) indexed from negative to positive, and the final dimension is the cartesian vector components in (i,j,k). Similarly, the ionospheric data are stored as 'Gorgon_[YYYYMMDD]_[RUN]_IS_params_[XXXX]s.hdf5', containing the fieldaligned current density ('FAC') in SI units for multiple timesteps following initialisation at 7200s of simulation time. The dataset for each ionospheric variable is of shape (130, 256) where the first dimension is the grid index in colatitude, indexed from the north towards the south (i.e. 0 to 180 degrees), and the second dimension is the grid index in longitude, indexed from midnight towards noon via dawn (i.e. 0 to 360 degrees). Finally, the timeseries data are stored as 'Gorgon_[YYYYMMDD]_[RUN]_[XXX].csv' where 'X' is the simulation label and 'XXX' is the timeseries variable. These include the subsolar magnetopause standoff distance 'RMP' in RE, and the North (and South) polar cap flux content 'FPC' in Wb*RE^2; in each case the first column contains the simulation time in seconds, with the variables in the second (and third) column(s). NE/P017142/1

This dataset contains data outputs generated using the Gorgon Magnetohydrodynamic (MHD) code, for simulations of the steadystate magnetosphereionosphere system during southward interplanetary magnetic field (IMF) with dipole tilt angles from 090 degrees. This data were collected as part of the NERC project Space Weather Impacts on Groundbased Systems (SWIGS). The MHD equations were solved in the magnetosphere on a regular 3D cartesian grid of resolution 0.5 RE (Earth radii), covering a domain of dimensions (30,90) RE in X, (40,40) RE in Y and (40,40) RE in Z with an inner boundary at 4 RE. In this coordinate system the Sun lies in the negative Xdirection, the Z axis is aligned to the dipole in the 0 degree tilt case (where positive tilt points the north magnetic pole towards the Sun), and Y completes the righthanded set. The ionospheric variables were calculated on a separate 2D spherical grid of dimensions 66x128 in latitude and longitude (with the north pole at 90 degrees latitude and the sun at 180 degrees longitude), coupled to the magnetospheric domain at the inner boundary. Output data is timestamped in seconds and is defined at the centre of the grid cells. The simulation data corresponding to each dipole tilt are stored in separate directories 'XXdeg', e.g. in '00deg' for a 0 degree tilt angle. The data are stored in hdf5 format. The magnetospheric variables are stored in the files 'Gorgon_[YYYYMMDD]_[XX]deg_MS_params_[XXXXX]s.hdf5' where XX is the tilt angle in degrees and XXXXX is the simulation time in seconds. The magnetospheric data includes the magnetic field ('Bvec_c'), plasma bulk velocity ('vvec') and electric current density ('jvec') after 4h of simulation, as well as the magnetic field and velocity in 5 minute intervals for the preceding 30 minutes. The dataset for each magnetospheric variable is of shape (240,160,160,3) where the first 3 dimensions are the grid indices in (X,Y,Z) indexed from negative to positive, and the final dimension is the cartesian vector components in (i,j,k). Similarly, the ionospheric data are stored as 'Gorgon_[YYYYMMDD]_[XX]deg_IS_params_[XXXXX]s.hdf5', containing the fieldaligned current ('FAC') and electric potential ('phi') after 4h of simulation, as well as the potential in 5 minute intervals for the preceding 30 minutes. The dataset for each ionospheric variable is of shape (66, 128) where the first dimension is the grid index in colatitude, indexed from the north towards the south (i.e. 0 to 180 degrees), and the second dimension is the grid index in longitude, indexed from midnight towards noon via dawn (i.e. 0 to 360 degrees).

This dataset contains Global Precipitation Measurements (GPM) Integrated MultisatellitE Retrievals (IMERG) v6. The precipitation estimates from the various precipitationrelevant satellite passive microwave (PMW) sensors comprising the GPM constellation are computed using the 2017 version of the Goddard Profiling Algorithm (GPROF2017), then gridded, intercalibrated to the GPM Combined Ku RadarRadiometer Algorithm (CORRA) product, and merged into halfhourly 0.1°x0.1° (roughly 10x10 km) fields. Level 3 data are averaged global gridded products, screened for bad data points The Global Precipitation Measurement (GPM) mission is an international network of satellites that provide the nextgeneration global observations of rain and snow.