We conduct a global survey of magnetosonic waves and compute the associated bounce and drift averaged diffusion coefficients, taking into account co-located measurements of fpe/fce, to assess the role of magnetosonic waves in radiation belt dynamics, where fpe is the plasma frequency and fce is the electron gyrofrequency.. The average magnetosonic wave intensities increase with increasing geomagnetic activity and decreasing relative frequency with the majority of the wave power in the range fcp < f < 0.3fLHR during active conditions, where fcp is the proton gyrofrequency and fLHR is the lower hybrid resonance frequency. In the region 4.0 <= L* <= 5.0, the bounce and drift averaged energy diffusion rates due to magnetosonic waves never exceed those due to whistler mode chorus, suggesting that whistler mode chorus is the dominant mode for electron energisation to relativistic energies in this region. Further in, in the region 2.0 <= L* <= 3.5, the bounce and drift averaged pitch angle diffusion rates due to magnetosonic waves can exceed those due to plasmaspheric hiss and very low frequency (VLF) transmitters over energy-dependent ranges of intermediate pitch angles. We compute electron lifetimes by solving the 1D pitch angle diffusion equation including the effects of plasmaspheric hiss, VLF transmitters and magnetosonic waves. We find that magnetosonic waves can have a significant effect on electron loss timescales in the slot region reducing the loss timescales during active times from 5.6 to 1.5 days for 500 keV electrons at L* = 2.5 and from 140.4 days to 35.7 days for 1 MeV electrons at L* = 2.0. The research leading to these results has received funding from the Natural Environment Research Council (NERC) Highlight Topic grant NE/P01738X/1 (Rad-Sat) and the NERC grants NE/V00249X/1 (Sat-Risk) and NE/R016038/1.

The data files in this directory were used to create Figures 2-7 in the paper: Horne et al. (in press - 2018/7/18). Figure 1 of the paper was constructed using publically available data from other sources.

We present a concurrent series of 144 monthly reanalyses of Super Dual Auroral Radar Network (SuperDARN) plasma velocity measurements, using the method of data-interpolating Empirical Orthogonal Functions (EOFs). For each monthly reanalysis, the 5-minute median values of the northern polar region''s radar-measured line-of-sight Doppler plasma velocities are binned in an equal-area grid defined in quasi-dipole latitude and quasi-dipole magnetic local time (MLT). The grid cells each have an area of approximately 110,000km2, and the grid extends to 30 degrees colatitude. Within this spatial grid, the sparse binned data are infilled to provide a measurement at every spatial and temporal location via two different EOF analysis models: one tailored to instances of low data coverage, the other tailored to higher data coverage. These two models each comprise 144 monthly sets of orthogonal modes of variability (spatial and temporal patterns), along with the timestamps of each epoch, and the spatial coordinate information of all bin locations. A companion dataset determines which of the two models should be chosen in each location for each month, in order to ensure the best accuracy of the infill solution. We also provide the temporal mean of the data in each spatial bin, which is removed prior to the EOF analysis. Collectively, the reanalysis delivers the SuperDARN data in terms of cardinal north and east vector components (in the quasi-dipole coordinate frame), without its usual extreme sparseness, for studies of ionospheric electrodynamics for the period 1997.0 to 2009.0. Funding was provided by NERC Standard grant NE/N01099X/1, titled ''Thermospheric Heating Modes and Effects on Satellites'' (THeMES) and the NERC grant NE/V002732/1, titled ''Space Weather Instrumentation, Measurement, Modelling, and Risk: Thermosphere'' (SWIMMR-T).

This dataset contains data produced by two Gorgon Global magnetohydrodynamic (MHD) simulations with steady solar wind conditions interacting with the Earth''s magnetosphere, as utilised in the study of Desai et al. (2021b). Further description of the Gorgon MHD model can be found at Mejnertsen et al., (2016,2018), Eggington et al., (2020) and Desai et al., (2021a). The data was produced on the Imperial College High Performance Computing Service (doi: 10.14469/hpc/2232). Two MHD simulations are contained; one with northward Interplanetary Magnetic Field (IMF) conditions and one with southward (IMF) conditions. The northward IMF condition is run with a grid resolution of 0.25 earth radii (RE) and the southward IMF conditions is run three times for grid resolutions of 0.5, 0.25 and 0.125 RE. The MHD equations were solved in the magnetosphere on a regular 3-D Cartesian grid, covering a domain of dimensions (-20,100) 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 X-direction, 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 right-handed set. Output data is timestamped in seconds and is defined at the centre of the grid cells. The simulation data corresponding to each shock are stored in separate directories ''NorthwardX'' and ''SouthwardX'' where X is the grid resolution in RE of: 0.5 for the northward case and 0.5, 0.25 and 0.125 for the southward case. The data are stored in hdf5 format. The magnetospheric variables are stored in the files: ''Gorgon_[YYYYMMDD]_MS_params_[XXXXX]s.hdf5'' where XXXXX is the simulation time in seconds. The magnetospheric data includes the magnetic field, (''Bvec_c'') and Electric field, (''Evec''), after 2hrs of simulation. The data are 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 component in (i,j,k). Funding was provided by NERC Highlight grant to NE/P017347/1 (Rad-Sat).

This data set contains the ULF wave model output data required to produce the figures in the article: A. W. Degeling, I. J. Rae, C. E. J. Watt, Q. Q. Shi, R. Rankin and Q. G. Zong, "Control of ULF Wave Accessibility to the Inner Magnetosphere by the Convection of Plasma Density", J. Geophys. Res. (accepted Dec. 2017) doi:10.1002/2017JA024874 The dataset has a Matlab binary file format. It consists of a structure array "d" (with 325 elements). These elements correspond to the 2D parameter scan in driver frequency and elapsed time during plume development performed for this study. The elapsed time parameter has 25 elements, ranging 0 to 24 hours (i.e. 1 hour spacing), and the driver frequency parameter has 13 elements ranging from 1 to 7 mHz (with 0.5 mHz spacing). e.g. use "d = reshape(d,25,13);" to reshape the structure array into 2D with columns for the frequency scan and rows for the elapsed time scan. The Matlab function "make_PDP_figs.m" is used to read the data, perform the necessary post-processing operations and output the article figures. To produce all six figures, simply run the file without any input arguments.

These files contain the data from the figures in "A 30 year simulation of the outer electron radiation belt", S.A. Glauert, et al., Space Weather 2018. The paper describes a 30 year (1 January 1986 - 1 January 2016) reconstruction of the Earth''s electron radiation belt from L*=2 to L*=6.1 (approximately geostationary orbit), for energies ranging from 100 keV to 30 MeV at L*=6.1.

We present a reanalysis of SuperDARN plasma velocity measurements, using the method of data-interpolating Empirical Orthogonal Functions (EOFs). The northern polar region''s radar-measured line of sight Doppler velocities are binned in an equal-area grid (areas of approximately 110,000km2) in quasi-dipole latitude and quasi-dipole magnetic local time (MLT). Within this spatial grid, which extends to 30 degrees colatitude, the plasma velocity is given in terms of cardinal north and east vector components (in the quasi-dipole coordinate frame), with the median of every SuperDARN measurement in the spatial bin taken every 5 minutes. These sparse binned data are infilled to provide a measurement at every spatial and temporal location via EOF analysis, ultimately comprising a reanalysis spanning the month of February 2001. This resource provides a convenient method of using SuperDARN data without its usual extreme sparseness, for studies of ionospheric electrodynamics. The reanalysis is provided in sets of orthogonal modes of variability (spatial and temporal patterns), along with the timestamps of each epoch, and the spatial coordinate information of all bin locations. We also provide the temporal mean of the data in each spatial bin, which is removed prior to the EOF analysis. Funding was provided by NERC standard grants NE/N01099X/1 (THeMES) and NE/V002732/1 (SWIMMR-T).

Whistler mode chorus is an important magnetospheric emission, playing fundamental roles in the dynamics of the Earth''s outer radiation belt and the production of the Earth''s diffuse and pulsating aurora. In this study we extend our existing database of whistler mode chorus by including ~3 years of data from RBSP-A and RBSP-B and an additional ~6 years of data from THEMIS A, D, and E, greatly improving the statistics and coverage in the near-equatorial region (|MLAT|<18^o). We produce new global maps of whistler mode chorus as a function of spatial location and frequency. This work is reported in Meredith et al. [2020] and the data provided here enable reconstruction of all of the figures in the paper. The research leading to these results has received funding from the Natural Environment Research Council (NERC) Highlight Topic grant NE/P01738X/1 (Rad-Sat) and the NERC grant NE/R016038/1. Wen Li and Xiao-Chen Shen received funding from NASA grants NNX17AG07G and 80NSSC19K0845, NSF grant AGS-1847818, and the Alfred P. Sloan Research Fellowship FG-2018-10936. Jacob Bortnik received funding from NASA grants NNX14AI18G, and RBSP-ECT and EMFISIS funding provided by JHU/APL contracts 967399 and 921647 under NASA''s prime contract NAS5-01072.

This dataset contains two NetCDF files: Chorus_daa.nc (labelled from here as a) which contains the chorus pitch angle diffusion coefficients presented in Figure 1 of Reidy et al (2020) and Combined_daa.nc (labelled from here as b) containing the combined pitch angle diffusion coefficients which can be used to do the analysis presented in the remainder of the Reidy et al (2020) paper. These data sets include: a. A matrix containing the pitch angle diffusion coefficients for chorus waves at the angle of the loss cone for energies of 30, 100 and 300 keV between L*= 2-7.5, a full range of MLT sectors and for low (1 < Kp < 2), moderate (2 < Kp < 3) and high (4 < Kp < 7) geomagnetic activity levels. These were calculated from an average wave model presented in Meredith et al (2020) to capture the effect of wave-particle interactions in the BAS Radiation Belt Model (BAS-RBM). Also the arrays containing the energy, L*, MLT and Kp dependence are also included. b, A matrix containing the combined pitch angle diffusion coefficients for chorus, hiss and EMIC waves and coulomb collisions between alpha = 0.5deg -9.45deg, Energy = 28.18-2511.89 keV , L* = 4.25-7.25, MLT = 0-24 and 6 different activity levels. The arrays containing the pitch angle, energy, L*, MLT and Kp dependence are also included. Funding was provided by NERC Highlight Topic Grant NE/P01738X/1 and NERC National Capability grants NE/R016038/1 and NE/R016445/1

Radiation belts are hazardous regions found around several of the planets in our Solar System. They consist of very hot, electrically charged particles that are trapped in the magnetic field of the planet. At Saturn the most important way to heat these particles has for many years been thought to involve the particles drifting closer towards the planet. This paper builds on previous work on the emerging idea at Saturn that a different way to heat the particles is also possible where the heating is done by waves, in a similar way to what we find at the Earth. This work is reported in the paper "Acceleration of electrons by whistler-mode hiss waves at Saturn" by E.E. Woodfield et al., 2021. The data provided here enable reconstruction of all the figures in the paper. E.E.W., R.B.H., and S.A.G. were funded by STFC grant ST/S000496/1. R.B.H., S.A.G. and A.J.K. were funded by NERC grant NE/R016038/1 and R.B.H. and S.A.G. by NERC grant NE/R016445/1. J.D.M. and Y.Y.S. were supported by NASA grants NNX11AM36G and NNX16AI47G. University of Iowa (J.D.M.) was supported by NASA contract 1415150 with JPL. Y.Y.S. was supported by EC grant H2020 637302.