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57 results for “geomagnetic storm”
Data for: Ring Current Electron Precipitation During the 17 March 2013 Geomagnetic Storm: Underlying Mechanisms and Their Effect on the Atmosphere
<p>All data are included as MATLAB figure files, png files and MATLAB MAT files.</p><p>File precipitated_flux.mat contains a 4-D array of values of precipitated electron flux in [1/(s cm^2 keV)] for 289 time points from 16 March 2013 to 19 March 2013, with a 15 min time step; 100 values of energy in a range from 10 keV to 1 MeV, with a 10 keV step; on a spatial grid of 28 by 49 (P, R).</p><p>netCDF data can be opened with a variety of software tools, including Matlab, Origin or Python.</p>
Geomagnetic Storms - Classified - 1993 - 2025
<p>List of Geomagnetic Storms from 1993 to 2025 classified in main and recovery phase. The requirement for a storm to be identified is that it reaches an SMR index of -50 [nT]</p> <p>More information on the SMR ring current index can be found here : http://supermag.jhuapl.edu </p> <p>This version is based on the work published on Geophysical Research letters (GRL) "Plasma sheet Magnetic Flux Transport During Geomagnetic Storms" : https://agupubs.onlinelibrary.wiley.com/doi/epdf/10.1029/2024GL110839</p> <p>Columns are in order: index, storm number, minimum SMR, start time, end time, phase characterization, and duration.</p> <p>Comapred to version V2 the latest storms require manual verification</p>
The impact of 11 May 2024 super geomagnetic storm on the plasma distribution over the Indian equatorial/low latitude ionospheric region
<p>The file contains the data set and the software for the generation the plots used in the manuscript " The impact of 11 May 2024 super geomagnetic storm on the plasma distribution over the Indian equatorial/low latitude ionospheric region".</p>
Improving estimates of the ionosphere during geomagnetic storm conditions through assimilation of thermospheric mass density
<p>Swarm A/B/C neutral mass density normalized to 400 km to be assimilated by the CTIPe physics based model coupled with the thermosphere ionosphere data assimilation scheme (TIDA). Swarm-A is assimilated and B/C are used for validation purposes. The selected period is March 2015 that contains the St. Patrick's Day storm 2015 between 16-18 of that month.</p>
The Impact of the 8-10 March 2012 Geomagnetic Storm on Inner Zone Protons as Measured by Van Allen Probes
<p>Dataset for manuscript</p> <p>ctr.mat: test-particle count, Fig4</p> <p>psdgoes.mat, psdob0.mat: PSD from RD, Fig5, 6, 8</p> <p>mar2012-ts05-flux-777001.txt, mar2012-ts05-flux-777003.txt: test-particle trajectories, Fig7</p> <p> </p>
Data sets for distributed ionospheric L-band scintillation and TEC observations made in the American sector during the March 23-24, 2023 geomagnetic storm
<p>These data sets contain the scintillation measurements presented in the manuscript titled, "On the extraordinary L-band scintillation event observed in the American sector during the March 23-24, 2023 geomagnetic storm".</p> <p><br>The HDF5 files are organized by constellations and satellites. Each satellite includes the following parameters: Azimuth (AZIM), Elevation (ELEV), Number of Samples (NOS), Amplitude Scintillation Index (S4), 1-minute average SNR (SNR), relative Total Electron Content (PTEC), and Time of Week in seconds (S_TW)</p>
Dataset for "Three-dimensional modeling of the ground electric field in Fennoscandia during the Halloween geomagnetic storm", Marshalko et al. (2023), Space Weather
<p>Results of 3-D modeling of the ground electric field in Fennoscandia during the Halloween geomagnetic storm in 2003 (29-31 October).</p> <p>Electric_field_YYYYMMDDHHMMSS_YYYYMMDDHHMMSS.h5 files (in hdf5 format) contain horizontal electric field components Ex and Ey (in mV/km) corresponding to 6 h of data and latitude and longitude grids corresponding to Ex and Ey arrays. Ex and Ey are 2160x567x543 arrays (temporal resolution is 10 s, thus, 2160 time steps). Latitude and Longitude are 567x543 arrays. All values are in single-precision floating-point format. Electric field values were obtained with the use of the conductivity-based inducing source following Marshalko et al. (2023).</p> <p>Files Electric_field_CB_20031029000000_20031031235950.dat, Electric_field_MT_20031029000000_20031031235950.dat, and Electric_field_SECS_20031029000000_20031031235950.dat contain the ground electric field time series (in mV/km) modeled during the Halloween geomagnetic storm in 2003 (29-31 October) at IMAGE magnetometers' locations, Mäntsälä Finnish natural gas pipeline GIC recording point (MAN), and Point X located 0.5 degrees north of MAN. The files are in plain-text (column-based) format. Electric field values in Electric_field_CB_20031029000000_20031031235950.dat, Electric_field_MT_20031029000000_20031031235950.dat, and Electric_field_SECS_20031029000000_20031031235950.dat were obtained with the use of the conductivity-based inducing source, MT intersite impedance method, and Spherical Elementary Current Systems (SECS) based approach, correspondingly, following Marshalko et al. (2023).</p>
The SafeSpace magnetospheric models sample forecast for the 2015 St Patrick's geomagnetic storm
<p>This dataset presents the sample forecast of the magnetosphere models in the SafeSpace project, for the March 2015 St Patrick's storm. It is build from a synthetic solar wind forecast at L1 and corresponding Kp forecast. This forecast if fed in the SPM plasma density model, as well as in a VLF wave intensities model, yielding the dataset presented here.</p> <p>All files are in the CDF file format.</p> <ul> <li>The <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/GEOIDX_20150301.cdf">GEOIDX_20150301.cdf</a> file contains the synthetic solar wind and Kp ensemble forecast.</li> <li>The <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/Bw2_20150301.cdf">Bw2_20150301.cdf</a> file contains the corresponding VLF wave intensities.</li> <li>The <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/SPM_dens_20150301.cdf">SPM_dens_20150301.cdf</a> file contains the corresponding plasma densities.</li> <li>The <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/SafeSpace_RBSP_A_Nowcast.cdf">SafeSpace_RBSP_A_Nowcast.cdf</a> and <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/SafeSpace_RBSP_A_Nowcast.cdf">SafeSpace_RBSP_B_Nowcast.cdf</a> files contains the reconstructed electron fluxes along the RBSP spacecrafts for the whole March 2015 month, using data assimilation in the SafeSpace pipeline.</li> <li>The <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/SafeSpace_RBSP_A_Nowcast.cdf">SafeSpace_RBSP_A_Forecast.cdf</a> and <a href="https://zenodo.org/api/files/eb6a5ea3-366a-4830-bb14-71799a6f00cf/SafeSpace_RBSP_A_Nowcast.cdf">SafeSpace_RBSP_B_Nowcast.cdf</a> files contains a 4 days forecast of the electron fluxes along the RBSP spacecrafts for March 17th to March 20th, 2015.</li> </ul> <p>This dataset and the SafeSpace pipeline is described in details in the article by Brunet et al. "Improving the electron radiation belt nowcast and forecast using the SafeSpace data assimilation modelling pipeline", currently in review in AGU Space Weather.</p> <p> </p>
Solar wind plasma, magnetic field parameters and geomagnetic storm index SYM-H from 2000 to 2020
<p>SYM-H index is used to quantify the intensity of geomagnetic storm. Its temporal variation is related to the solar wind plasma and magnetic field parameters. This dataset offers time series of solar wind density, solar wind velocity and solar wind magnetic field, SYM-H index. The python and matlab code files for processing and plotting data are also included. </p>
Solar wind plasma, magnetic field parameters and geomagnetic storm index SYM-H from 2000 to 2020
Open the record for dataset details and reuse information.
A statistical study on the local time dependence of equatorial spread F (ESF) irregularities and their relation to low latitude Es layers under geomagnetic storms
<p>The data can be downloaded from this site about our work.</p>
Data repository for Lin et al. (2022) "Origin of Dawnside Subauroral Polarization Streams during Major Geomagnetic Storms"
This dataset contains the necessary data and plotting tools supporting the paper titled "Origin of Dawnside Subauroral Polarization Streams during Major Geomagnetic Storms", by Lin et al., 2022. The data includes solar wind/IMF data on 20 November 2003, DMSP F16 measurements of electron precipitation energy flux, electron density, cross track ion drift velocity, magnetic perturbation from 13:51 UT to 14:31 UT on 20 November 2003; MAGE model simulation results of EnFlux, Vhorz, and FAC along the same DMSP trajectory; MAGE simulation results of zonal ion drift, FAC, and magnetospheric equatorial plasma pressure at 06:30 UT and 18:30 UT; MAGE/RCM outputs of ring current pressure at 06 MLT and 18 MLT; RCM outputs of effective potential; CHIMP simulation results of test particle ions at 06:30 UT and 18:30 UT.
Ionosphere-Thermosphere Data Published in "Responses of the Thermosphere and Ionosphere System to Concurrent Solar Flares and Geomagnetic Storms"
<p>This dataset supports the Journal of Geophysical Research publication "Responses of the Thermosphere and Ionosphere System to Concurrent Solar Flares and Geomagnetic Storms" by Qian et al., 2019. The data files are selected output and related analyses from the thermosphere-ionosphere-electrodynamics general circulation model (TIEGCM). The format of the data files are either IDL save files or NetCDF files or ASCII.</p>
TIEGCM simulations associated with the February 2016 geomagnetic storm
<p>These are simulation results from the thermosphere-ionosphere-electrodynamics GCM (TIEGCM) described in the manuscript "Importance of the lower atmospheric forcing and magnetosphere-ionosphere coupling in simulating neutral density during the February 2016 geomagnetic storm" by Maute et al. submitted to Frontiers. The study is focused on examining the effect on the neutral density of different lower boundary forcing and different high latitude forcing methods. The simulations are compared to Swarm-C neutral density along the satellite orbit.</p> <p>There are three different TIEGCM simulations which output is provided and vary by their forcing</p> <p>1. lower atmospheric forcing by WACCM-X/SD perturbations and mean, high latitude foricng via field-aligned current (labeled WacXBP_FAC) </p> <p>2. lower atmospheric forcing by climatological Global Scale Wave Model GSWM) (perturbations) and climatological background, high latitude forcing via field-aligned current (labeled Climate_FAC) </p> <p>3. lower atmospheric forcing by WACCM-X/SD perturbations and mean, high latitude forcing via Weimer empirical model (labeled WacXBP_Weimer) </p> <p>There are two additional simulations for which the neutral density is provided</p> <p>4. lower atmospheric forcing by WACCM-X/SD perturbations and climatological background, high latitude foricng via field-aligned current (labeled WacXP_Bclimate_FAC)</p> <p>5. lower atmospheric forcing by WACCM-X/SD symmetric perturbations (with respect to geographic latitude) and mean, high latitude foricng via field-aligned current (labeled WacXBPsym_FAC)</p>
Data for paper titled "Penetrating electric field during the Nov 4 2021 Geomagnetic Storm"
<p>The data is part of publication for a paper titled "Penetrating electric field during the Nov 4 2021 Geomagnetic Storm" to be submitted to the JGR Space Physics. The data contains simulation from the NCAR MAGE model of the Nov 4, 2021 Geomagnetic storm. We used the simulation to study the penetrating electric field, which affects the low latitude region ionosphere.</p>
Data for "Low- and mid-latitude ionospheric response to the 2013 St Patrick's Day geomagnetic storm in the American Sector: GITM simulation"
<p>The dataset stores the GITM simulation results for the study "Low- and mid-latitude ionospheric response to the 2013 St Patrick's Day geomagnetic storm in the American Sector: GITM simulation"</p>
Data for "Assessment of using field-aligned currents to drive the Global Ionosphere Thermosphere Model: A case study for the 2013 St Patrick's Day geomagnetic storm"
GITM Simulation results for the paper "Assessment of using field-aligned currents to drive the Global Ionosphere Thermosphere Model: A case study for the 2013 St Patrick's Day geomagnetic storm"
Multi-process driven unusually large equatorial perturbation electric fields during the April 2023 geomagnetic storm
<p>Dataset of the article entitled "Multi-process driven unusually large equatorial perturbation electric fields during the April 2023 geomagnetic storm" submitted to <a href="https://www.frontiersin.org/journals/astronomy-and-space-sciences">Frontiers in Astronomy and Space Sciences</a>. The data include the outputs of simulations from the four empirical vertical drift models used in the article: Fejer and Scherliess (1997), Scherliess and Fejer (1999), Kelley and Retterer (2008), and Manoj and Maus (2012).</p>
Large-Scale Traveling Ionospheric Disturbances over the European sector during the geomagnetic storm on March 23-24, 2023: energy deposition in the source regions and the propagation characteristics
<p>IMAGE 2D Ionospheric Equivalent Currents for 23 and 24 March 2023 (https://space.fmi.fi/image/). </p> <p><em>We thank the institutes who maintain the IMAGE Magnetometer Array (<a href="https://space.fmi.fi/image/">https://space.fmi.fi/image/</a>): Tromsø Geophysical Observatory of UiT the Arctic University of Norway (Norway), Finnish Meteorological Institute (Finland), Institute of Geophysics Polish Academy of Sciences (Poland), GFZ German Research Centre for Geosciences (Germany), Geological Survey of Sweden (Sweden), Swedish Institute of Space Physics (Sweden), Sodankylä Geophysical Observatory of the University of Oulu (Finland), DTU Technical University of Denmark (Denmark), and Science Institute of the University of Iceland (Iceland). The provisioning of data from AAL, GOT, HAS, NRA, VXJ, FKP, ROE, BFE, BOR, HOV, SCO, KUL, and NAQ is supported by the ESA contracts number 4000128139/19/D/CT as well as 4000138064/22/D/KS. The authors would like to thank Dr. Liisa Juusola for providing the IMAGE 2D Ionospheric Equivalent Currents data.</em></p>
BAS-PRO Model Solution for "Modeling Field Line Curvature Scattering Loss of 1 to 10MeV Protons during Geomagnetic Storms"
<p>The file <em>ModelingFLC_BASPRO_solution.zip</em> is a BAS-PRO model solution output archived as a zip file. After extracting the zip file, the solution will be spread across multiple plaintext files. The solution is a grid of proton phase space density multiplied by proton rest mass cubed, f, with units km-6 s3. f is specified in terms of the first, second and third adiabatic invariants μ, K and L as well as time.</p> <p>The solution files can be loaded using the BAS-PRO plotting library, available at <a href="https://github.com/atmosalex/BAS-PRO_plotting" target="_blank" rel="noopener">https://github.com/atmosalex/BAS-PRO_plotting</a>. A copy of the BAS-PRO plotting library has also been bundled with this dataset (<em>BAS-PRO_plotting-main.zip</em>) to prevent potential compatibility issues arising from future updates to the online repository. It is recommend to follow the steps in the "Getting started" section of the plotting library README.md file, as this will result in plots of the solution, and will also convert the plaintext solution files into a single file in binary .cdf format which allows for faster loading.</p> <p>The plaintext solution included in this dataset is made up of two sets of files which correspond to different grid resolutions:</p> <ul> <li>Files ending in 'dyn.txt' are 'dynamic output' files, containing the sampled time evolution of f throughout the simulation period. The dynamic output grid is lower resolution than the original BAS-PRO simulation grid in order to save disk space. These files are useful for producing plots.</li> <li>Files <strong>not</strong> ending in 'dyn.txt' are 'simulation grid' files, containing f at the final simulation epoch only, at the original simulation grid resolution. These files are useful for loading into BAS-PRO as an initial condition, or for plotting the final epoch at higher resolution.</li> </ul> <p>The coordinate range of the 'simulation grid' ('dynamic output') files is as follows:</p> <ul> <li>log10(μ/ (1MeV/G)) ranges from: 0.029384425 to 4.2519649 (0.17108176 to 4.1952860)</li> <li>K ranges from: 0 to 5.729029 (0 to 5.729029) in units G0.5 RE</li> <li>L ranges from: 1.13 to 4.0 (1.13 to 4.0)</li> <li>time ranges from 1388534400 to 1517443200, given in terms of seconds passed since January 1, 1970 UTC, and this time range is from January 1, 2014 to February 1, 2018.</li> </ul> <p>The following table gives a description of each file included:</p> <table> <tbody> <tr> <td><em>axis_mu.txt</em></td> <td>first dimension axis: a list of log10(μ/ (1MeV/G)) for the μ of each simulation grid point</td> </tr> <tr> <td><em>axis_K.txt</em></td> <td>second dimension axis: a list of K for each simulation grid point, with units G0.5 RE</td> </tr> <tr> <td><em>axis_L.txt</em></td> <td>third dimension axis: a list of L at each simulation grid point</td> </tr> <tr> <td><em>axis_t.txt</em></td> <td>time axis: a list of each simulation epoch, showing the history of timestepping</td> </tr> <tr> <td><em>map_iK-aeq.txt</em></td> <td>a 2D grid of equatorial pitch angle (degrees) corresponding to each L (rows) and K (columns) listed in the corresponding simulation axis files. A fill value of -1 is used to signify coordinates outside the trapping region.</td> </tr> <tr> <td><em>iK-0001_2D_en.txt</em></td> <td>a 2D grid of energy, with units of megaelectron volt, at each μ (rows) and L (columns) coordinate defined in the simulation axis files, at the K corresponding to the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K.txt</em> file. </td> </tr> <tr> <td><em>iK-0001_2D_f.txt</em></td> <td>a 2D grid of f, with units km-6 s3, at each μ (rows) and L (columns) coordinate defined in the simulation axis files, at the K corresponding to the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K.txt</em> file.</td> </tr> <tr> <td><em>iK-0001_axis_aeq.txt</em></td> <td>a list of equatorial pitch angle (degrees) at each L in the <em>axis_L.txt</em> file, at the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K.txt</em> file. A fill value of -1 is used to signify coordinates outside the trapping region.</td> </tr> <tr> <td><em>...<br></em></td> <td>...</td> </tr> <tr> <td><em>axis_mu_dyn.txt</em></td> <td>first dimension axis: a list of log10(μ/ (1MeV/G)) for the μ of each grid point in the dynamic output of the model</td> </tr> <tr> <td><em>axis_K_dyn.txt</em></td> <td>second dimension axis: a list of K for each grid point in the dynamic output of the model, with units G0.5 RE</td> </tr> <tr> <td><em>axis_L_dyn.txt</em></td> <td>third dimension axis: a list of L at each grid point in the dynamic output of the model</td> </tr> <tr> <td><em>axis_t_dyn.txt</em></td> <td>time axis: a list of each dynamic output epoch</td> </tr> <tr> <td><em>map_iK-aeq_dyn.txt</em></td> <td>a 2D grid of equatorial pitch angle (degrees) corresponding to each L (rows) and K (columns) listed in the corresponding axis files for the dynamic output. A fill value of -1 is used to signify coordinates outside the trapping region.</td> </tr> <tr> <td><em>iK-0001_2D_en_dyn.txt</em></td> <td>a 2D grid of energy, with units of megaelectron volt, at each μ (rows) and L (columns) coordinate defined in the dynamic output axis files, at the K corresponding to the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K_dyn.txt</em> file. </td> </tr> <tr> <td><em>iK-0001_2D_f_dyn.txt</em></td> <td>a 2D grid of f, with units km-6 s3, at each μ (rows) and L (columns) coordinate defined in the dynamic output axis files, at the K corresponding to the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K_dyn.txt</em> file. The 2D grid is output for every timestep and appended to the file, so subsequent 2D grids correspond to subsequent timesteps at the same K.</td> </tr> <tr> <td><em>iK-0001_axis_aeq_dyn.txt</em></td> <td>a list of equatorial pitch angle (degrees) at each L in the <em>axis_L_dyn.txt</em> file, at the K index listed in the file name. For example, iK-0001... means the first K on the 3D model grid, corresponding to the first value of K listed in the <em>axis_K_dyn.txt</em> file. A fill value of -1 is used to signify coordinates outside the trapping region.</td> </tr> <tr> <td><em>...</em></td> <td>...</td> </tr> <tr> <td><em>progress.txt</em></td> <td>a file used by the BAS-PRO model to continue from partially complete simulations. It contains three values (one per line): epoch of the simulation start time; total simulation time elapsed (seconds); and a mode select value (1 for dynamic, 0 for steady state)</td> </tr> <tr> <td><em>resume.config</em></td> <td>a backup of the original configuration options used to execute the BAS-PRO simulation, used only by the model</td> </tr> </tbody> </table>
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