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57 results for “geomagnetic storm”
Simulation Data from STORMI and SWMF Models for the May 2024 Geomagnetic Storm Analysis
<p>Simulation Data from STORMI and SWMF Models for the May 2024 Geomagnetic Storm Analysis.</p>
Event list for intense geoelectric fields identified from EarthScope sites during geomagnetic storms
<p>This data set contains properties of intense geoelectric field events identified from 24 EarthScope sites during geomagnetic storms with Dst minima of less than - 100 nT from 2006 to 2019. Columns are the name of EarthScope site that detected the event (station), geoelectric field component in which the event was detected (Ecomp), the component value of geoelectric fields (Edata), geoelectric field peak prominence, geoelectric field peak width, dBx/dt at the time of the geoelectric field peak, dBy/dt at the time of geoelectric field peak, date and time when the intense geoelectric field peak was observed, geographical latitude of the EarthScope site (glat), geographical longitude of the EarthScope site (glon), geomagnetic latitude of the EarthScope site (mlat), geomagnetic longitude of the EarthScope site (mlon), and magnetic local time of the EarthScope site when the event was detected (mlt).</p>
Geomagnetic field variations recorded at EMMA during the November 2021 geomagnetic storm
<p>This data set contains daily files of 1-sec geomagnetic field variations from 22 stations of the European quasi-Meridional Magnetometer Array (EMMA) collected in the interval 29 October - 8 November 2021. The stations available are AQU, BEL, BRZ, HAN, HLP, IVA, KEV, KIL, LOP, MAS, MUO, NUR, OUJ, PEL, PPN, RAN, RNC, SOD, SUW, TAR, THY, ZAG.</p> <p>The header lines in each file indicate the station name, geodetic coordinates, and the reference frame (HDZ or XYZ). Data are expressed in nanoTesla. Missing data are represented by 99999.99.</p>
Citizen Science Reports on Aurora Sighting and Technological Disruptions during the 10 May 2024 Geomagnetic Storm – ARCTICS Survey
<div> <div> <div> <div> <p>The geomagnetic storm that began on 10 May 2024 provided stunning auroral displays observed worldwide. This dataset contains data collected via an online survey designed and distributed by the "Auroral Research Coordination – Towards Internationalised Citizen Science" (ARCTICS) collaboration sponsored by the International Space Science Institute (ISSI) in Bern, Switzerland (see https://collab.issibern.ch/arctics/). A total of 696 observers from over 30 countries filled in the survey and reported on aurora sightings and experienced disruptions in technological systems during the superstorm.</p> <p>The dataset consists of two data files in the CSV format and a text file providing a detailed description of the data. The collected data have been anonymised and pre-processed to obtain a homogeneous data set.</p> <p>Dataset associated with the <span>egusphere-2024-2174 preprint by Grandin et al. ("<span>The geomagnetic superstorm of 10 May 2024: Citizen science observations</span>"), submitted to Geoscience Communication.</span></p> </div> </div> </div> </div>
Modeling the Depletion and Recovery of the Outer Radiation Belt During a Geomagnetic Storm: Combined MHD and Test Particle Simulations
<p>Data associated with JGR: Space Physics paper, "Modeling the Depletion and Recovery of the Outer Radiation Belt During a Geomagnetic Storm: Combined MHD and Test Particle Simulations".</p>
Lower ionospheric disturbances due to geomagnetic storms of March & April 2023: inferred from VLF navigational signals and numerical simulations
<p>This is VLF data used in the research paper as per title</p>
Data and Code for "Study of Solar Wind and Interplanetary Magnetic Field Features Associated with Geomagnetic Storms: The Cross Wavelet Approach"
<p>These files are the supplementary information, including dataset, codes and plots for the research work entitled "Study of Solar Wind and Interplanetary Magnetic Field Features Associated with Geomagnetic Storms: The Cross Wavelet Approach".</p>
MHD-test particles simulations of moderate CME and CIR-driven geomagnetic storms at solar minimum
<p>field100x180.t0.data contains results from GAMERA code to produce Figure 3. Variables, grids, and units are described in the file. </p> <p><a href="https://zenodo.org/api/files/caa1f0ae-8f00-45f8-90bc-d639a9c39e97/May2019_kp3_2000_both-Lstar_PSD.h5">May2019_kp3_2000_both-Lstar_PSD.h5</a> contains simulated 2000 MeV/G electron phase space density during the May event on a radial and time grid and is used to plot Figure 5. Its radial profile at 05/14 10UT is used in Figure 7a. The unit of PSD is (c/MeV/cm)^3.</p> <p><a href="https://zenodo.org/api/files/caa1f0ae-8f00-45f8-90bc-d639a9c39e97/May2019_kp3_2000_both-Lstar_PSD.h5">May2019_kp3_5000_both-Lstar_PSD.h5</a> contains simulated 5000 MeV/G electron phase space density during the May event on a radial and time grid. Its radial profile at 05/14 10UT is used in Figure 7b. The unit of PSD is (c/MeV/cm)^3.</p> <p><a href="https://zenodo.org/api/files/caa1f0ae-8f00-45f8-90bc-d639a9c39e97/Sept2019_Gamera_2000_both-Lstar_PSD.h5">Sept2019_Gamera_2000_both-Lstar_PSD.h5</a> contains simulated 2000 MeV/G electron phase space density during the May event on a radial and time grid and is used to plot Figure 6. Its radial profile at 09/03 00UT is used in Figure 7c. The unit of PSD is (c/MeV/cm)^3.</p> <p><a href="https://zenodo.org/api/files/caa1f0ae-8f00-45f8-90bc-d639a9c39e97/Sept2019_Gamera_2000_both-Lstar_PSD.h5">Sept2019_Gamera_5000_both-Lstar_PSD.h5</a> contains simulated 5000 MeV/G electron phase space density during the May event on a radial and time grid. Its radial profile at 09/03 00UT is used in Figure 7d. The unit of PSD is (c/MeV/cm)^3.</p>
List of geomagnetic storms for the period September 2012 - July, 2019
<p>The following dataset includes the epoch times and corresponding Sym-H minima for the 144 geomagnetic storms identified between September 2012 and July 2019. </p>
The growth of ring current/SYM-H under northward IMF Bz conditions present during the 21-22 January 2005 geomagnetic storm
<p>Database for "The growth of ring current/SYM-H under northward IMF $B_z$ conditions present during the 21-22 January 2005 geomagnetic storm". This collection of the Solar wind, Interplanetary magnetic field, and other satellite data are used in the study to determine the causes of the sustained peak of the ring current indices under unfavorable conditions. The paper is submitted to the Space Weather Paper ( MS# 2023SW003489).</p>
Large Scale Travelling Ionospheric Disturbances during geomagnetic storms of 17 March and 23 June 2015 in the Australian region
<p>This repository contains compilation of data in .mat (Matlab) format used in this work.</p> <p>Raw foF2 data e.g., in Data15-20Mar2015.mat has the format [Month, Day, Hour, Minute, foF2]. These are provided for each site of the network under the URSI station code. </p> <p>Residuals data e.g., in Residuals_15_20Mar2015.mat contains fof2 perturbations after removing daily trends and outliers and have been upscaled to 1 minute intervals. Note: y11 - Brisbane, y22 - Canberra, y33 - Camden, y44 - Hobart, y55 - Norfolk, y66 - Townsville, y77 - Darwin, and time is in seconds.</p> <p>Dst and AE data (AE_DST_struct_files.mat) is contained in a structure array with Dst in field 1 and AE in field 2. </p> <p>IMF Bz data (IMF_Bz_LSTID_Paper.mat) has the format [Year DOY Hour Value].</p> <p> </p>
TEC obtained from Madrigal for 'typical' Geomagnetic storms over the US (2000-2018)
<p>Contains Quiet day and storm day TEC gridded on the basis of dip and declination over the United States.</p> <p>TEC data are obtained from the Madrigal database (<a href="http://millstonehill.haystack.mit.edu/">http://millstonehill.haystack.mit.edu/</a>)</p> <p>Quiet days are in the same month as the storm days. These days are obtained from the kyoto database</p> <p>Files named as Storm/Quiet_ID_Sector.h5</p> <p>The storm ID and sector information are in a paper submitted to JGR-Space Physics.. </p>
Investigation of a neutral 'tongue' observed by GOLD during the geomagnetic storm on May 11, 2019
<p>This dataset include all the data needed for the figures in the main text of JGR paper "Investigation of a neutral 'tongue' observed by GOLD during the geomagnetic storm on May 11, 2019". It include the percentage difference of TIE-GCM simulated column density ratio of O to N2 (O/N2) between DOY 128 and 130, between DOY 128 and 131, and the absolute difference of horizontal advection of O and N2 at pressure level -1.375 between DOY 128 and 131 from 0:10 to 6:10 UT, and the absolute difference of zonal and meridional wind at pressure level -1.375 between DOY 128 and 131 from 0:10 to 6:10</p>
Coupled Thermosphere-Ionosphere Tongue-like Structure During the Recovery Phase of the Geomagnetic Storm on May 12, 2021
<p>The file named 'Indices' includes Kp, F10.7p, By and Bz indices, AE and Dst indices, which are used to plot Figure 1. The file named 'GOLD_131', 'GOLD_132' and 'GOLD_133' include the parameters of O/N2 and temperature from GOLD observations, which are used to plot for Figures 2 and S1. The file named 'GPS_131', 'GPS_132' and 'GPS_133' include the parameters of TEC from GPS observations, which are used to plot for Figures 4 and S2. The file named 'TIEGCM_131' and 'TIEGCM_133' includes O/N2, Temperature, horizontal winds, TEC and diagnostic analysis terms of O+ density from the TIEGCM simulations on DOY 131 and 133 in 2021, which are used to plot for Figures 3 and 4, Movie S1 and S2.</p>
Solar wind parameters and geomagnetic indices for severe (SYM-H < -100nT) geomagnetic storms over two solar cycles
<p><em><strong>Severe storms data set (1996-2022)</strong></em></p> <p><em>Lotz, Grant, Davel (2024).</em></p> <p><strong>Changes from previous version:</strong></p> <ul> <li>Previous version had errors in calculation of `HER_eh` and `ABK_eh`. The mistake is corrected in this version.</li> <li>This version includes storms from 1996-2022. Previous version had 1996-2019.</li> </ul> <p>This data set is curated from 1-minute time resolution OMNI [4] and INTERMAGNET [7] data, spanning the period 1996 - 2022.</p> <p>It consists of all geomagnetic storms that reached minimum SYM-H (Symmetric-H index) of < -100 nT. We classified these as "severe" storms. There are 115 such events in the period 1996 - 2018. No severe storms detected between 2007-2010 or in 2019. Each file in the set contains the events in that year (YYYY) in the format "severe_YYYY.pickle". The geomagnetic storms are identified by the procedure described in [1], with thresholds -100 nT and -20 nT (see [1] for further detail).</p> <p>The data sets are Pandas "dataframes" [2], saved in the Python "pickle" format [3]. Each dataframe contains 23 variables, listed in the table below, with their description and unit.</p> <p>Fourteen of the parameters are solar wind plasma and magnetic field parameters from the High Resolution OMNI data set [4].</p> <p>There are 7 geomagnetic variables:</p> <ul> <li>one is the global Sym-H index,</li> <li>four are H-component geomagnetic observations from Hermanus, South Africa (HER: 34.4 S, 19.22 E) and Abisko, Sweden (ABK: 68.35 N, 18.82 E) and their time derivatives</li> <li>two are the e_h index [5] calculated at HER and ABK</li> </ul> <p>Finally, we list the time shift applied to each data point to shift to the bow shock nose (described for OMNI at [6]) and a string identifier for each geomagnetic storm.</p> <p> </p> <table> <tbody> <tr> <td><strong>#</strong></td> <td><strong>Name</strong></td> <td><strong>Description</strong></td> <td><strong>Unit</strong></td> </tr> <tr> <td>1</td> <td>time_shift</td> <td> <p>Time shift applied to shift solar wind parameters to bow shock</p> </td> <td>s</td> </tr> <tr> <td>2</td> <td>Bt</td> <td>Magnitude of interplanetary magnetic field (IMF)</td> <td>nT</td> </tr> <tr> <td>3</td> <td>Bx</td> <td>X-component of IMF</td> <td>nT</td> </tr> <tr> <td>4</td> <td>By_GSE</td> <td>Y-component of IMF (GSE coordinates)</td> <td>nT</td> </tr> <tr> <td>5</td> <td>Bz_GSE</td> <td>Z-component of IMF (GSE coordinates)</td> <td>nT</td> </tr> <tr> <td>6</td> <td>By_GSM</td> <td>Y-component of IMF (GSM coordinates)</td> <td>nT</td> </tr> <tr> <td>7</td> <td>Bz_GSM</td> <td>Z-component of IMF (GSM coordinates)</td> <td>nT</td> </tr> <tr> <td>8</td> <td>Vsw</td> <td>Bulk solar wind speed</td> <td>km/s</td> </tr> <tr> <td>9</td> <td>Vx</td> <td>X-component of solar wind</td> <td>km/s</td> </tr> <tr> <td>10</td> <td>Vy</td> <td>Y-component of solar wind</td> <td>km/s</td> </tr> <tr> <td>11</td> <td>Vz</td> <td>Z-component of solar wind</td> <td>km/s</td> </tr> <tr> <td>12</td> <td>Np</td> <td>Proton number density in solar wind plasma</td> <td>#/cc</td> </tr> <tr> <td>13</td> <td>Temp</td> <td>Temperature of solar wind plasma</td> <td>K</td> </tr> <tr> <td>14</td> <td>Pd</td> <td>Dynamic or flow pressure of solar wind plasma</td> <td>nPa</td> </tr> <tr> <td>15</td> <td>E_field</td> <td>Solar wind electric field</td> <td>mV/km</td> </tr> <tr> <td>16</td> <td>SymH</td> <td>Symmetric-H index of the geomagnetic field</td> <td>nT</td> </tr> <tr> <td>17</td> <td>HER_H</td> <td>H-component of the geomagnetic field at Hermanus</td> <td>nT</td> </tr> <tr> <td>18</td> <td>HER_dHdt</td> <td>Time derivative of HER_H</td> <td>nT/min</td> </tr> <tr> <td>19</td> <td>HER_eh</td> <td>e_h index at HER</td> <td>nT/min</td> </tr> <tr> <td>20</td> <td>ABK_H</td> <td>H-component of the geomagnetic field at Abisko</td> <td>nT</td> </tr> <tr> <td>21</td> <td>ABK_dHdt</td> <td>Time derivative of ABK_H</td> <td>nT/min</td> </tr> <tr> <td>22</td> <td>ABK_eh</td> <td>e_h index at ABK</td> <td>nT/min</td> </tr> <tr> <td>23</td> <td>Storm_ID</td> <td>String identifier of the geomagnetic storm</td> <td>-</td> </tr> </tbody> </table> <p> </p> <p><em><strong>References</strong></em></p> <ol> <li>Lotz, S. I., & Danskin, D. W. (2017). <em>Space Weather</em>, 15, 1347– 1356. <a href="https://doi.org/10.1002/2017SW001662">https://doi.org/10.1002/2017SW001662</a></li> <li><a href="https://omniweb.gsfc.nasa.gov/ow_min.html">https://omniweb.gsfc.nasa.gov/ow_min.html</a></li> <li><a href="https://pandas.pydata.org/">https://pandas.pydata.org/</a></li> <li><a href="https://docs.python.org/3/library/pickle.html">https://docs.python.org/3/library/pickle.html</a></li> <li>Wintoft, P., Wik, M., & Viljanen, A. J. Space Weather Space Clim., 5, A7 (2015). <a href="http://dx.doi.org/10.1051/swsc/2015008">http://dx.doi.org/10.1051/swsc/2015008</a></li> <li><a href="https://omniweb.gsfc.nasa.gov/html/ow_data.html#time_shift">https://omniweb.gsfc.nasa.gov/html/ow_data.html#time_shift</a></li> <li><a href="https://www.intermagnet.org/index-eng.php">http://www.intermagnet.org</a></li> </ol>
Effects of subauroral polarization streams on ionospheric radial currents during the geomagnetic storm on April 23, 2023
<p>The simulation from TIEGCM used in the manuscript entitled"</p> <p><strong><span>Effects of subauroral polarization streams on ionospheric radial currents during the geomagnetic storm on April 23, 2023</span></strong></p> <p>"</p>
Geomagnetic storm data
Open the record for dataset details and reuse information.
Dataset for Investigation of Thermospheric Response to Geomagnetic Storms Using GITM-OVATION Prime and -FTA model With Comparison to GOLD and SABER Observations
<div> <div> <div> <div> <h4>Dataset Overview</h4> <p>This dataset accompanies the research paper titled " Investigation of Thermospheric Response to Geomagnetic Storms Using GITM-OVATION Prime and -FTA model With Comparison to GOLD and SABER Observations" and contains all the necessary data and scripts required to reproduce the results presented in the paper. The dataset is organized by figure numbers, corresponding directly to the figures in the paper, making it straightforward to locate and generate the specific results.</p> <h4>Structure of the Dataset</h4> <p>The dataset is divided into multiple folders, each named according to the figure numbers in the paper (e.g., Figure_1, Figure_2, etc.). Inside each of these folders, you will find:</p> <ul> <li><strong>Data Files</strong>: These files contain the raw and processed data used to generate the figures.</li> <li><strong>Scripts</strong>: MATLAB scripts (e.g., Figure_2*.m) that process the data and generate the respective figures.</li> <li><strong>Readme.txt</strong>: A text file providing detailed instructions on how to use the data and scripts, including any dependencies or specific steps required.</li> </ul> <h4>Instructions for Reproducing Figures</h4> <ol> <li> <p><strong>Download the Dataset</strong>:</p> <ul> <li>Download the entire dataset or specific figure folders as needed.</li> </ul> </li> <li> <p><strong>Prepare Your Environment</strong>:</p> <ul> <li>Ensure that MATLAB is installed on your local machine.</li> <li>Verify that all necessary MATLAB toolboxes and dependencies are installed, as specified in the Readme.txt files within each figure folder.</li> </ul> </li> <li> <p><strong>Generate Figures</strong>:</p> <ul> <li>Navigate to the directory where the dataset is saved.</li> <li>Open MATLAB and set the current directory to the folder containing the downloaded data and scripts.</li> <li>Run the script corresponding to the figure you wish to generate. For example, to generate Figure 1, navigate to the Figure_1 folder and run the <code>Figure_1*.m.</code></li> </ul> </li> <li> <p><strong>Refer to Readme.txt for Further Details</strong>:</p> <ul> <li>Each figure folder contains a Readme.txt file with additional details, including specific instructions, data descriptions, and any figure-specific requirements or notes.</li> </ul> </li> </ol> <p>By following these steps, you can successfully reproduce the figures and results presented in the paper "Paper 1 vs Paper 2" using the provided dataset and scripts. If you encounter any issues or have questions, refer to the Readme.txt files or contact the authors for further assistance.</p> </div> </div> </div> </div>
The high latitude ionospheric response to the major May 2024 geomagnetic storm: A synoptic view (Datasets)
<p>Manually scaled ionosonde, ionosonde drift, and ISR datasets for the paper. </p>
Video: The asymmetric geospace as displayed during the geomagnetic storm on August 17, 2001
<p>Measurements from multiple instruments showing large north-south asymmetries in polar geospace during a geomagnetic storm on 17 August 2001. This video is published with the paper "The asymmetric geospace as displayed during the geomagnetic storm on August 17, 2001", by Østgaard et al., at https://www.ann-geophys-discuss.net/angeo-2018-65/. The paper is currently in the first phase of review, open for discussion.</p> <p>The observations:<br> UV aurora in the north, in three different wavelength, from the IMAGE FUV instruments (left)</p> <p>UV aurora in the south, observed with the VIS Earth camera on the Polar satellite (right). The images from the north and south are simultaneous, within ~1 min.</p> <p>Equivalent currents from SuperMAG ground magnetometers are shown as red pins in the northern hemisphere</p> <p>Electron energy flux measured with the NOAA POES satellites, and the DMSP satellites, is shown as pink bars.</p> <p>Field-aligned currents, derived with in-situ magnetometer measurements on the CHAMP satellite are shown in red (up) and blue (down) colour.</p> <p>Convection measurements from SSIES on the DMSP satellites are shown as green bars</p> <p>The locations of SuperDARN backscatter are shown as green dots. The line-of-sight measurements are not shown in the video, but used in the analysis in the paper.</p> <p>Time series of magnetic indices and interplanetary magnetic field components are shown in the upper right corner.</p>
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