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6 results for “Geomagnetic observations”
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>
Ionosphere-thermosphere data published in 'The 2D evolution of thermospheric ∑O/N2 response to weak geomagnetic activity during solar-minimum observed by GOLD'
This dataset was used to generate plots for a paper in the Geophysical Research Letter, an AGU journal. It includes the percentage difference of column density ratio of O/N2 between quiet time (DOY 153 in 2019) and weak geomagnetic activity time (DOY 156 in 2019), together with the meridional wind, zonal wind, meridional component and the zonal component of E cross B drift at pressure level -1.375 (160-170 km).
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>
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>
Observations and Modeling Investigations of Ionospheric Response to April 23-24, 2023, G4-Class Geomagnetic Storm over Indian Sector
<p>This study explores the ionospheric response over the Indian sector to the G4-class geomagnetic storm of April 23-24, 2023. Utilizing multi-instrument observations and SAMI2 modeling, ionospheric behavior was examined during the storm's main phase (17:41 UT, April 23 - 04:03 UT, April 24) and the recovery phase (04:03 UT - 22:44 UT, April 24). During the main phase, ionosonde data from Tirunelveli showed rapid F-layer height (h’F) variations driven by westward and eastward prompt penetration electric fields (PPEFs). The westward PPEF, induced by undershielding, led to an initial decrease in h’F followed by an increase, suppressing pre-existing Equatorial Plasma Bubbles (EPBs) within two hours of the storm’s onset. Despite a late-night rise in h’F due to overshielding, no new EPB formed. The recovery phase exhibited a positive storm effect at low latitudes and a negative effect at higher latitudes, linked to disturbance dynamo electric fields (DDEFs) and thermospheric composition changes (O/N₂). Isofrequency analysis of CADI ionosonde and GNSS TEC data revealed large-scale traveling ionospheric disturbances (LSTIDs) with a ~2-hour period, ~2,450 km wavelengths, and ~340 m/s equatorward propagation speed. These LSTIDs were likely driven by atmospheric gravity waves or auroral heating. The westward DDEF suppressed the equatorial ionization anomaly (EIA) and inhibited post-sunset EPBs, while eastward DDEF increased h’F post-midnight without EPB formation. We speculate this absence might be due to a lack of seeding mechanisms. SAMI2 simulations incorporating E×B drift data reproduced several storm-time features in the main and recovery phases.</p>
RInex files from HK GNSS network in observing simultaneous and consecutive occurrence of thunderstorm and geomagnetic storm
<p>These are the RInex files from HK GNSS network in observing simultaneous and consecutive occurrence of thunderstorm and geomagnetic storm</p>
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