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103 results for “magnetosphere”
MHD Model of Ganymede's Magnetosphere: Predicted OCFB and magnetic footprint surface locations for Juno's flyby
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish coordinates for the predicted location of the open-closed-field line-boundary (OCFB) on Ganymede's surface. Additionally we provide coordinates of Juno's magnetic footprint, namely the surface locations that connect to Juno's trajectory through magnetic field lines.</p> <p>For the surface locations we use a western longitude planetographic coordinate system where 0° longitude is in direction of the y-axis and 90° in direction of the x-axis of the cartesian GPhiO system. The GPhiO system is defined by the primary direction<br> z parallel to Jupiter’s rotation axis, the secondary direction y is pointing towards Jupiter barycenter<br> and x completes the right-handed system approximately in direction of plasma flow.</p> <p><strong>Duling2022_JunoGanymede_modeled_surface_OCFB.txt</strong></p> <p>Columns:</p> <p>Longitude [°]<br> Northern OCFB latitude [°]<br> Southern OCFB latitude [°]</p> <p><strong>Duling2022_JunoGanymede_modeled_magnetic_footprint.txt</strong></p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Magnetic footprint longitude [°]<br> Magnetic footprint latitude [°]<br> Length of field line between Juno and surface [radii]<br> Length of field line between Juno and surface [km]<br> r coordinate of Juno [radii]<br> Latitude of Juno [°]<br> Longitude of Juno [°]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p> <p><strong>Duling2022_JunoGanymede_surface_map.png</strong></p> <p>A plot that visualizes the data of this repository.</p>
8 years of dayside Magnetospheric Multiscale (MMS) unsupervised clustering plasma regions classifications
<p>These files contain the 1-minute resolution dataset (“labeled_sunside_data.csv”) and 15 minute or longer region list (“<region_name>_region_list.csv”) for Toy-Edens et al.'s Classifying 8 years of MMS Dayside Plasma Regions via Unsupervised Machine Learning. The 1-minute resolution file contains the rolled up 1-minute epoch, probe name (mms1, mms2, mms3, mms4), features that go into clustering and post-cleansing methods, spacecraft positions (in GSE, GSM, and magnetic latitude/local time), raw and cleansed clustering labels, and transition name. The 15+ minute region lists contain the name of the plasma region type, the probe name (mms1, mms2, mms3, mms4), and the start and stop epoch of >= 15 minute epoch where the probe is solidly within that region. NOTE: for the 15+ minute region lists we are only looking for changes in plasma regions, this means that missing data may artificially inflate the duration of the epoch, we suggest looking at the full 1-minute resolution dataset to confirm the region timing.</p> <p>We ask that if you use any parts of the dataset that you cite Toy-Edens et al.'s Classifying 8 years of MMS Dayside Plasma Regions via Unsupervised Machine Learning (DOI:10.1029/2024JA032431).</p> <p>This work was funded by grant 2225463 from the NSF GEM program.</p> <p> </p> <p>The following tables detail the contents of the described files:</p> <p><strong>labeled_sunside_data.csv description</strong></p> <table> <tbody> <tr> <td> <p><strong>Column Name</strong></p> </td> <td> <p><strong>Description</strong></p> </td> </tr> <tr> <td> <p>Epoch</p> </td> <td> <p>Epoch in datetime</p> </td> </tr> <tr> <td> <p> probe</p> </td> <td> <p>MMS probe name</p> </td> </tr> <tr> <td> <p> ratio_max_width</p> </td> <td> <p>Ratio of the width of the most prominent ion spectra peak (in number of energy channels) to max number of energy channels. See paper for more information</p> </td> </tr> <tr> <td> <p> ratio_high_low</p> </td> <td> <p>Ratio of the mean of the log intensity of high energies in the ion spectra to the mean of the log intensity of low energies in the ion spectra. See paper for more information</p> </td> </tr> <tr> <td> <p> norm_Btot</p> </td> <td> <p>Magnitude of the total magnetic field normalized to 50nT. See paper for more information</p> </td> </tr> <tr> <td> <p> small_energy_mean</p> </td> <td> <p>The denominator in ratio_high_low</p> </td> </tr> <tr> <td> <p> large_energy_mean</p> </td> <td> <p>The numerator in ratio_high_low</p> </td> </tr> <tr> <td> <p> temp_total</p> </td> <td> <p>Total temperature from the DIS moments. See paper for more information</p> </td> </tr> <tr> <td> <p> r_gse_x</p> </td> <td> <p>x position of the spacecraft in GSE</p> </td> </tr> <tr> <td> <p> r_gse_y</p> </td> <td> <p>y position of the spacecraft in GSE</p> </td> </tr> <tr> <td> <p> r_gse_z</p> </td> <td> <p>z position of the spacecraft in GSE</p> </td> </tr> <tr> <td> <p> r_gsm_x</p> </td> <td> <p>x position of the spacecraft in GSM</p> </td> </tr> <tr> <td> <p> r_gsm_y</p> </td> <td> <p>y position of the spacecraft in GSM</p> </td> </tr> <tr> <td> <p> r_gsm_z</p> </td> <td> <p>z position of the spacecraft in GSM</p> </td> </tr> <tr> <td> <p> mlat</p> </td> <td> <p>magnetic latitude of spacecraft</p> </td> </tr> <tr> <td> <p> mlt</p> </td> <td> <p>magnetic local time of spacecraft</p> </td> </tr> <tr> <td> <p> raw_named_label</p> </td> <td> <p>Raw cluster assigned plasma region label (allowed values: magnetosheath, magnetosphere, solar wind, ion foreshock)</p> </td> </tr> <tr> <td> <p> modified_named_label</p> </td> <td> <p>Cleansed cluster assigned plasma region label (use these unless have a specific reason to use raw labels). See paper for more information</p> </td> </tr> <tr> <td> <p> transition_name</p> </td> <td> <p>Transition names (e.g. quasi-perpendicular bow shock, magnetopause). See paper for more information</p> </td> </tr> </tbody> </table> <p> </p> <p><strong><region_name>_region_list.csv description</strong></p> <table> <tbody> <tr> <td> <p><strong>Column Name</strong></p> </td> <td> <p><strong>Description</strong></p> </td> </tr> <tr> <td> <p>start</p> </td> <td> <p>Starting Epoch in datetime</p> </td> </tr> <tr> <td> <p>stop</p> </td> <td> <p>Stopping Epoch in datetime</p> </td> </tr> <tr> <td> <p>probe</p> </td> <td> <p>MMS probe name</p> </td> </tr> <tr> <td> <p>region</p> </td> <td> <p>Cleansed cluster name associated with 1-minute resolution “modified_named_label”</p> </td> </tr> </tbody> </table> <p> </p> <p> </p> <p> </p>
MHD Model of Ganymede's Magnetosphere: Predicted magnetic field on Juno's trajectory
<p>This dataset contains model results from a magnetohydrodynamic (MHD) model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021. Here we publish predicted magnetic field components on Juno's trajectory that can be compared to MAG measurements and are displayed in Figure 3 of Duling et al. (2022).</p> <p>Each file contains data from one model. The dataset includes all models with parameter variations from Duling et al. (2022). These are summarized in Table 1 of Duling et al. (2022) and displayed in Figure 3 with the gray lines.</p> <p>If not varied, all models are run with the following parameters:</p> <p>Upstream Jovian background magnetic field B<sub>0 </sub>= (−15,24,−75) nT<br> Upstream plasma velocity v<sub>0</sub> = 140 km/s<br> Upstream plasma mass density <span class="math-tex">\(\rho\)</span><sub>0</sub> = 100 amu/cm<sup>3</sup><br> Upstream plasma thermal pressure p<sub>0</sub> = 2.8 nPa<br> Ionization frequency <span class="math-tex">\(\nu_{ion}\)</span> = 2.2e-8/s<br> Atmospheric surface mass density <span class="math-tex">\(n_{n,0}\)</span> = 8e6/cm<sup>3</sup><br> Dipole Gauss coefficient <span class="math-tex">\(g_1^0\)</span> = −716.8 nT</p> <p> </p> <p>The published data files correspond to the following models with each one parameter variation:</p> <table> <thead> <tr> <th scope="col">Parameter</th> <th scope="col">Value</th> <th scope="col">Filename Suffix</th> </tr> </thead> <tbody> <tr> <td>default model</td> <td> - </td> <td>default</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured before flyby)</td> <td>B<sub>0 </sub>= (−16,3,−70) nT</td> <td>B0before</td> </tr> <tr> <td>Upstream Jovian background magnetic field (measured after flyby)</td> <td>B<sub>0 </sub>= (−14,43,−80) nT</td> <td>B0after</td> </tr> <tr> <td>Upstream plasma velocity (min)</td> <td>v<sub>0</sub> = 120 km/s</td> <td>v-</td> </tr> <tr> <td>Upstream plasma velocity (max)</td> <td>v<sub>0</sub> = 160 km/s</td> <td>v+</td> </tr> <tr> <td>Upstream plasma mass density (min)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 10 amu/cm<sup>3</sup></td> <td>rho-</td> </tr> <tr> <td>Upstream plasma mass density (max)</td> <td><span class="math-tex">\(\rho\)</span><sub>0</sub> = 160 amu/cm<sup>3</sup></td> <td>rho+</td> </tr> <tr> <td>Upstream plasma thermal pressure (min)</td> <td>p<sub>0</sub> = 1.0 nPa</td> <td>p-</td> </tr> <tr> <td>Upstream plasma thermal pressure (max)</td> <td>p<sub>0</sub> = 5.0 nPa</td> <td>p+</td> </tr> <tr> <td>Ionization frequency (min)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 0.5e-8/s</td> <td>prod-</td> </tr> <tr> <td>Ionization frequency (max)</td> <td> <span class="math-tex">\(\nu_{ion}\)</span> = 10.0e-8/s</td> <td>prod+</td> </tr> <tr> <td>Atmospheric surface mass density (min)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 1.6e6/cm<sup>3</sup></td> <td>nn-</td> </tr> <tr> <td>Atmospheric surface mass density (max)</td> <td> <span class="math-tex">\(n_{n,0}\)</span> = 40e6/cm<sup>3</sup></td> <td>nn+</td> </tr> <tr> <td>Dipole Gauss coefficient (min)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −702.5 nT</td> <td>dipole-</td> </tr> <tr> <td>Dipole Gauss coefficient (max)</td> <td> <span class="math-tex">\(g_1^0\)</span> = −731.1 nT</td> <td>dipole+</td> </tr> </tbody> </table> <p>Magnetic Field components and Juno's position are in GPhiO system. GPhiO is defined by the primary direction z parallel to Jupiter’s rotation axis, the secondary direction y is pointing from Ganymede's towards Jupiter's barycenter and x completes the right-handed system approximately in direction of plasma flow.</p> <p>Columns:</p> <p>Spacecraft time [UTC]<br> Bx modeled magnetic field in GPhiO [nT]<br> By modeled magnetic field in GPhiO [nT]<br> Bz modeled magnetic field in GPhiO [nT]<br> B modeled magnetic field magnitude [nT]<br> x of Juno in GPhiO [km]<br> y of Juno in GPhiO [km]<br> z of Juno in GPhiO [km]</p>
Data for "Constraints on the Observability of Energetic Neutral Atoms from the Magnetosphere-Atmosphere Interactions at Callisto and Europa" by Haynes et al.
<p>Accompanying data products for publication entitled "Constraints on the Observability of Energetic Neutral Atoms from the Magnetosphere-Atmosphere Interactions at Callisto and Europa". The manuscript was submitted to JGR Space Physics shortly after upload.</p> <p>Data includes all simulation outputs that are depicted in this work, both for the AIKEF hybrid model (i.e., Figure 4) and the model used to produce synthetic ENA images (Figures 3, 6, 8, 9, 11, A1, and B1). All other figures in the work are used for illustrative purposes and were not generated with simulation output. </p> <p>Information regarding the organization and file structure can be found in H24_data_readme.txt , as well as which dataset corresponds to which figure. Any inquiries, questions, or comments may be addressed through the email associated with this data publication.</p>
Saturn's magnetospheric proton and electron intensities from Cassini
<p>Differential intensities of 3keV – 40MeV protons and 10eV – 10MeV electrons in Saturn’s magnetosphere and radiation belts at L-shell distances between 1 and 20 Saturn radii from mission-averages of the MIMI/LEMMS, MIMI/CHEMS, and CAPS/ELS instruments on the Cassini spacecraft that was in orbit between 2004 and 2017.</p>
Global Empirical Picture of Magnetospheric Substorms Inferred from Multi-Mission Magnetometer Data
<p>Data associated with Journal of Geophysical Research: Space Physics article titled: "Global Empirical Picture of Magnetospheric Substorms Inferred from Multi-Mission Magnetometer Data". This includes all the digital data that was used in constructing the Figures from the main and supplementary text, along with files containing the fit set of coefficients and parameters for the model, and files describing the subset of magnetometer used for fitting the model. </p>
Dataset: Random forest models of ultra-low frequency magnetospheric wave power.
<p>Predictive models of ground-based ultra-low frequency (ULF, 1-15 mHz) wave power, corresponding to magnetospheric waves. The series of decision tree ensembles (random forests) are dependent on solar wind properties, latitude and azimuthal angle around the Earth (magnetic local time, MLT).</p>
The impact of solar wind magnetic field fluctuations on the magnetospheric energetics
<p>This dataset provides the results and analysis tools of the manuscript by Ala-Laht et al. "The impact of solar wind magnetic field fluctuations on the magnetospheric energetics". In addition, relevant SWMF simulation input files are included. See ReadMe.txt for information.</p>
Dataset of steady magnetospheric convection events in Earth's magnetosphere from 1997 to 2013
<p>This dataset is a list of steady magnetospheric convection (SMC) events occurring in Earth's magnetosphere between 1997 and 2013. The criteria and method of SMC selection are documented in the following two papers:</p> <p>Kissinger et al. (2011), "Steady magnetospheric convection and stream interfaces: Relationship over a solar cycle", JGR, doi:10.1029/2010JA015763.<br> <br> Kissinger et al. (2012), "Diversion of plasma due to high pressure in the inner magnetosphere during steady magnetospheric convection", JGR, doi:10.1029/2012JA017579.</p> <p>The filename "smc_list_1997_2013.csv" is a list of every SMC selected during this time period. This is a comma-separated file with two columns: the first column is the timestamp indicating the start of the SMC event, and the second column is the timestamp indicating the end of the SMC event. </p> <p>The filename "smc_list_1997_2013_longerthan5hrs.csv" is a subset of the first list, filtered to only SMCs with a duration longer than 5 hours. The schema of this file matches the first one, with an additional third column showing the duration of the SMC in hours.</p>
Thin Filaments in an Average Magnetosphere: Pure Interchange vs. Ballooning Oscillations
<p>This paper describes magnetospheric waves of very long wavelength in thin magnetic filaments. We consider an average magnetospheric configuration with zero ionospheric conductance and calculate waves using two different formulations: classic interchange theory and ideal MHD. Classic interchange theory, which is developed in detail in this paper, is basically analytic and is relatively straightforward to determine computationally, but it can’t offer very high accuracy.</p> <p>The two formalisms agree well for the plasma sheet and also for the inner magnetosphere. The eigenfrequencies range over about a factor of seven, but the formulations generally agree with a root-mean-square difference between the logarithms of interchange and MHD frequencies to be $\sim 0.054$. The pressure perturbations in the classic interchange theory are assumed constant along each field line, but the MHD computed pressure perturbations along the field line vary in a range $\sim 30 \%$ in the plasma sheet but are larger in the inner magnetosphere. The parallel and perpendicular displacements, which are very different in the plasma sheet and inner magnetosphere, show good qualitative agreement between the two approaches. In the plasma sheet, the perpendicular displacements are strongly concentrated in the equatorial plane, whereas the parallel displacements are spread through most of the plasma sheet away from the equatorial plane; and can be regarded as buoyancy waves. In the inner magnetosphere, the displacements are more sinusoidal and are more like conventional slow modes. The different forms of the waves are best characterized by the flux tube entropy $PV^\gamma$.</p>
MHD model output for Ganymede's magnetosphere during Juno's flyby
<p>This dataset contains the complete simulation output from our MHD model of Ganymede's magnetosphere adapted to Juno's PJ34 flyby in 2021 (Duling et al. 2022).</p> <p>The data was obtained by our application of the PLUTO simulation code v4.4 (Mignone et al. 2007) (http://plutocode.ph.unito.it/) described in Duling et al. 2022.</p> <p>The dataset includes the simulation variables on the simulation grid for a single timestep after steady state was reached. The grid has spherical geometry (r, theta, phi) with phi=0° longitude pointing towards Jupiter (positive y axis of the GPhiO system), phi=90° longitude pointing in the upstream direction (negative x axis of GPhiO) and theta=0° latitude at Ganymede's north pole (positive z axis of GPhiO). The following model variables are included:</p> <p>rho: plasma mass density<br> prs: thermal plasma pressure<br> vx1: plasma velocity radial component<br> vx2: plasma velocity theta component<br> vx3: plasma velocity phi component<br> Bx1: magnetic field radial component<br> Bx2: magnetic field theta component<br> Bx3: magnetic field phi component</p> <p>Additionally the following derived variables are included:</p> <p>Jx1: electric current density radial component<br> Jx2: electric current density theta component<br> Jx3: electric current density phi component<br> Bpx1: plasma magnetic field radial component<br> Bpx2: plasma magnetic field theta component<br> Bpx3: plasma magnetic field phi component</p> <p>Plasma magnetic field means that part of the total magnetic field that results from the plasma interaction. It equals the total magnetic field subtracted by the homogeneous upstream field and Ganymede's intrinsic and induced field.</p> <p>All values are in normalized units with these normalization factors:</p> <p>NORMR = 2.631e8 cm<br> NORMV = 1.4e7 cm/s<br> NORMRHO = 1.661e-22 g/cm^3<br> NORMPRS = 3.255e-08 dyne/cm^2<br> NORMB = 6.395e-04 Gauss<br> NORMJ = 5.801e-03 statA/cm^2</p> <p>In Duling et al. 2022 we present results of a model sensitivity study. This dataset includes model output from our best guess setup (default setup) only.</p> <p>Since the data is in PLUTO's binary format "flt" we provide a Python code snippet that reads the data to data arrays.</p> <p><strong>grid.out</strong><br> This ASCII file contains the grid dimensions and coordinates of the cell boundaries.</p> <p><strong>data.0020.flt</strong><br> This binary file contains the simulation variables on the cell centers of the grid.</p> <p><strong>pluto.0.log</strong><br> This ASCII file contains the header of the PLUTO logfile.</p> <p><strong>read_data.py</strong><br> This Python code snippet helps with reading the data.</p>
Modeling the Emission of Energetic Neutral Atoms in Titan's Dynamic Magnetospheric Environment
<p>Data for the manuscript "Modeling the Emission of Energetic Neutral Atoms in Titan's Dynamic Magnetospheric Environment" by Tippens et al., (2024). See README.txt for a description of the data files included here.</p>
Buoyancy Waves in Earth's Nightside Magnetosphere: Normal-Mode Oscillations of Thin Filaments
<ul> <li>A theory has been developed for small oscillations of a thin filament in the magnetosphere.</li> <li>For the lowest-frequency even modes, the eigenfunctions are essentially buoyancy waves in the plasma sheet, but they are more like slow modes in the inner magnetosphere.</li> <li>For the lowest-frequency even modes, the eigenfrequencies (radians/s) have peak values of approximately 0.07 s<sup>-1</sup> between the inner plasma sheet and plasmapause, for an average magnetospheric field. </li> <li>This includes software and model data used in this paper.</li> <li>Submitted to JGR for review</li> </ul>
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>
The Plasma Distribution in Saturn's Inner Magnetosphere from 2.4 to 10 Rs: A Diffusive Equilibrium Model
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics, <a href="https://doi.org/10.1029/2019JA027545">10.1029/2019JA027545</a></p> <p>Abstract:</p> <p>Electron density measurements have been obtained by the Cassini Radio and Plasma Wave Science (RPWS) instrument covering the period from 30 June, 2004 to 19 April, 2017, spanning latitudes up to ~30<sup>o </sup>and <em>L</em> values from 2.4 to 10. Near the F ring, electron densities are derived from RPWS measurements of electron plasma oscillations at high latitudes and from the Langmuir Probe (RPWS/LP) sweep data at low latitudes. The electron density measurements from the ring-grazing orbits, beginning in December 2016, have made it possible to extend the work of a previous diffusive equilibrium model to include the distribution of the ring plasma. Beyond the ring-grazing orbits, the densities are derived from RPWS measurements of the upper hybrid resonance frequency. These density measurements are used to anchor the fit of an expanded diffusive equilibrium density model for a two-species plasma consisting of water group and hydrogen ions in Saturn’s inner magnetosphere. Density contour plots for the two ion species and the electrons are presented. The distribution of the derived plasma densities is consistent with two primary sources, the Enceladus plumes and the extended ring atmosphere. There is also an indication of a weaker plasma source at Dione. In the region just outside the A Ring and in the region including the Enceladus orbit, the diffusive equilibrium model also clearly shows the expansion of lighter ions and electrons to higher latitudes along the magnetic field lines with evidence of a weaker plasma expansion between the orbits of Tethys and Dione.</p>
Simulation dataset of "Particle-in-cell simulations of characteristics of rising-tone chorus waves in the inner magnetosphere"
<p>Simulation dataset of "Particle-in-cell simulations of characteristics of rising-tone chorus waves in the inner magnetosphere", including magnetic fields and parallel and perpendicular temperatures of energetic electrons.</p>
The_Global_Distribution_of_Ultra-Low-Frequency_Waves_in_Jupiter's_Magnetosphere_MannersH_ds01
<p>A supporting information dataset for the article "The Global Distribution of Ultra-Low-Frequency Waves in Jupiter's Magnetosphere", submitted by H. Manners and A. Masters. The file contains an Excel spreadsheet detailing the "datetime" intervals containing the events used in the survey described by the article. Additional details are listed alongside the datetimes: the average positions of the spacecraft during each event in radius from the planet, latitude and local time, expressed in Sysem III Jovian coordinates.</p>
Simulation datum of Full particle simulation of whistler-mode triggered falling-tone emissions in the magnetosphere
<p><strong>Overview</strong></p> <p>This dataset is obtained from <a href="http://space.rish.kyoto-u.ac.jp/software/">KEMPO1</a> code with minor modifications. This dataset consists of raw data of simulation, an example of the python code, and Dockerfile to construct a drawing environment using Python. For more detail, please refer README.md.</p> <p><strong>Command example using <a href="https://www.docker.com/">Docker</a></strong></p> <p>If you draw figures using Docker, please download <strong>ALL the files</strong> in the dataset.<br> Make sure that all files are put at the same directory.</p> <pre><code class="language-bash">cd (path to downloaded files) docker build -t kempo1data . docker run -v ${PWD}:/data -it kempo1data python plot_data.py <data_file>.h5</code></pre>
Solar Energetic Proton Access to the Inner Magnetosphere during the 7-8 September 2017 event
<p>Dataset used in the manuscript.</p> <p> </p> <p>2fluxLFM.txt: The first two columns are time from 09/07 00UT in hours and L along RBSP-B trajectory where the cutoff energy in vertical direction calculated using LFM model is 21 MeV. The third and fourth columns are time from 09/07 00UT in hours and L along RBSP-A trajectory where the cutoff energy in vertical direction calculated using LFM model is 21 MeV. Columns 5 and 6 are time from 09/07 00UT in hours and L where the 21 MeV proton flux measured by RBSP-B is 50% of the interplanetary flux. Columns 7 and 8 are time from 09/07 00UT in hours and L where the 21 MeV proton flux measured by RBSP-A is 50% of the interplanetary flux. </p> <p>2fluxTS.txt: Columns 1 and 2 are time from 09/07 00UT in hours and L where the 21 MeV proton flux measured by RBSP-B is 50% of the interplanetary flux. Columns 3 and 4 are time from 09/07 00UT in hours and L where the 21 MeV proton flux measured by RBSP-A is 50% of the interplanetary flux. Columns 5 and 6 are time from 09/07 00UT in hours and L along RBSP-A trajectory where the cutoff energy in vertical direction calculated using LFM model is 21 MeV. Columns 7 and 8 are time from 09/07 00UT in hours and L along RBSP-B trajectory where the cutoff energy in vertical direction calculated using LFM model is 21 MeV. </p> <p>acut_0907.txt and acutoff_0908.txt are the cutoff energy along RBSP-A orbit calculated using TS07. The first column is time in seconds, the next three columns are the satellite location (radial distance in Re, latitude and longitude), and the last three columns are the cutoff energy in MeV in west, vertical and east direction. </p> <p>bcut_0907.txt and bcutoff_0908.txt are the cutoff energy along RBSP-B orbit calculated using TS07. The first column is time in seconds, the next three columns are the satellite location (radial distance in Re, latitude and longitude), and the last three columns are the cutoff energy in MeV in west, vertical and east direction. </p> <p>cutoffa_t700_fixed.dat and cutoffb_t700.dat are the cutoff energy along RBSP-A and RBSP-B orbits calculated using LFM. The first column is time in seconds, the next three columns are the satellite location (radial distance in Re, latitude and longitude), and the last three columns are the cutoff energy in MeV in west, vertical and east direction. </p> <p>tmax_test.txt is the cutoff energy using different tmax parameters at two time points. The first column is time in seconds from the start of the simulation. The next three column are the satellite location (radial distance in Re, latitude and longitude). The last three columns are the cutoff energy in MeV in west vertical and east directions. Lines corresponds to different tmax parameters. </p> <p>vap_081.txt and vap_082.txt are external Bz in nT measured by RBSP-B along an outbound orbit on 09/08 0719-1110UT and an inbound orbit on 09/08 1145-1545UT.</p> <p>ts05_081.txt and ts05_082.txt are external Bz in nT calculated using TS05 magnetic field model at RBSP-B location along an outbound orbit on 09/08 0719-1110UT and an inbound orbit on 09/08 1145-1545UT.</p> <p>ts07_081.txt and ts07_082.txt are external Bz in nT calculated using TS07 magnetic field model at RBSP-B location along an outbound orbit on 09/08 0719-1110UT and an inbound orbit on 09/08 1145-1545UT</p> <p>lfm_081.txt and lfm_082.txt are external Bz in nT calculated using LFM global MHD model at RBSP-B location along an outbound orbit on 09/08 0719-1110UT and an inbound orbit on 09/08 1145-1545UT</p> <p>b1430TS05 and EXTERNALTS07.txt are the magnetic field in nT calculated by TS05 and TS07 on 09/08 1430UT. </p>
Data for "Direct evidence reveals transmitter signal propagation in the magnetosphere"
<p>The data and codes for figures in "Direct evidence reveals transmitter signal propagation in the magnetosphere"</p>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
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DANDI Archive for NWB datasets
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International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.