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16 results for “MHD data”
Additional evidence for a pulsar wind nebula in SN 1987A from multi-epoch X-ray data and MHD modelling
<p>This is a basic reproduction package for the paper "Additional evidence for a pulsar wind nebula in the hearth of sN 1987A from multi-epoch X-ray data and MHD modeling" by Greco et al. 2022. It aims to provide the most important data products to check and reproduce the main results of the paper.</p>
Data sets for "Magnetic helicity dissipation and production in an ideal MHD code"
<pre>The tar archive Helicity_in_IdealMHDCode.tar contains an index.html file with links to a directory with "Add-ons" to the FLASH code and the flash.par file. We also list the IDL directory with secondary data and plot routines for each figure used in the paper "Magnetic helicity dissipation and production in an ideal MHD code" by Axel Brandenburg (Nordita) and Evan Scannapiecoo (Arizona State University) with the URL https://arxiv.org/abs/1910.06074.</pre>
Data for "The Spatiotemporal Structure of Induced Magnetic Fields in Callisto's Plasma Environment due to their Propagation with MHD Modes" by Strack & Saur
<div>This dataset contains data from the publication Strack & Saur, 2024 (<a href="https://doi.org/10.1029/2024JA033235">https://doi.org/10.1029/2024JA033235</a>), including the output of our MHD model as well as processed data used in Figures 4, 5, and 6.<br> <div> </div> <div>We use a Cartesian and a spherical coordinate system, both with the origin at the geometric center of Callisto. In the Cartesian system, the z-axis is parallel to Jupiter’s rotation axis, the y-axis points to the center of Jupiter and the x-axis, which completes the right-handed coordinate system, is approximately in direction of Callisto's orbital motion. In the spherical coordinate system, phi=0° is defined on the Jupiter-facing meridian (positive y-axis) and is counted in an easterly direction, i.e., phi=90° is the upstream direction (negative x-axis). Theta is taken from the positive z-axis.<br><br></div> <div> <div> <h2>Simulation Output</h2> <br> <div>The PLUTO simulation code (v4.4, Mignone et al. 2007, http://plutocode.ph.unito.it) was used for the numerical solution of the MHD model. A description of the model equations, boundary conditions and simulation process is given Strack & Saur, 2024.</div> <br> <div>The simulations were performed in spherical geometry (r, theta, phi). Each "*.flt" output file contains the model variables on the simulation grid for a single time step. The respective simulation grid is specified in the "grid.out" file. The model variables are:</div> <ul> <li>rho: Plasma mass density</li> <li>vx1: Plasma bulk velocity, r component</li> <li>vx2: Plasma bulk velocity, theta component</li> <li>vx3: Plasma bulk velocity, phi component</li> <li>Bx1: Magnetic field, r component</li> <li>Bx2: Magnetic field, theta component</li> <li>Bx3: Magnetic field, phi component</li> <li>prs: Thermal plasma pressure</li> </ul> <div> <div>Each simulation output file also contains the following additional variables:</div> <ul> <li>Bpx1: In our case, this is the same as Bx1</li> <li>Bpx2: In our case, this is the same as Bx2</li> <li>Bpx3: In our case, this is the same as Bx3</li> <li>Jx1: Electric current density, r component</li> <li>Jx2: Electric current density, phi component</li> <li>Jx3: Electric current density, theta component</li> </ul> <div>In the output files, all values are in normalized units. The normalization factors (in CGS units) are:</div> <ul> <li>norm_r = 2410e3 cm</li> <li>norm_t = 1.255e1 s</li> <li>norm_rho = 1.594e-24 g/cm^3</li> <li>norm_v = 1.92e7 cm/s</li> <li>norm_B = 8.593e-05 Gauss</li> <li>norm_prs = 5.877e-10 dyne/cm^3</li> <li>norm_J = 8.508e-04 statA/cm^2</li> </ul> <div>Since the simulation output files are in PLUTO's binary ".flt" format, we provide the Python script "read_data.py" to read the simulation data and grid specifications.</div> <br> <div>We provide the following simulation data:</div> <br> <div>For Section 4 in Strack & Saur, 2024</div> <ul> <li>`./symmetric_model_reference`: The reference simulation, i.e., moon-magnetosphere interactions only<br>`./symmetric_model_full_A075`: The (main) full simulation with A=0.75, i.e., moon-magnetosphere interactions and induced magnetic field<br>`./symmetric_model_full_A025`: The full simulation with A=0.25<br>`./symmetric_model_full_A050`: The full simulation with A=0.50<br>`./symmetric_model_full_A100`: The full simulation with A=1.00</li> </ul> <div>For Section 5 in Strack & Saur, 2024</div> <div> <ul> <li>`./C03_high_density_reference`: The reference simulation for the C03 flyby with the higher initial plasma mass density</li> <li>`./C03_high_density_full`: The full simulation with A=0.85 for the C03 flyby with the higher initial plasma mass density</li> <li>`./C03_low_density_reference`: The reference simulation for the C03 flyby with the lower initial plasma mass density</li> <li>`./C03_low_density_full`: The full simulation with A=0.85 for the C03 flyby with the lower initial plasma mass density</li> <li>`./C09_high_density_reference`: The reference simulation for the C09 flyby with the higher initial plasma mass density</li> <li>`./C09_high_density_full`: The full simulation with A=0.85 for the C09 flyby with the higher initial plasma mass density</li> <li>`./C09_low_density_reference`: The reference simulation for the C09 flyby with the lower initial plasma mass density</li> <li>`./C09_low_density_full`: The full simulation with A=0.85 for the C09 flyby with the lower initial plasma mass density</li> </ul> </div> <br> <div>Note that in the simulation data that is provided for the symmetric model (Section 4), the output numbers of the data files are different. This is because a higher output frequency was used for the reference simulation and the A=0.75 full simulation. All output files for the symmetric full simulations refer to the end of the propagation time span shown in Figure 4. For the reference simulation, the output is provided at the beginning and end of this time span.</div> <div> </div> <div> <div> <h2>Processed Data</h2> <p>In addition to the simulation output, we provide processed data used in Figures 4, 5 and 6 of Strack & Saur, 2024.</p> <p>The directory `./data_figure_4_and_5` contains the following files for each of the four panels in Figure 4:</p> <ul> <li>`fig4_panel_*_reference.csv`: The magnetic field of the reference simulation for the respective profile. Provided are the mean, minimum, and maximum values of each component (Bx, By, Bz) in the analyzed time period.</li> <li>`fig4_panel_*_full_Bx.csv`: The time series of the Bx magnetic field component of the full simulation for the respective profile. Each column contains values for a different position (given in the first row) and each row contains values for a different point in time (given in the first column).</li> <li>`fig4_panel_*_full_By.csv`, `fig4_panel_*_full_Bz.csv`: The time series of the By and Bz magnetic field components, respectively.</li> </ul> <p>The data given for panels a and b are also used in Figure 5.</p> <p>The directory `./data_figure_6` contains a single file `fig6_sample_data.csv` with the data used for Figure 6.</p> <ul> <li>The first three columns of the file give the Cartesian coordinates of the sample points</li> <li>"B_sec_infinity" is the magnitude of the induced magnetic dipole field in a vacuum environment with A=1.0 (Equation 1)</li> <li>"dB_reference" is the numerical variability of the reference simulation in its approximately stationary state</li> <li>The last four columns (e.g. "B_sec_A025") contain the transport altered induced magnetic field magnitudes in the plasma environment for a true dipole amplitude of A=0.25, A=0.50, A=0.75, and A=1.00</li> </ul> <p>Note that length, time and magnetic field in the processed data are given in units of Callisto radii (Rc), seconds and nanotesla.</p> </div> <h2>References:</h2> <div> <div>Mignone, A., Bodo, G., Massaglia, S., Matsakos, T., Tesileanu, O., Zanni, C., & Ferrari, A. (2007). PLUTO: A Numerical Code for Computational Astrophysics. The Astrophysical Journal Supplement Series, 170(1), 228–242. https://doi.org/10.1086/513316</div> <br> <div>Strack, D., Saur, J. (2024). The Spatiotemporal Structure of Induced Magnetic Fields in Callisto's Plasma Environment Due to Their Propagation With MHD modes. Journal of Geophysical Research: Space Physics, 129(12), https://doi.org/10.1029/2024JA033235</div> </div> </div> </div> </div> </div> </div>
Selected BATSRUS MHD output data and IE solver data for August 3, 2016
<p>This is a dataset for BATSRUS MHD model output and IE module output used to prepare Figures 2, 3, 4 for a second submission to GRL of a paper by A. M. Keese, N. Buzulukova, C. Mouikis and E. E. Scime "Mesoscale structures in Earth's magnetotail observed using energetic neutral atom imaging". The dataset has one file in .zip format.</p> <p>The file BATSRUS_IE_data_Fig2_3_4.zip contains the data for plotting BATSRUS results and IE module results for the Figures 2, 3, 4.</p> <p>Figure 2: file Fig2_imf_BATSRUS_input.dat has solar wind data used as an input to BATSRUS run.<br> file Fig2_ae_index.dat has model AU and AL indices</p> <p>Figure 3: files Fig3* are standard output files for IE module (ASCII) and could be plotted with spacepy package.</p> <p>Figure 4: file Fig4_BATSRUS_3D_0520UT_nx300_ny150_nz150.csv has 3D output from BATSRUS interpolated to a regular grid (nx=300, ny=150, nz=150) required to plot Figure 4. The Figure 4 could be reproduced with ParaVew free 3D plotting software.</p>
Exploring Localized Geomagnetic Disturbances in Global MHD: Physics and Numerics (Model Data)
<p>Model Data to reproduce plots from article "Exploring Localized Geomagnetic Disturbances in Global MHD: Physics and Numerics". README contains information on where to access model and visualization tools.</p>
Data for the paper "Computing MHD equilibria of stellarators with a flexible coordinate frame"
<p>Data for the revised paper "<span>Computing MHD equilibria of stellarators with a </span><span>flexible coordinate frame"</span></p> <p>Thetitle has changed from the submission title: "A generalized Frenet frame for computing MHD equilibria in stellarators"</p> <p>We provide the input and output files for all GVEC simluations presented at the "JOINT VARENNA - LAUSANNE INTERNATIONAL WORKSHOP: THEORY OF FUSION PLASMAS, 2024" and to be published in PPCF.</p> <p>An ipython script that generates the postprocessing /plots is also provided.</p> <p>New content computing the frame from a boundary surface obtained from quasr is now also part of this compilation.</p> <p>See the README.md file for details.</p>
Data for the manuscript named 'Soft X-ray imaging of the magnetosheath and cusps under different solar wind conditions: MHD simulations'
<p> This is the data used by the manuscript named 'Soft X-ray imaging of the magnetosheath and cusps under different solar wind conditions: MHD simulations'.</p> <p> The uploaded data is the X-ray intensity data for all the five cases studied in the manuscritpt. 'Casen' (n=1, 2, 3, 4, and 5) in the name of each data file indicates the case number, and 'sat pointX' (X=A, B, C, D) show the satellite positions analyzed in the manuscript. </p> <p> The data can be read by IDL using the following program statments:</p> <p>openr,lun,datai,/get_lun<br> xgse=0. & ygse=0. & zgse=0.<br> readf,lun,xgse,ygse,zgse ;;;;(satellite position in the GSE coordinate)<br> xsat=0. & ysat=0. & zsat=0.<br> readf,lun,xsat,ysat,zsat ;;;;(satellite position in the GSM coordinate)<br> xpoint=0. & ypoint=0. & zpoint=0.<br> readf,lun,xpoint,ypoint,zpoint ;;;;(satellite pointing of SXI, aim point)<br> nthtmax=0L & nphimax=0L<br> readf,lun,nthtmax,nphimax ;;;;(number of the tht and phi grids)<br> thti=fltarr(nthtmax) & phii=fltarr(nphimax)<br> readf,lun,thti,format='(e14.6)' ;;;;(the tht grids)<br> readf,lun,phii,format='(e14.6)' ;;;;(the phi grids)<br> Pxraytp=fltarr(nthtmax,nphimax)<br> readf,lun,Pxraytp,format='(e14.6)' ;;;;(X-ray intensity)<br> close,lun<br> free_lun,lun</p>
3D Global MHD Simulation Data
<p>Particle in cell data are transformed to Matlab binary data.</p> <p>File </p> <p>273xyz.mat: xyz grid data </p> <p>273btotal.mat:pysical data </p> <p>Nx=241;<br>Ny=161;<br>Nz=161;</p> <p>start at [x0 y0 z0]=xyz(:,1,1,1) end at [X Y Z]=xyz(:,Nx,Ny,Nz)</p> <p> </p> <p> </p> <p> </p>
Data from: Multi-fluid MHD study of the disappearing solar wind event observed by MAVEN: Effects of solar wind density
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Data of 3D MHD Simulation for manuscript "Characteristics of Transpolar Arc Motion and its Corresponding Magnetospheric Dynamic Process"
<p>Data of 3D MHD Simulation for manuscript "Characteristics of Transpolar Arc Motion and its Corresponding Magnetospheric Dynamic Process"</p> <p>There are 6 types of data files:</p> <p>1) -3)MHD simulation results for FAC, plasma density, and temperature, projected at the x = -40RE position, with the viewpoint from the magnetotail towards the earth</p> <p>4) FAC mapping.rar. These data are the parametters in the plane of about Z=0 RE, which were mapped to the 7.2 Re, along the magnetic field lines.</p> <p>5) The simulation results of the model are plotted for FAC on Z=0RE.</p> <p>The results of the above data simulation plot are from 20171115 23:00 UT to 20171116 02:00 UT.</p> <p>6) XXBDd0142.rar, which is full 3D Simulation data at 2017.11.16 01:22 UT;</p> <p>All of these data include the following parameters:</p> <p>time, x, y, z, logrho, Vx, Vy, Vz, Bx, By, Bz, Pr, Jx, Jy, Jz, Edj</p> <p>7) SSUSI data at 2017.11.16.</p> <p> </p>
Simulation data from the three-dimensional multifluid MHD model of Najib et al. (2011)
<p>Simulation data from the three-dimensional multifluid MHD model of Najib et al. (2011).</p> <p>We use the data to study the ion escape at Mars.</p> <p> </p>
Global MHD simulation data for SWCX
<p>IDL> .run idlscript</p> <p>to produce Figs. 1, 3, and 4. Details can be found as comments in idlscript.pro.</p> <p>For 3D views in Fig. 2,</p> <p>$ paraview sbz.pvsm</p> <p>or</p> <p>$ paraview sbz_lowb.pvsm</p> <p>using paraview software.</p>
Data of 3D PPMLR-MHD model Simulation for manuscript "Formation and Evolution of Nightside Transpolar arc and Its Relationship with Energetic Plasma in the Magnetotail Lobe"
<p><span>Data of 3D PPMLR-MHD model Simulation for manuscript "Formation and Evolution of Nightside Transpolar arc and Its Relationship with Energetic Plasma in the Magnetotail Lobe"</span></p> <p><span>These data come from a fully run of a 3D MHD Simulation model that is named PPMLR-MHD model (detailed descriptions below).</span></p> <p><span>There are 2 types of data files:</span></p> <p><span>1) X15dXXXX.mat is saved simulation parameters. </span></p> <p><span>2) Xing15XXXX_heatflux.mat is saved heat flux from simulation parameters. </span></p> <p><span>XXXX is the number of files, and files with the same serial number correspond to the same time.</span></p> <p><span> </span></p> <p><span>The first type files of data include the following parameters:</span></p> <p><span>time, x, y, z, logrho, Vx, Vy, Vz, Bx, By, Bz, Pr, Jx, Jy, Jz</span></p> <p><span>Where, time is simulation time, which need to plus the start time to transfer them to universal time: time+16:00.</span></p> <p><span> (x,y,z) are the three components of the position of simulation point in GSM coordinates;</span></p> <p><span> logrho is the plasma density at the simulation point;</span></p> <p><span> (Vx, Vy,Vz) are the three components of plasma velocity at the simulation point in GSM coordinates;</span></p> <p><span> (Bx, By,Bz) are the three components of magnetic field at the simulation point in GSM coordinates;</span></p> <p><span> Pr is the plasma dynamic presure at the simulation point;</span></p> <p><span> (Jx, Jy,Jz) are the three components of plasma electric current at the simulation point in GSM coordinates;</span></p> <p><span> </span></p> <p><span>The second type file of data includes the simulated heat flux along the magnetic field lines at the simulation point in GSM coordinates. </span></p> <p><span>PPMLR-MHD model</span></p> <p><span>The PPMLR-MHD model is on the basis of an extension of the piecewise parabolic method (1) with a Lagrangian remap to magnetohydrodynamics (MHD) (2, 3). It is a three-dimensional MHD model, designed specially for the solar wind–magnetosphere–ionosphere system (4-6). The model possesses a high resolution in capturing MHD shocks and discontinuities and a low numerical dissipation in examining possible instabilities inherent in the system (4).</span></p> <p><span>The model uses a Cartesian coordinate system with the Earth’s center at the origin and X, Y, and Z axes pointing towards the Sun, the dawn-dusk direction, and the north, respectively. The size of the numerical box extends from 25 RE to –100 RE along the Sun-Earth line and from –50 RE to 50 RE in Y and Z directions, with 240×240×240 grid points and a minimum grid spacing of 0.2 RE. An inner boundary of radius 3 RE is set for the magnetosphere to avoid the complexities associated with the plasmasphere and large MHD characteristic velocity from the strong magnetic field (6). An electrostatic ionosphere shell with height-integrated conductance is imbedded, allowing an electrostatic coupling process introduced between the ionosphere and the magnetospheric inner boundary. The Earth’s magnetic field is approximated by a dipole field with a dipole moment of 8.06×1022 A/m in magnitude. The model is run to solve the whole system by inputting the real interplanetary conditions for the current event.</span></p>
MHD/PSD data: Simulation of Radiation Belt Wave-Particle Interactions in an MHD-particle Framework
<p>MHD and phase space density simulation results.</p>
Data Mining Inspired Localized Resistivity in Global MHD Simulations of the Magnetosphere
<p>The upload contains data for the paper submitted to the Journal of Geophysical Research.</p>
SuperDARN convection data and the 3D PPMLR-MHD simulation data on 27 February 2014
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