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68 results for “MHD”
MHD simulation results for the investigation of FTEs
<p>The unit of data:</p> <p>Length unit, like x, y z, is Re(the radius of the Earth).</p> <p>The unit of magnetic field data is nT.</p> <p>The unit of velocity is km/s.</p> <p>The unit of density is cm^-3.</p> <p>The unit of pressure is nPa.</p> <p><strong>1</strong>.'no2_bn_mp_betsuni_topo_halfopen_17_r0.dat ' contains the magnetic field and some plasma data on the surface of magnetopause in full time step(201 time steps) of case 2.</p> <p>This is a binary data, and you can read it as follows"</p> <p>read,ntht,nphi (ntht,nphi are integers)</p> <p>define xmp,ymp,zmp as the two dimension array (ntht,nphi)</p> <p>read,xmp,ymp,zmp (xmp,ymp,zmp is the coordinates of points, the unit is Re) </p> <p>define bn,bl,bm,p_1,b_mag,vx_1,d_1 (these are 2 dimensional arrays (ntht, nphi))</p> <p>begin the loops for i=0,200</p> <p>read,time(this is the time , you need to multiply 0.935 to get the physical time. For example, if the value of time you read is 680, then the physical time is 680*0.935)</p> <p>read, bn,bl,bm,p_1,b_mag,vx_1,d_1 (bn,bl,bm are the magnetic field data,p_1 is pressure, vx_1 is the magnitude of velocity,d_1 is the density)</p> <p>endfor</p> <p><strong> 2</strong>. 'S05D07V750B0013-13bt_cut_large_bipolar_bt119 ' , 'S05D07V750B0013-13bt_cut_large_bipolar_bt120' and 'S05D07V750B0013-13bt_cut_large_bipolar_bt121' are the data in 3d of case2 in 119th(2225.3s),120th(2244s) and 121th(2262.7s) time step separately.</p> <p>These are binary data, you can read as follows:</p> <p>read,m,n,l (m,n,l are integers)</p> <p>define, x,y,z as 1 dimensional array, x(m), y(n), z(l)</p> <p>read,,x,y,z</p> <p>define d,vx,vy,vz,bx,by,bz,p,tracer as 3 dimensional arrays, like d(m,n,l). d is density, vx is the velocity of x axis, vy is the velocity of y direction, vz is the velocity of z axis, bx, by and bz are the magnetic field in x, y, z, p is pressure. tracer is the percentage of solar wind particles. </p> <p>read,d,vx,vy,vz,bx,by,bz,p,tracer</p> <p><strong>3</strong>.S05D07V750B0013-13bt_cut_large_bipolar_bt121.silo is a 3 dimensional data which can be opened and plotted by Visit.</p> <p><strong>4</strong>.no1_bn_mp_betsuni_topo_half_r0_178.dat and no3_bn_mp_betsuni_topo_half_1120_34.dat contains the magnetic field and some plasma data on the surface of magnetopause in only one time step of case 1 and case3.</p> <p>The time step of case1' s data is 178th, that is 3328.6s.</p> <p>The time step of case3' s data is 34th, that is 635.8s.</p> <p>These are binary data, you can read the data as follows:</p> <p>read,ntht,nphi ( these are integers)</p> <p>define xmp,ymp,zmp as 2 dimensional arrays, like xmp(ntht,nphi)</p> <p>read, xmp,ymp,zmp</p> <p>read, time( if you want to get the physical time point, you should calculate 0.935*time)</p> <p>define bn,bl,bm,p_1,b_mag,vx_1,d_1 as 2 dimensional arrays, like bn(ntht,nphi)</p> <p>read,bn,bl,bm,p_1,b_mag,vx_1,d_1</p> <p><strong>5</strong>. S05D48V300B0033-33bt_cut_large_bipolar37 , S05D07V750B0013-13bt_cut_large_bipolar_bt37 and S05D03V1200B0008-08bt_cut_large_bipolar_bt37 are the data in 3 dimension of case1 ,2 and 3 in the 37th(691.9s) time step separately.</p> <p>These data are the binary data and you can read these as the steps shown in 2.</p>
Fine Structures in Interlaced Magnetic Flux Ropes via Hall-MHD simulations
<p>This data set contains data files used for Figures 1-7 of paper "Fine structures in interlaced magnetic flux ropes via Hall-MHD simulations," AIP Advances, January 2025, American Institute of Physics,<br>DOI: <span>10.1063/5.0238316.</span></p> <p>Each file is zip compressed ascii format.</p> <p>Each file has a header to describe the contents:</p> <p>Each file is a 3-d model output that contains the following variables in columns:</p> <p>"X [R]" "Y [R]" "Z [R]" "Rho [amu/cm^3]" "U_x [km/s]" "U_y [km/s]" "U_z [km/s]" "B_x [nT]" "B_y [nT]" "B_z [nT]" "P [nPa]"</p> <p>File name contains the time of each result: 02h indicates t=2 hours stimulation time.</p> <p>Each number is a 7-digit accuracy floating number.</p> <p> </p>
The Structure of the Cusp Diamagnetic Cavity and Test Particle Energization in the GAMERA Global MHD Simulation
<p>CHIMP test particle simulation data. The data set is described in the supporting information from the publication "The Structure of the Cusp Diamagnetic Cavity and Test Particle Energization in the GAMERA Global MHD Simulation"</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>
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>
Datasets for "Polarization of gravitational waves from helical MHD turbulent sources"
<p>The tar archive helical.tar contains the run directories for each run<br> in Table 1 and the figures of the paper "Polarization of gravitational<br> waves from helical MHD turbulent sources", https://arxiv.org/abs/2107.05356.<br> by A. Roper Pol, S. Mandal, A. Brandenburg, and T. Kahniashvili.<br> The run directories, the plots, and the code to generate the plots can be<br> found in https://github.com/AlbertoRoper/GW_turbulence.</p>
3D MHD Simulations of Magnetospheres from Obliquely Rotating Magnetic Massive Stars
<p>We present results from the first 3D MHD simulations of the stellar-wind-fed magnetospheres from massive stars with a dipole magnetic axis that has an arbitrary obliquity angle (<span class="math-tex">\(\beta\)</span>) to the star’s rotation axis. As an initial direct application, we examine the global structure of co-rotating disks for tilt angles <span class="math-tex">\(\beta =\)</span> 0, 45 and 90 degrees using <span class="math-tex">\(\zeta\)</span> Pup stellar parameters as a prototype. We find that for models with rapid stellar rotation (~0.7 critical rotation), accumulation surfaces closely resemble the form predicted by the analytic Rigidly Rotating Magnetosphere (RRM) model, but with a mass distribution and outer disk termination set by centrifugal breakout processes. Moreover, models with low stellar rotation rates show a far more variable and complex structure than simple predictions. These models can be used to synthesize rotational modulation of photometric absorption and H-alpha emission for a direct comparison with observations.</p>
GAMERA Global MHD: ideal simulations
<p>Grid Agnostic MHD for Extended Research Applications (GAMERA) global terrestrial magnetohydrodynamic simulation outputs at 1 minute resolution Each simulation covers 1 hour. Files contain grid information and MHD variables. Variable names can be read as h5 attributes.</p>
Dataset and Python Scripts used in the manuscript "Global-MHD Simulations using MagPIE : Impact of Flux Transfer Events on the Ionosphere"
<p>Dataset and Python Scripts used in the manuscript "Global-MHD Simulations using MagPIE : Impact of Flux Transfer Events on the Ionosphere".</p> <p>Authors: Arghyadeep Paul, Antoine Strugarek and Bhargav Vaidya<br> Date: 21 May, 2023</p> <p> </p> <ul> <li>Figure 1 has been plotted from two data files named Bx_By_Bz_prs_t_4783_C0.vtk and Bx_By_Bz_prs_t_4783_C1.vtk using the visualisation toolkit VisIt. Visit can be freely downloaded from https://wci.llnl.gov/simulation/computer-codes/visit</li> <li>Figure 2 has been plotted using the ipython notebook named "figure_2.ipynb" and the associated data files have been uploaded alongwith.</li> <li>Figure 3 has been plotted using the data file named "visit_prs_Bx_By_Bz_t_4964s.vtk" and the visualisation toolkit VisIt.</li> <li>Figure 4 has been plotted using the associated data files and the visualisation toolkit VisIt.</li> <li>Figures 5 and 6 has been plotted using the ipython notebook named "new_fig_5_and_6.ipynb" and the associated data files have been uploaded alongwith.</li> <li>Figure 7 has been plotted using the ipython notebook named "figure_7.ipynb" and the associated data files have been uploaded alongwith.</li> <li>Figure 8 has been plotted using the ipython notebook named "figure_8.ipynb" and the associated data files have been uploaded alongwith.</li> <li>Figure 9 has been plotted using the ipython notebook named "figure_9.ipynb" and the associated data files have been uploaded alongwith. An example swarm CSV data file is added for the python script. The original SWARM data can be downloaded from <a href="https://swarm-diss.eo.esa.int/">https://swarm-diss.eo.esa.int/</a> and the FAC data from two spacecrafts, Swarm A and C, named SW_OPER_FAC_TMS_2F has been used. This data was first published in Dong et.al. 2023 [https://doi.org/10.1029/2022GL102460].</li> </ul>
Grad-Shafranov equation: MHD simulation of the new solution obtained from the Fadeev and Naval models
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Comprehensive comparison of two global multi-species MHD models of Mars
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Data from: Multi-fluid MHD study of the disappearing solar wind event observed by MAVEN: Effects of solar wind density
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Simulation output from "Multiscale MHD-Kinetic PIC Study of Energy Flux Caused by Reconnection"
<p>Results from an implicit particle-in-cell simulation (IPIC3D) of the energy fluxes from magnetic reconnection in Earth's magnetotail. The results consist of six files in HDF5 format that contain the electric field, magnetic field, the density, velocity and energy flux. Each file contains one time step. </p> <p>The IPIC3D simulation is described in</p> <p>Markidis, S., Lapenta, G. and Rizwan-uddin (2010) Multi-scale simulations of plasma with IPIC3D . Mathematics and Computers and Simulation, 80, 1509-1519.</p> <p>The energy conserving version of IPIC3D used in this study is described in</p> <p>Lapenta, G., (2017) Exactly energy conserving semi-implicit particle in cell formulation, J. Computational Physics, 334, 349-366.</p> <p>The application of IPIC3D to Earth's magnetosphere is described in </p> <p>Walker, R., Lapenta, G., Berchem, J., El-Alaoui, M., and Schriver, D., (2019) Embedding particle-in-cell simulations in global magnetohydrodynamic simulations of the magnetosphere, Journal of Plasma Physics, 85(1). </p>
The effect of pre-existing islands on disruption mitigation in MHD simulations of DIII-D
<p>Data underlying all figures. </p>
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>
Dataset for Sakata et al. (2024) "Effects of an Intrinsic Magnetic Field on Ion Escape from Ancient Mars Based on MAESTRO Multifluid MHD Simulations"
<div> <p>This dataset contains the simulation results in Sakata et al. (2024), Effects of an Intrinsic Magnetic Field on Ion Escape from Ancient Mars Based on MAESTRO Multifluid MHD Simulations, Journal of Geophysical Research: Space Physics.</p> </div>
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>
Non-ideal MHD chemodynamical simulations
<p>Non-ideal MHD chemodynamical simulations for various physical parameters (described in title and accompanying paper) at a central density of n(H2) = 10^6 cm^-3</p>
Transport and distribution of sodium ions in Mercury's magnetosphere: results from multi-fluid MHD simulations
<p>This dataset contains VTK files of the four simulations that are presented in the paper<em> </em><a href="https://essopenarchive.org/doi/full/10.22541/essoar.171629607.76912814/v1">Transport and distribution of sodium ions in Mercury’s magnetosphere: results from multi-fluid MHD simulations</a> .</p> <p>The physical parameters for each of the simulations are summarized below:</p> <div> <div>Sim-1: IMF = [0,0,-8.5] nT, V_sw = [-400,0,0] km/s</div> <div>Sim-2: IMF = [0,0,-8.5] nT, V_sw = [-400,0,0] km/s</div> <div>Sim-3: IMF = [0,0,-8.5] nT, V_sw = [-400,0,0] km/s</div> <div>Sim-4: IMF = [-15.2,8.4,-8.5] nT, V_sw = [-400,50,0] km/s</div> <div> <div> </div> <div>The Hall term is switched off in sim-2, but switched on in the rest of the simulations. The sodium source is used in all the simulations except for sim-3. In all the simulations, the solar wind density is 40 amu/cc with a temperature of 7.5 eV. We refer the readers to the aforementioned paper for more details.</div> </div> </div> <p>These VTK files can be opened with Paraview.</p>
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International Brain Laboratory public data
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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.