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75 results for “plasma waves”
Polar / Plasma Waves Investigation processed dataset and ephemeris used to produced the Smith et al. (2022) catalogue (doi:10.5281/zenodo.7260994 )
<p>This data set contains Polar / Plasma Waves Investigation processed using the SPACE Labelling Tool (Louis et al., 2022, doi:10.5281/zenodo.6886528). It also contains the Polar ephemeris in the geocentric solar ecliptic (GEO) coordinate system (from https://sscweb.gsfc.nasa.gov/cgi-bin/Locator.cgi)</p> <p>This processed dataset contains Auroral Kilometric Radiation (AKR) observations and was used to produced the Smith et al. (2022) catalogue of AKR (doi:10.5281/zenodo.7260994)</p> <p>This work has been funded by Science Foundation Ireland Grant 18/FRL/6199, and by a 2022 SCOSTEP/PRESTO<br> Grant.</p>
Transport Ratios for Plasma Waves Observed by MAVEN at Mars
<p>Transport ratios calculated for coherent plasma waves observed upstream from Mars by the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. These values were calculated by sub-sampling the ion velocity distribution measurements made by the Solar Wind Ion Analyzer (SWIA) instrument and binning them by the wave phase as estimated from the vector magnetic field measured by the Magnetometer (MAG) instrument. </p>
Plasma density turbulence obtained from a Hasegawa-Wakatani drift-wave turbulence model within the BOUT++ framework
<p>A Hasegawa-Wakatani drift-wave turbulence model [1] within the BOUT++ framework [2] was used to generate a set of turbulent plasma density profiles. Drift-wave turbulence is thought to be the dominant mechanism responsible for the anomalous transport observed in the edge of tokamak plasmas.</p> <p>The motivation to generate this rather large set of density profiles was to properly study the influence of plasma density fluctuations on traversing microwaves which requires ensemble-averaging to get statistically relevant results.</p> <p>The density data is given in normalized units (1.0 would correspond to 100 % fluctuation degree) on a mean-free background and the spatial coordinates are given in units of the ion Larmor radius.</p> <p>The form of equations used was the un-modified Hasegawa-Wakatani model [3]. Input parameters were kappa = 1.0 (normalised background density gradient), alpha = 0.5 (adiabaticity parameter), and diffusion constant D=1e-2.</p> <ol> <li>Wakatani, M., Hasegawa, A. (1984). <em>A collisional drift wave description of plasma edge turbulence.</em> Phys. Fluids <strong>27</strong>(3), 611. doi:10.1063/1.864660</li> <li>Dudson, B. <em>et al.</em> (2009). <em>BOUT++: A framework for parallel plasma fluid simulations</em>. Comp. Phys. Comm. <strong>180</strong>(9), 1467. doi:10.1016/j.cpc.2009.03.008</li> <li>Numata, R., Ball, R., & Dewar, R. L. (2007). <em>Bifurcation in electrostatic resistive drift wave turbulence</em>. Phys. Plasmas <strong>14</strong>(10), 102312. doi:10.1063/1.2796106</li> </ol>
Juno Plasma Wave Observations at Europa
<p>This is the supporting data set for the paper by the same title published in AGU JGR Space Physics.</p><p><strong>Abstract</strong><br>Juno passed by Europa at an altitude of 355 km on 29 September, day 272, 2022. As one of Juno's in situ science instruments, the Waves instrument obtained observations of plasma waves that are essential contributors to Europa's interaction with its environment. Juno observed chorus, a band at the upper hybrid frequency providing the local plasma density, and electrostatic solitary structures in the wake. In addition, impulses due to micron-sized dust impacts on Juno were recorded with a local maximum very close to Europa. The peak electron density near Europa was ∼ 330 cm−3 while the surrounding magnetospheric density was in the range of 50 to 150 cm−3. There was a significant separation between the Europa flyby and Juno's crossing of Jupiter's magnetic equator, enabling a unique identification of effects associated with the moon as opposed to magnetospheric phenomena normally occurring at the magnetic equator near 10 Jovian radii.</p>
Radio frequency wave interactions with a plasma sheath: the role of wave and plasma sheath impedances
<p>The accompanying files contain digital data for figures in the article "Radio frequency wave interactions with a plasma sheath: the role of wave and plasma sheath impedances" by J.R. Myra and H. Kohno, to be submitted to the journal Physics of Plasmas.</p> <p><br> Abstract:<br> RF sheaths form near surfaces where plasma and strong RF fields coexist. The effect of these RF sheaths on wave propagation near the boundary can be characterized by an effective sheath impedance that includes both resistive and capacitive contributions describing RF sheath rectification and RF power absorption in the sheath [J. R. Myra and D. A. D'Ippolito, Phys. Plasmas 22, 062507 (2015)]. Here we define a dimensionless parameter, the ratio of incoming wave impedance to the sheath impedance, which determines the characteristics of the interaction, ranging from quasi-conducting to quasi-insulating, or in the case of matched impedances, to a sheath-plasma resonance. A semi-analytical analysis is carried out for electrostatic slow waves in the ion cyclotron range of frequencies (ICRF). For the propagating slow wave case, where the incident wave is partially reflected, the fraction of power dissipated in the sheath is calculated. For the evanescent slow wave case, which admits a sheath-plasma resonance, an amplification factor is calculated. Using the impedance ratio approach, RF sheath interactions are characterized for a range of RF wave and plasma parameters including plasma density, magnetic field angle with respect to the surface, wave frequency and wave-vector components tangent to the surface. For a particularly interesting example case, results are compared with the rfSOL code [H. Kohno and J. R. Myra, Comput. Phys. Commun. 220, 129 (2017)]. Finally electromagnetic effects, absent from the semi-analytical analysis, are assessed.</p>
Datasets for "Relic gravitational waves from the chiral plasma instability in the standard cosmological model"
<pre>This directory contains an index.html file with links to the run directories and idl plotting routines with secondary data for the other figures for the paper "Relic Gravitational Waves from the Chiral Plasma Instability in the Standard Cosmological Model". If anything turns out to be incomplete, please email brandenb@nordita.org.</pre>
The linear dispersion relation of the electrostatic waves in magnetized anisotropic dysty plasma
<p>The linear and weakly nonlinear dust-ion-acoustic wave propagation obliquely with respect to an external magnetic field is studied in magnetized dusty plasma, which consists of magnetized fluid ions bearing with anisotropic pressure, suprathermal electrons, and static dust grains. In the linear regime, the magnetized dusty plasma supports the propagation of fast dust-ion-cyclotron (EDIC) mode and the slow electrostatic dust-ion-acoustic (DIA) mode.</p>
Dataset of "Particle simulation study of obliquely propagating whistler waves in low-beta plasmas"
<p>This dataset contain all necessary output data to make the plots contained in the article. It also includes parameter files to run simulations.<br><br>Dataset list:</p> <p>parameter files/*.py: Input parameter files<br>rms_amplitude.npz: RMS maximum wave amplitude for each run<br>run_1-distributions/*.npz: Electron distribution function at different moments.<br>run_1-Bz-*.npz: 2D Wave field or wave number spectrum data of run 1<br>run_1-freq_spectrum.npz: spacially averaged wave fequency spectrum of Bz<br>run_1-spectrogram.npz: wave Bz spectrogram recorded at y=0<br>scalars_run*.npz: raw scalar output of each run, containing wave and particle enegy profiles<br>summary_data.npz: a summary data containing info of each run (init paras, maximum wave amplitude, init linear growth rate, etc)<br>temperature_profile_run*.npz: the time evolution of parallel and perpendicular temerature of each run<br><br></p> <p>* Not all raw datas are included in this repository due to the limit of file size. One can directly contact the author for more detailed datas.</p>
Tail-Wave-Assisted Positron Acceleration in Nonlinear Laser Plasma Wakefields
<p>The data and vector diagrams of the results of positron trapping and acceleration when the initial parameters are modified.</p>
Complex Whistler-Mode Wave Features Created by a High Density Plasma Duct in the Magnetosphere
<p>Raytracing simulation trajectories (from "DenRay" code) for modeling an RBSP observation of a duct-like structure in the magnetosphere.</p> <p>The data is saved in MATLAB's '.mat' format. it contains the following variables:</p> <p>x: x- position of rays</p> <p>z: z- position of rays</p> <p>kx: x-component of whistler mode wavevector</p> <p>kz: x-component of whistler mode wavevector</p> <p>t: vector of times along ray trajectory</p> <p>The dataset includes 10,000 rays and 859 time steps per ray.</p> <p>Please contact Vijay Harid (vijay.harid@ucdenver.edu) for specifics on the simulation.</p>
Trifurcate structure of oxygen band EMIC waves excited in a warm magnetospheric plasma: Linear theory
<p>Simulation data of "Trifurcate structure of oxygen band EMIC waves excited in a warm magnetospheric plasma: Linear theory"</p>
Properties of whistler waves' ducting in plasmas with systems of small-scale density depletions. Simulation results.
<p><strong>Properties of whistler waves' ducting in plasmas with systems of small-scale density depletions. </strong><strong>Simulation results.</strong></p> <p>The results of numerical FDTD simulations for the paper entitled "Properties of Whistler Waves’ Ducting in Plasmas With Systems of Small-scale Density Depletions" by Zudin I.Yu. et al.</p> <p>All files stored here are vectors or matrices coefficients presented in the text format and space symbol separated. "loadtxt" function from "numpy" library can be used for the data loading by a Python user. Each folder corresponds to a figure with the same number. The data stored in "data.zip" archive сontaining the following folders.</p> <p><strong>Fig2 folder</strong></p> <p>All files are the solutions of the dispersion equations wrote in the paper. Each of file consist in two columns. First column is the density depletion width</p> <p>(in meters), and second column is wavenumber <span class="math-tex">\(p\)</span></p> <ul> <li>"even_0.dat", "even_1.dat" ... are the fist, the second etc. even modes of the plain depletion.</li> <li>"odd_0.dat", "odd_1.dat" ... are the fist, the second etc. odd modes of the plain depletion.</li> <li>"m=0_0.dat", "m=0_1.dat" ... are the fist, the second etc. brunches of the modes of the cylindrical depletion with azimuth number m=0.</li> <li>"m=+1_0.dat", "m=+1_1.dat" ... are the fist, second the etc. modes of the cylindrical depletion with azimuth number m=1.</li> <li> "m=-1_0.dat", "m=-1_1.dat" ... are the fist, second the etc. modes of the cylindrical depletion with azimuth number m=-1.</li> </ul> <p><strong>Fig3 folder</strong></p> <p>All files are the dependences of normalized localization scale <span class="math-tex">\(\delta / d\)</span> from <span class="math-tex">\(d\)</span>. Each of file consist in two columns. The first one is the density depletion width <span class="math-tex">\(d\)</span> (in meters), and the second column is <span class="math-tex">\(p\)</span>.The files is named in such a manner as in Figure2 folder.</p> <p><strong>Fig5 folder</strong></p> <p>"Ex.dat", "Ey.dat" and so on are the amplitudes of electric and magnetic field components presented in Figure #5 of the paper. "Ne.dat" is simulated density profile at z=60 km, as in above the file consists in two columns. The first is the</p> <p>coordinate and the second is the density. "xgrid.dat" and "zgrid.dat" are Cartesian coordinates of the grid's nodes used for field representation. So Ex(x[i],z[j])=Ex[j,i]</p> <ul> <li>units of plasma density is "m(-3)"</li> <li>units of electrical field components is "mkV/m"</li> <li>units of magnetic field components is "pT"</li> <li>units of Cartesian coordinates is "km"</li> </ul> <p>The grid used for the data presentation is less detailed than that used for actual simulation.</p> <p><strong>Fig6 folder</strong></p> <p>The same description as for Fig5 folder.</p> <p><strong>Fig7 folder</strong></p> <p>"subdecameter.Sz.dat", "subdecameter.Sx.dat", "subhectometer.Sz.dat", and "subhectometer.Sz.dat" are the Pointing vector projections calculated in the cases of subdecameter and subhectometer depletions. "xgrid.dat", "zgrid.dat" are the coordinates of the grid's nodes. "subdecameter.Ne.dat" and "subhectometer.Ne.dat" is is simulated density profiles of systems of subdecameter and subhectometer depletions. The files ogranized in such mannar as in Figure5 folder. The grid used for the data presentation is less detailed than that used for actual simulation.</p> <ul> <li>units of plasma density is "m(-3)"</li> <li>units of energy flux is "mkW/m(2)"</li> <li>units of Cartesian coordinates is "km"</li> </ul> <p><strong>Fig8 folder</strong></p> <p>"subdecameter.Sz.dat", "subdecameter.Sz.dat" are the Pointing vector projections calculated in the cases of subdecameter and subhectometer depletions. "subhectometer.Ex.dat", and "subhectometer.Ex.dat" are the amplitudes of the electric field component. "xgrid.dat", "zgrid.dat" are the coordinates of the grid's nodes. "subdecameter.Ne.dat" and "subhectometer.Ne.dat" is is simulated density profiles of systems of subdecameter and subhectometer depletions. The files organized in such manner as in Figure5 folder. The grid used for the data presentation is less detailed than that used for actual simulation.</p> <ul> <li>units of electrical field components is "mkV/m"</li> <li>units of plasma density is "m(-3)"</li> <li>units of energy flux is "mkW/m(-2)"</li> <li>units of Cartesian coordinates is "km"</li> </ul> <p><strong>Fig9 folder</strong></p> <p>"subhectometer.Ex.dat", "subhectometer.Ex.dat" etc. are the profiles along <span class="math-tex">\(x\)</span> of the components of the electric field and the plasma density. The files organized in such a manner. First column is coordinates values, the second one is the field component or density value.</p> <ul> <li>units of plasma density is "m(-3)"</li> <li>units of electrical field components is "mkV/m"</li> <li>units of Cartesian coordinates is "km"</li> </ul> <p><strong>Fig10 folder</strong></p> <p>"subhectometer.Ex.dat", "subhectometer.Ex.dat" are the 2d-spectrums of the <span class="math-tex">\(E_x\)</span> complex amplitude in the cases of subhectometer and subdecameter depletions. "kx_grid.dat" and "kz_grid.dat" are the Cartesian coordinates of the grid's nodes used for spectrums representation.</p> <ul> <li>units of electrical field components is "mkV/m km(2)"</li> <li>units of Cartesian coordinates is "km(-1)"</li> </ul> <p><strong>Fig11 folders</strong></p> <p>"subhectometer.Ex.dat", "subhectometer.Ex.dat", and "smoothed.Ex.dat" are the 1d spectrums presented on the Figure #11 the cases of subhectometer, subdecameter and smoothed depletions.</p> <ul> <li>units of electrical field components is "mkV/m km"</li> <li>units of Cartesian coordinates is "km(-1)"</li> </ul> <p><strong>Fig12 folders</strong></p> <p>"subhectometer.Ex.dat", "subhectometer.Ex.dat", and "smoothed.Ex.dat" are the 1d spectrums presented on the Figure #12 the cases of subhectometer, subdecameter and smoothed depletions.</p> <ul> <li>units of electrical field components is "mkV/m km"</li> <li>units of Cartesian coordinates is "km(-1)"</li> </ul> <p> </p>
A Randomized Controlled Trial of Ultrasound-guided Platelet-Rich-Plasma (PRP) Injection Versus Extracorporeal Shock Wave Therapy (ESWT) for Great Trochanter Pain Syndrome (GTPS) With Gluteus Medius or
ClinicalTrials.gov study NCT03774251. IPD Sharing: NO. Countries: 1. Publications: 9.
Effect of Extracorporeal Shock Wave Combined With Autologous Platelet-rich Plasma Injection on Rotator Cuff Calcific Tendinitis
ClinicalTrials.gov study NCT06372600. IPD Sharing: NO. Countries: 0. Publications: 1.
Hidden quasiperiodic attractors of six types for ion-acoustic waves in a magnetized Thomas-Fermi plasma.
<p>The figures (a) and (b) represent coexisting hidden quasiperiodic attractors of six different types for ion-acoustic<br> waves with f<sub>0 </sub>= 3.96 and f<sub>0 </sub>= 6.5 in a magnetized Thomas-Fermi plasma.</p>
Dataset for "The Emergence of inertial waves from coherent vortex source in strongly coupled dusty plasma"
<p><strong>fig1.zip:</strong> This zip file contains three folders of data for \Gamma=9, 50, and 110 to plot fig.1.</p> <p>Each folder has two data files namely QUIVER_time_30 and QUIVER_time_60 correspond to time t=30 and 60, respectively. To plot vorticity, position and velocities along the x-axis, y-axis, and corresponding vorticity are required. In QUIVER_time_* files, the first five columns are x-position, y-position, velocity along the x-axis (v<sub>x</sub>), velocity along the y-axis (v<sub>y</sub>), and vorticity.</p> <p> </p> <p><strong>fig2.zip:</strong> fig2.zip folder has data file for time_1, time_5, time_8, time_10. Each time_* files contain five columns. They are as follows:</p> <p>Col-1: Serial number</p> <p>Col-2: x-position</p> <p>Col-3: y-position</p> <p>Col-4: velocity along the x-axis (v<sub>x</sub>)</p> <p>Col-5: velocity along the y-axis (v<sub>y</sub>)</p> <p>Plotting script is given insider the folder.</p> <p> </p> <p><strong>fig3.zip: </strong>fig3.zip folder has STATE file for various initial velocity U<sub>0</sub>. Each STATE_* files contain five columns. They are as follows:</p> <p> </p> <p>Col-1: Serial number</p> <p>Col-2: x-position</p> <p>Col-3: y-position</p> <p>Col-4: velocity along the x-axis (v<sub>x</sub>)</p> <p>Col-5: velocity along the y-axis (v<sub>y</sub>)</p> <p> </p> <p>Plotting script is given insider the folder.</p> <p> </p> <p><strong>fig4.zip: </strong>This zip file contains four folders of data for \kappa=0.5, 1.0, 2.0, and 5.0 to plot fig.4.</p> <p>Each folder has 151 data files, namely QUIVER_time_*, which corresponds to various times. To plot wave propagation, position, and velocities along the x-axis, the y-axis is required. In QUIVER_time_* files, the first five columns are x-position, y-position, velocity along the x-axis (v<sub>x</sub>), velocity along the y-axis (v<sub>y</sub>), and vorticity.</p> <p><strong>fig5.txt:</strong> Data file has various rows. They are as follows:</p> <p>Row-1: Various \kappa values</p> <p>Row-2: Longitudinal sound speed</p> <p>Row-3: Transverse sound speed</p> <p>Row-4: Various \kappa values to plot C<sub>NLW </sub>for various initial velocities vs \kappa values</p> <p>Row-5 to 11: Speed of nonlinear wave C<sub>NLW</sub> for various initial velocities U<sub>0</sub>=0.1, 0.35, 0.75, 1.5, 2.5, 3.5, 5.0.</p> <p> </p> <p><strong>fig6.txt:</strong> First and second rows correspond to Mach numbers and maximum amplitude of absolute value of nonlinear wave velocity along x-direction (v<sub>x</sub>), respectively.</p> <p> </p> <p> </p>
Phase portrait and potential energy function of the dynamical system corresponding to modified ZK equation for ion-acoustic waves in a magnetized electron-ion plasma with generalized (r, q) distributed electrons
<p>These figures (a) and (b) represent phase portrait and potential energy function of the dynamical system corresponding to the mZK equation for ion-acoustic waves in a magnetized electron-ion plasma with generalized (r, q) distributed electrons for q = 5 and r = 0.1. These figures contain three fixed points P<sub>0,</sub> P<sub>1 </sub>and P<sub>2</sub> with one separatrix. The figure (a) contains one family of supernonlinear periodic orbits, two families of periodic orbits and one pair of homoclinic orbits at P<sub>0. </sub>The figure (b) contains the potential energy function with two local minima and one maxima which is necessary condition for supernonlinear wave. </p>
Resonant excitation of plasma waves in a plasma channel - data
Open the record for dataset details and reuse information.
Data of "Saturation properties of whistler wave instability in a plasma with two electron components"
<p>Data of 1D particle simulation results, containing energy and temperature data.</p>
Data from Vlasov Plasma Waves solver Kinetic Alfven Waves Solutions in the inner magnetosphere
<p>Dispersion analysis output files for plasma waves propagating, at different L-shells and different propagation angles, in the inner magnetosphere considering multi-species and also electron-proton plasma. All data correspond to frequency and plasma wave diagnostic spectra as a function of wavenumber.</p> <p>Data includes:</p> <p>complex frequency</p> <p>polarization</p> <p>magnetic helicity</p> <p>magnetic compressibility </p> <p>electric field </p> <p>magnetic field</p>
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Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
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.