Find research datasets worth reusing

opencc-by-4.0Feb 2020View details →

Reconnection rates of the paper "Simulation of plasmaspheric plume impact on dayside magnetic reconnection"

This repository contains the dataset needed for the paper "Simulation of plasmaspheric plume impact on dayside magnetic reconnection", i.e. the magnetic reconnection rates at each time and the quantities needed to normalize them. All the data are stored in the file "rates_norm.h5". The file "si_content.pdf" explain how the data are stored and how you can extract them.

opencc-by-4.0Dec 2020View details →

Three-dimensional magnetic reconnection in particle-in-cell simulations of anisotropic plasma turbulence (Simulation Data)

This folder contains the output of the following simulation:  We use the explicit Plasma Simulation Code (PSC, Germaschewski et al.2016) to simulate eight anisotropic counter-propagating Alfvén waves in an ion-electron plasma. The anisotropy of the initial fluctuation is set up according to the theory of critical balance by Sridhar & Goldreich (1994) and Goldreich & Sridhar (1995) at the small scale end of the inertial range: $k_{\parallel} d_{i} = C (|k_{\perp}|d_{i})^{2/3}$, where $C= 10^{-4/3}$. The normalization parameters are the speed of light $c = 1$, the vacuum permittivity $\epsilon_{0} = 1$, the magnetic permeability $\mu_{0} = 1$, the Boltzmann constant $k_{b}=1$, the elementary charge $q=1$, the ion mass $m_{i}=1$, the density of ions and electrons $n_{i}=n_{e}=1$ and the ion inertial length $d_{i}=c/\omega_{pi}$ where $\omega_{pi}=\sqrt{n_{i}q^{2}/m_{i}\epsilon_{0}}$ is the ion plasma frequency. We set $\beta_{s,\parallel}=1$ and $T_{s,\parallel}/T_{s,\perp}=1$, where $\beta_{s,\parallel}=2 n_s \mu_{0} k_{B}T_{s,\parallel}/B_{0}^{2}$ is the ratio between the plasma pressure parallel to the background magnetic field $\mathbf{B}_{0}$ and the magnetic pressure and $T_{s,\parallel}$ is the parallel temperature. The magnetic field is normalised to $B_{0}=V_{A}/c$,  where $V_{A}=B_{0} / \sqrt{\mu_{0}n_{i}m_{i}}$ is the ion Alfvén speed. We use 100 particles per cell (100 ions and 100 electrons), a mass ratio of $m_{i}/m_{e} = 100$ so that $d_e = 0.1 d_{i}$ where $m_{e}$ is the electron mass and $d_{e}$ is the electron inertial length. The simulation box size is $L_{x} \times L_{y} \times L_{z} = 24d_{i}\times24d_{i}\times125d_{i}$ and the spatial resolution is $\Delta x =\Delta y = \Delta z = 0.06d_{i}$. We use a time step $\Delta t =0.06/ \omega_{pi}$. In our normalisation, the Debye length $\lambda_{D}=d_{i}\sqrt{\beta_{i}/2}V_{A}/c$ defines the minimum spatial distance that needs to be resolve in the simulation and $\lambda_D=0.07d_i$. This output corresponds to $t=120 \omega_{pi}$.  These data were produced using the Data Intensive at Leicester (DIaL) facility provided by the DiRAC project dp126 "Identifying and Quantifying the Role of Magnetic Reconnection in Space Plasma Turbulence".

opencc-by-4.0Dec 2023View details →

Parker Solar Probe Reconnection Exhaust Data Set for Close Encounters 4-11

The data set contained in the ascii text files consist of the current sheet (CS) time intervals and the associated parameters of identified magnetic reconnection exhausts across CSs recorded by the Parker Solar Probe within R<0.26 AU from the Sun for close encounters 4-11. A detailed description is available in a manuscript submitted to The Astrophysical Journal by Eriksson et al. [2024] entitled "Parker Solar Probe Observations of Magnetic Reconnection Exhausts in Quiescent Plasmas Near the Sun".The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_tctr.txt contains a center time of the optimized Walen relation (tc, column 1) and columns 2-3 show the CS start (CS1) and end (CS2) times. This is followed by the time duration dtcs in seconds (column 4) and whether a SPAN-I instrument survey (s=sf00) or burst (a=af00) data product exist (column 5). The RTN components of the adjacent  time averaged magnetic field before (B1_R, B1_T, B1_N) and after (B2_R, B2_T, B2_N) the CS then follows in columns 6-11 and a corresponding magnetic field rotation angle (Bshear1) at the CS (column 12). The CP dL, dM, dN columns 13-15 list the distances covered along the hybrid-LMN coordinate system based in a Cross-Product normal to the CS in terms of the average ion inertial length diavg (column 16), which is based on a non-corrected proton density (Np1+Np2)/2=Npavg (columns 17-19). The subsequent columns 20-28 are the adjacent VL,VM,VN on the two sides of the CS from the MVAB LMN system as well as their averages (VL1+VL2)=VLavg, (VM1+VM2)/2=VMavg and (VN1+VN2)/2=VNavg. This is followed (columns 29-37) by the corresponding VL,VM,VN and averages in the hybrid-LMN system using the cross-product (CP) normal. The adjacent average total magnetic field Btot1 and Btot2 (columns 38-39) and the LMN components of the magnetic field in the MVAB system [BL1, BL2], [BM1, BM2], [BN1, BN2] in columns 40-45 are followed by the corresponding magnetic fields in the CP hybrid-LMN system (columns 46-51). The ratio of the intermediate to minimum eigenvalue ratio is included (column 52) followed by the unit vectors of the MVAB system L=[L_R, L_T, L_N], M=[M_R, M_T, M_N], and N=[N_R, N_T, N_N] in columns 53-61. The times adjacent to the CS used to obtain this set of MVAB eigenvectors is found in columns 62-63 (MVAB UT1 and MVAB UT2). The magnetic fields (B1 and B2) used to obtain the local hybrid-LMN system relative these MVAB times relatively farther from the CS are associated with a rotation angle (Bshear2) in column 64. The local hybrid-LMN system from the CP normal is then listed in columns 65-73  LCP=[L_R, L_T, L_N], MCP=[M_R, M_T, M_N], NCP=[N_R, N_T, N_N]. The angle (degrees) between the MVAB N and NCP is listed in column 74 (Nmv*Ncp) followed by the last two columns 75-76 that contain the time interval (s) relative CS1 and CS2 to obtain average plasma data (dext) and magentic field data (bext).A letter "m" right before column 1 flags the five events in this list of 236 events when the magnetic field did not change sign across the assumed CS. A letter "d" marks the 10 events associated with two opposite (double) exhausts.The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_qtn.txt contains the same current sheet (CS) start (CS1) and end (CS2) times (columns 1-2). This file also lists the adjacent average proton (non-corrected) density in columns 3-4 as in the first (tctr) file which is followed by the average proton temperatures (Tp1 and Tp2 in columns 5-6), solar wind speed (Vtot1 and Vtot2 in columns 7-8) and the hybrid system L-components of the velocity (VL1 and VL2 in columns 9-10). Columns 11-16 contain the minimum and maximum values within each CS of the non-correct proton density, proton temperature and VL component. Column 17 lists the daily median density ratio from the electron density (Ne) and the non-corrected proton density (Np) where Ne is obtained through quasi-thermal noise spectroscopy by Kruparova et al. (2023). Column 18 lists the average of this daily ratio. Column 19 lists a value fc. A value larger than 1.0 indicates that a CS event time period is corrected to a local Ne value using Npfc=(Ne/Np)*Np*fc, where Np is a non-corrected proton density, Ne/Np is the median of the daily Ne/Np ratio.The ascii data file zenodo_psp_ce_lmn_cs_output_sorted_positions.txt contains the Parker Solar Probe median of its radial position within each CS1-CS2 time period in both solar radius and astronomical unit.The PDF figures psp_ceXX_apj_plots_qtn_final.pdf for XX=04,05,06,07,08,09,10 and 11 contain all CS events with a reconnection exhaust for each close encounter 04-11 on the basis of the agreement with a Walen prediction. Each plot shows the pitch-angle distribution (0-180 degrees) of the supra-thermal energy flux, proton temperature (MK), proton density (black) corrected to a daily median ratio Ne/Np as Npcorr=(Ne/Np)*Np, where Ne (red dots) is obtained from a QTN analysis by Kruparova et al. (2023), L-components of the magnetic field and proton velocity with a red trace showing a Walen prediction to this VL across the CS, the M and N components of the magnetic field with BM shifted by its time-period average, and the M and N components of the proton velocity with VM shifted by its time-period average. The LMN unit vectors of the employed hybrid LMN system are shown below each plot for reference.Finally, the eight ~11-day overview plots for each close encounter 4-11 marks the center times (tc) of each confirmed exhaust interval in this study of 231 events (red vertical dotted line) with the five marginal events marked as a black vertical dotted line. The panels from the top show the pitch-angle distribution (0-180 degrees) of the supra-thermal energy flux, proton temperature (MK), magnetic field strength, R-components of B and V, N-components of B and V, and the radial postion of Parker Solar Probe in terms of the solar radius. Here, R and N are two of the three RTN system components of B and V.

opencc-by-4.0Aug 2024View details →

Data for "Impact of the Out-of-Plane Flow Shear on Magnetic Reconnection at the Flanks of Earth's Magnetopause"

Data for Figures 3-8 in the paper (data for Figures 5 has been updated on 2024-09-20). The data is compatible with all data-analysis software. Here are the guidelines for reading and visualizing the data: (1) The filenames "noshear", "MA0p7", and "MA2p3" correspond to the simulation runs with no flow shear, Mach number M_A=0.7 flow shear, and M_A=2.3 flow shear. (2) The "upper" and "lower" mean upper and lower current sheet, corresponding to dusk-side and dawn-side reconnection respectively. For the "noshear" case, only the "upper" is considered. (3) Each data file (*.dat) is written in ASCII format and has multiple columns. The first row is the header. <ul> <li>The first column is always the x-coordinates of the figure. </li> <li>For the line plots, all columns starting from the second column are the y-coordinates for different variables. The variables names can be found at the header. </li> <li>For the 2D image plots, the second column is the y-coordinates, and the third column is the value of the variable at a given (x,y) location. </li> </ul> (4) The files "fig4_*_field_*.dat" are the magnetic potential in the x-y domain. The contour of this potential gives the in-plane field line configurations.

opencc-by-4.0Dec 2023View details →

Data and Software for "Determining the orientation of a magnetic reconnection X line and implications for a 2D coordinate system"

Supporting information for "Determining the orientation of a magnetic reconnection X line and implications for a 2D coordinate system", by Denton et al. Includes a copy of the paper and previous relevant papers, the simulation data used in the paper, and the reconstruction code used in the paper. See the readme files.

opencc-by-4.0Oct 2024View details →

The spreading of magnetic reconnection X-line in particle-in-cell simulations– mechanism and the effect of drift-kink instability

This dataset contains data and Python scripts in "The spreading of magnetic reconnection X-line in particle-in-cell simulations– mechanism and the effect of drift-kink instability" prepared to submit to the Journal of Geophysical Research.

opencc-by-4.0Feb 2023View details →

Data files of the paper "Energy conversion by magnetic reconnection in multiple ion temperature plasmas"

Reconnection rate and energy budget files for the simulations used in for the paper "Energy conversion by magnetic reconnection in multiple ion temperature plasmas". The paper has two simulations. The first one, without cold ions, has his reconnection rate data stored in "rate_147.dat" and the energy budget data in "Ebudget_symm_nocold_Xframe.h5". The second one, with cold ions, has his reconnection rate data stored in "rate.dat" and the energy budget data in "Ebudget_symm_cold_Xframe.h5". On top of that is a datafile from simulation 1 at time 144.5 (corresponding to the time of the picture A in figure 1) with all the output fields from the simulation at this given time.

opencc-by-4.0Dec 2022View details →

Estimates of the Wavenumber Wavelet Power Spectrum of Magnetic Fluctuations during Magnetic Reconnection Figure Data

This is data for the publication, "Estimates of the Wavenumber Wavelet Power Spectrum of Magnetic Fluctuations during Magnetic Reconnection".

opencc-by-4.0Mar 2020View details →

Dataset: 2D particle-in-cell (PIC) simulation of the magnetic reconnection for the paper "Electron mixing and isotropization in the exhaust of asymmetric magnetic reconnection with a guide field"

This repository contains pubilicly available numerical data of a 2D magnetic reconnection event, which includes the field data and plasma moment data. The simulation is performed with the VPIC code. The simulated data are used for the paper "Electron mixing and isotropization in the exhaust of asymmetric magnetic reconnection with a guide field".

opencc-by-4.0Dec 2023View details →

Intermittent Lobe Reconnection under Prolonged Northward Interplanetary Magnetic Field Condition: Insights from Cusp Spot Event Observations

SuperDARN is a collection of radars funded by national scientific funding agencies of Australia, Canada, China, France, Italy, Japan, Norway, South Africa, United Kingdom and the United States of America.  We would like to thank British Antarctic Survey (https://www.bas.ac.uk/project/superdarn) and the University of Saskatchewanan (https://superdarn.ca) for hosting the SuperDARN data mirrors access.  The EISCAT dataset is available from the Madrigal database (http://millstonehill.haystack.mit.edu).  We acknowledge the use of DMSP/SSUSI data provided by the Johns Hopkins University Applied Physics Laboratory (https://cdaweb.gsfc.nasa.gov).  Additionally, the OMNI dataset is available from the OMNIWeb service online of NASA/GSFC's Space Physics Data Facility's (https://spdf.gsfc.nasa.gov/pub/data/omni/).

opencc-by-4.0Mar 2024View details →

Data and Analysis Files for Simulations of Radiatively-Cooled Magnetic Reconnection on the Z machine

This dataset contains processed simulation data, representative simulation output files, and Python code for analysis of simulations presented in Datta, Rishabh, et al. "Simulations of Radiatively Cooled Magnetic Reconnection Driven by Pulsed Power." J. Plasma Phys. (2024). The simulations were run using GORGON, a radiative resistive MHD code with van Leer advection. Details on GORGON can be found in Chittenden et al. (2004) 10.1063/1.1643756, and Ciardi et al. (2007) 10.1063/1.2436479.

opencc-by-4.0Nov 2024View details →

Simulation dataset for New Insights on the High Reconnection Rate and the Diminishment of Ion Outflow

The dataset contains simulation data used in the paper of "New Insights on the High Reconnection Rate and the Diminishment of Ion Outflow". Data are generated from a particle-in-cell simulation using the VPIC code. Please see the paper for the descriptions of the simulation setup. The fields_moments.gda files in runs.7z are fields and plasma moments data of the simulations presented in the paper. The time step in unit of twci for each simulation is: A1:0.025, A2:0.1, A3:0.25, A4:0.25, A5:0.5, B1:0.1, B2:0.1, B3:0.1, B4:0.025, B5:0.05, C1:0.02, C2:0.02. Each file contains float-type data arrays with a size of (Lx/Δ)×1×(Lz/Δ), corresponding to x-y-z dimensions, respectively. Lx, Lz and Δ for each simulation are presented in the paper. Data can be read by softwares like IDL, python, matlab, etc., using the standard data reading methods. The runs_Hparticle_t_x_z files contain ion particle data for the time step t, for the domain of x=[x-0.03, x+0.03]di, z=[z-0.03,z+0.03]di. The files are IDL save files. To read the data, use restore, file=file in IDL. Each data chunk constitues of the following variables in order: all_vxs, all_vys, all_vzs, ws, all_xs, all_ys. Here all_vxs, all_vys and all_vzs are velocities in unit of light speed (c); all_xs and all_ys are x and z locations in unit of de; ws represents the weight of the particles, so the contribution of a particle to the phase space density needs to multiply by this ws factor (In the paper, ws factors are re-normalized while the relative weights between particles remain the same).

opencc-by-4.0Oct 2021View details →

Configuration of magnetotail current sheet prior to magnetic reconnection onset

Data repository for "Configuration of magnetotail current sheet prior to magnetic reconnection onset". This repository contains the following files: (1) "xyarray" is the main dataset; (2) "read_pritchett_pic_2d.py" is the python module that reads xyarray; (3) "simulation_params2.py" is the auxiliary python module that stores simulation parameters; (3) The python scripts with prefix "prod2_" plot the production figures; (4) "plt_style.py" is the plotting style sheet; (5) "movie-prod2_ratio-force.mp4" shows the evolution of different terms in the momentum equation prior to magnetic reconnection (The gray lines stand for the sum of all terms).

opencc-by-4.0Aug 2022View details →

Particle-in-cell data in support of interchange reconnection paper

IDL programs (the .pro files) and data (the .dat file) to generate the simulation plots in "Interchange reconnection within coronal holes powers the solar wind".

opencc-by-4.0Jan 2019View details →

Reconnection scaling in quantum fluids

Data of the paper: "Reconnection scaling in quantum fluids" by Fonda, Sreenivasan, Lathrop, PNAS 2018