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9 results for “3D magnetic field”
3D motion of flexible ferromagnetic filaments under rotating magnetic field
<p>This repository contains experimental data and numerical results related to the publication: A. Zaben, G. Kitenbergs, A. Cēbers (2020), 3D motion of flexible ferromagnetic filaments under rotating magnetic field. Soft Matter, <a href="https://doi.org/10.1039/D0SM00403K">https://doi.org/10.1039/D0SM00403K</a> / <a href="https://arxiv.org/abs/2003.03737">https://arxiv.org/abs/2003.03737</a>.</p> <p>Figs_data.xlsx contains the data presented in the figures. Experimental_Data.rar contains experimental images used to obtain the results for Fig. 3 and 9. The files are named with the operating frequency, field strength and filament length. Numerical.rar contains numerical results used in Fig.6, 8 and 9. The files are named with Cm values. The results are in .dat files named with Cm values followed by wt (wend_cm_wt). The first column is for time(t) followed by x,y,z values of filament tips. </p> <p> </p>
3D co-registration of ultra-low-field and high-field magnetic resonance images (data)
<p>Dataset used for "3D co-registration of ultra-low-field and high-field magnetic resonance images" submitted to PlosOne.</p>
Cosmological Initial Conditions (3D magnetic fields for an alfa=1.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=-1.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Cosmological Initial Conditions (3D magnetic fields for an alfa=1.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=1.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Cosmological Initial Conditions (3D magnetic fields for an alfa=2.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=2.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Research Data - Magnetic Field Controlled Surface Localization of Spin-Wave Ferromagnetic Resonance Modes in 3D Nanostructures
<p>Source data from micromagnetic simulations performed in COMSOL Multiphysics software and Python codes for data post-processing utilized in the paper "Magnetic Field Controlled Surface Localization of Spin-Wave Ferromagnetic Resonance Modes in 3D Nanostructures."</p> <p>The files from Comsol (.mph) are without simulation solutions due to their large size - please contact me if needed.</p>
Cosmological Initial Conditions (3D magnetic fields for an alfa=0.0 magnetic spectrum) for 85Mpc^3
<p>Files representing the initial conditions at z=40 for ENZO-MHD cosmological simulation of a comoving 85Mpc^3 volume, for tangled magnetic fields from an alfaB=0.0 initial spectrum of magnetic fluctuations. The simulation has 1024^3 cells and 1024^3 DM particles. These data are in binary format and can be read by the ENZO code.</p> <p>More details of the simulations and on it cosmological parameter can be found at:</p> <ul> <li>https://ui.adsabs.harvard.edu/abs/2021Galax...9..109V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.5350V/abstract</li> <li>https://ui.adsabs.harvard.edu/abs/2017CQGra..34w4001V/abstract</li> </ul>
Data and code for "Quasiparticle effects in magnetic-field-resilient 3D transmons"
<p>This folder contains all data files and Jupyter notebooks needed to recreate the figures of our publication, <br>"Quasiparticle effects in magnetic-field-resilient 3D transmons",<br>written by J. Krause, G. Marchegiani, L. M. Janssen, G. Catelani, Yoichi Ando, and C. Dickel</p> <p>Measurements were done with quantify-core (https://quantify-os.org/docs/quantify-core/)</p> <p>Required python packages are quantify-core (tested to run with version 0.7.4) and all its dependencies, as well as cmcrameri (colormaps used for plots).<br>Qutip is used for master equation solving and Hamiltonian modeling (used version 4.7.5) and hmmlearn (version 0.3.2) for fitting gaussian hidden-markov-models.<br>From a clean conda environment one should just install the above 4 packages and it should work.</p> <p>Content:<br>Data/ <br>Contains the plotted measurement data used in the figures of the paper mostly in csv format.<br>The datasets are loaded and plotted in the respective notebooks for all figures. </p> <p>Data/quantify_datasets/<br>Contains a few quantify datasets (raw data format of quantify measurements)</p> <p>Data/20220710_parity_paper_device_afm/<br>Contains .tiff images and .txt files with AFM data of the device</p> <p>Figures/<br>Contains all paper figures as .pdf files</p> <p>Fits/transmon_spectrum_including_EJ_harmonics<br>Contains some auxiliary fit results so the fits of flux arcs do not have to be repeated.</p> <p>Fits/Gap_vs_Bpar<br>Contains numerical results for the superconducting gap Delta as a function of magnetic field for aluminum films of different thickness.<br>Used to check the cavity data and not used for other modeling.<br>Imported in Jupyter_notebooks/models_transmon_spectrum_including_higher_harmonics.py</p> <p>Jupyter_notebooks/<br>Contains the jupyter notebooks with the code that creates the figures including the relevant calculations and fits and the loading of the data.<br>The notebook name gives the figure(s) it creates.<br>There are several auxiliary .py files and two notebooks that do not make paper figures:</p> <p>Jupyter_notebooks/fit_params.py<br>Contains the fit parameters for the quasiparticle modeling and the transmon spectrum</p> <p>Jupyter_notebooks/models_qp_dynamics.py<br>Contains the functions for quasiparticle modeling vs field and temperature.</p> <p>Jupyter_notebooks/models_transmon_spectrum_including_higher_harmonics.py<br>Contains the models for the field dependent spectrum</p> <p>Jupyter_notebooks/models_cavity_transmon_interaction.py<br>Contains qutip model for the fitting of the transmon-cavity Hamiltonian to estimate the bare-dressed changes.</p> <p>Jupyter_notebooks/fit_quasiparticle_model.ipynb<br>Notebook that shows how the quasiparticle model can be fit to the data<br>Takes a bit longer to execute</p> <p>Jupyter_notebooks/fit_cavity_transmon_interaction.ipynb<br>Looks at a resonator-transmon model to understand the bare-dressed difference and estimate the coupling.<br>Not really used in the paper, except to estimate G. </p>
BARREL 3D Tri-axial Fluxgate Magnetometer (MAGN) Magnetic Field Data, no Gain Correction, not Despun, Level 2, 0.25 s Data
Three axis DC magnetometer data with nominal conversions applied. Data are neither gain corrected nor despun.The BARREL Mission was a multiple-balloon investigation designed to study electron losses from Earth's Radiation Belts. Selected as a NASA Living with a Star Mission of Opportunity, BARREL was designed to augment the Radiation Belt Storm Probes, RBSP, mission by providing measurements of the spatial and temporal variations of electron precipitation from the radiation belts. The RBSP mission has since been renamed the Van Allen Probes mission. Each BARREL balloon carried an X-ray spectrometer to measure the bremsstrahlung X-rays produced by precipitating relativistic electrons as they collide with neutrals in the atmosphere, and a DC magnetometer to measure ULF-timescale variations of the magnetic field. BARREL observations collected near latitudes close to either the antarctic and arctic circles at stratospheric altitudes at about 30 km. The BARREL instrumentation provided the first balloon measurements of relativistic electron precipitation while comprehensive in situ measurements of both plasma waves and energetic particles were available. Also, the BARREL data has been used to characterize the spatial scale of precipitation at relativistic energies.The initial pair of balloon campaigns that were conducted initially during the Austral summer months of January and February of 2013 and 2014 with launches from two stations located in Antarctica: the British base located at Halley Bay on the Brunt Ice Shelf and the South African SANAE IV base (SANAE stand for South African National Antarctic Expedition) located in Vesleskarvet, Queen Maud Land. For the 2013 and 2014 the balloon campaigns, the launch plan was designed to maintain an array with about five payloads spread across about six hours of magnetic local time, MLT, in the region that magnetically maps to the radiation belts. Thus, the BARREL balloon constellation constituted an evolving and slowly moving array able to study relativistic electron precipitation from the radiation belts.Later campaigns were undertaken in 2015 and 2016 from the Esrange Space Center located in Kiruna, Sweden. The 2015 and 2016 campaigns were undertaken in coordination with the Van Allen Probes mission, the European Incoherent Scatter Scientific Association, EISCAT, incoherent scatter radar system, and other ground and space based instruments. Seven balloon launches occurred during the August 2015 BARREL campaign. A total of eight flights occurred during August 2016.Summing over the four BARREL campaigns, over 50 small, approximately 20 kg, stratospheric balloons were successively launched. The website creeated and hosted by A.J. Halford (see Information URL below) reports that: "By the end of the campaigns, there were over 90 researchers coordinating on a daily basis with the BARREL team working on 7 different satellite missions, 1 other balloon mission, and way too many ground based instruments to count." Although the BARREL mission launched only balloons during the years from 2013 to 2016, research using data collected on these flights is ongoing, so stay tuned for updates! All data and analysis software are freely available to the scientific community.The information listed above in this resource description was compiled by referencing several BARREL related resources including primarily the Millan et al. (2013) Space Science Reviews publication, the BARREL at Dartmouth mission web site, and the website maintained by A.J. Halford.The current release of all BARREL CDF data products are Version 10 files.BARREL will make all its scientific data products quickly and publicly available but all users are expected to read and follow the BARREL Data Usage Policy listed below.BARREL Data Usage PolicyBARREL data products are made freely available to the public and every effort is made to ensure that these products are of the highest quality. However, there may occasionally be issues with either the instruments or data processing that affect the accuracy of data. When possible, a quality flag is included in higher level data products, and known issues are posted in the BARREL data repository. You are also strongly encouraged to follow the guidelines below if you are planning a publication or presentation in which BARREL data are used. This will help you ensure that your science results are valid.* Users should always use the highest version numbers of data and analysis tools. Browse/quick-look plots are not intended for science analysis or publication and should not be used for those purposes without consent of the principal investigator, PI.* Users should notify the BARREL PI of the data use and investigation objectives. This will ensure that you are using the data appropriately and have the most recent version of the data or analysis routines. Additionally, if a BARREL team member is already working on a similar or related topic, they may be able to contribute intellectually
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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
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OpenNeuro
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