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691 results for “magnetic field”
IMF clock angle proxy: orbital averaged magnetic field data from MAVEN in Martian magnetosheath
<p>The By and Bz components can be used as IMF clock angle proxy (IMF direction in MSO y-z plane). See the publication by Dong et al. 2019 for details: Dong, Y., Fang, X., Brain, D. A., Hurley, D. M., Halekas, J. S., Espley, J. R., et al. (2019). Magnetic field in the Martian magnetosheath and the application as an IMF clock angle proxy. <em>Journal of Geophysical Research: Space Physics</em>, 124, 4295–4313. <a href="https://doi.org/10.1029/2019JA026522">https://doi.org/10.1029/2019JA026522</a></p> <p>Formats: IDL save file and ASCII file</p> <p>Data descirption:</p> <p>Time span: Nov 11 2014 - May 21 2024</p> <p>Time: averaged unix time of MAVEN in magnetosheath of each s/c orbit</p> <p># of data points: # of data points (time resolution: 4s) taken in magnetosheath of each s/c orbit. Suggest using only # of data points >150 (i.e. duration > 10 min)</p> <p>Bx, By, Bz in MSO coordinate system</p> <p> </p>
Magnetic diffusion in Solar atmosphere produces measurable electric fields
<p>Stokes spectra in 397, 630, and 854 nm with a field-of-view of 10"x10" that contains the analyzed Ellerman bomb</p>
Simulations of the shock turbulence interaction: magnetic fields and particles datasets
<p>Simulation snapshots for hybrid-kinetic model of a perpendicular shock interacting with pre-existing plasma turbulence. This dataset allows to reproduce the analyses presented in Trotta et al. 2024. The filenames are organised in <level of turbulence>-Variable.txt *(e.g., dB_B_00_B_z.txt is the magnetic field z component for the case with turbulence level dB/B = 0.0). </p> <p>For support in reading the simulation data or if further variables/snapshots are needed for scientific purposes, please be in touch.</p>
The data for Prediction of Large Solar Flares Based on SHARP and HED Magnetic Field Parameters
<p>The <span>repository</span> includes HED and SHARP Datasets, along with descriptions of the <span>d</span>ata <span>p</span>rocessing <span>procedures</span>, and the experimental code u<span>tilized</span> in <span>our</span> study.</p> <p><span>The files named "HED parameters.csv" and "SHARP parameters.csv" </span><span>represent the raw data of HED and SHARP Datasets</span><span>, respectively. Each dataset consists of 286 ARs, specifically, each dataset includes 189 C-class flaring ARs, 86 M-class flaring ARs, and 11 X-class flaring ARs.</span> <span>The column name "AR" represents the NOAA AR numbers, the column name "time" represents the time at which the AR samples were acquired, and the column name "level" represents the flare class of the AR. Moreover,</span> <span>i</span>n the HED dataset, the column name "energy" represents the "E_{free}", "shear_mean" represents the "\Psi", "uj_mean" represents the "J_{Z}", "uhc_mean" represents the "H_{C}", "GBH_MEAN" represents the "B_{h}", <span>and </span>"ALP_MEAN" represents the "\alpha". In the <span>SHARP</span> dataset<span>, </span>the column names of the other columns correspond to the names of various parameters.</p> <p><span>The files named </span>"SHARP_CV<span>.zip</span>" and "HED_CV<span>.zip</span>" represent the ten cross-validation sets that have been normalized and divided using an AR-based cross-validation method.</p> <p><span>T</span>he <span>d</span>ata <span>p</span>rocessing <span>procedures are as follows. Si</span><span>nce the SHARP and HED parameters have distinct scales and units, they </span><span>are </span><span>individually normalized using mean-standard deviation</span><span>.</span> <span>Subsequently, we set the labels for C-class flaring </span><span>AR</span><span>s to </span><span>the negative class</span> <span>which are equal to 0</span><span>, and the labels for M/X-class flaring </span><span>AR</span><span>s</span> to <span>positive class which are equal to 1</span>. <span>We employ an AR-based cross-validation (CV) method to partition the SHARP and HED datasets with the distribution of the training, validation, and testing sets at a ratio of 60%, 20%, and 20%, respectively.</span> This process is repeated ten times, resulting in ten cross-validation sets in both SHARP datasets (SHARP_CV) and HED datasets (HED_CV), respectively. The column named "level" in the SHARP_CV data and the column named "key" in the HED_CV data represent the labels for the flare classes of the <span>AR</span>s.</p> <p><span>The file named </span>"Parameter description and formula of SHARP and HED as well as data division process.pdf" <span>represents the </span>description and formula of SHARP and HED <span>p</span>arameter<span>s, as well as the procedure for generating 10-fold cross-validation set divisions for the SHARP/HED datasets.</span></p> <p><span>We design five solar flare prediction models leveraging five currently popular deep learning algorithms: Transformer, BiLSTM-Attention, BiLSTM, LSTM-Attention, and LSTM. Moreover, we use the NN model as the baseline model to compare with other deep learning model. </span>The solar flare prediction model used in this <span>paper</span> can be accessed via https://drive.google.com/drive/folders/1n6fXcQdCBogKt6L0aaPFagraFcXmX0fw?usp=drive_link.</p> <p> </p>
Enhanced_Precipitation_of_energetic_protons_due_to_Uranus_asymmetric_magnetic_field
<p>The dataset pertaining to Figures 1-4 in the academic paper titled: "Enhanced Precipitation of energetic protons due to Uranus asymmetric magnetic field" by Matthew Acevski and Adam Masters</p>
Data and Code for "Study of Solar Wind and Interplanetary Magnetic Field Features Associated with Geomagnetic Storms: The Cross Wavelet Approach"
<p>These files are the supplementary information, including dataset, codes and plots for the research work entitled "Study of Solar Wind and Interplanetary Magnetic Field Features Associated with Geomagnetic Storms: The Cross Wavelet Approach".</p>
Data for the paper "Magnetic fields with precise quasisymmetry"
<p>This archive contains data and source code used for the paper "Magnetic fields with precise quasisymmetry".</p>
Plasmonic Metasurface Resonators to Enhance Terahertz Magnetic Fields for High-Frequency Electron Paramagnetic Resonance _experimental dataset
<p>This dataset contains the raw experimental data for Tesi et al., Plasmonic Metasurface Resonators to Enhance Terahertz Magnetic Fields for High-Frequency Electron Paramagnetic Resonance, Small Methods 2021, 2100376, DOI <a href="https://doi.org/10.1002/smtd.202100376">10.1002/smtd.202100376</a>. </p>
Energetic Electron Lensing Caused by 375 Ganymede's Magnetic Field
<p>Suplementary meterial for the paper <em>Energetic Electron Lensing Caused by Ganymede’s Magnetic Field</em> (perijove radiation data).</p>
Spherical harmonic models of the magnetic field of Mars from Cain et al. (2003)
<p>This archive contains spherical harmonic coefficients of the two magnetic field models of Mars that were published in Cain et al. (2003): FSU50 and FSU90. The two models here are identical to those found in the supplemental materials of that manuscript, with the exception that they have been reformatted for easy input into the pyshtools software.</p> <p>Cain, J. C., Ferguson, B. B., Mozzoni, D. (2003), An n = 90 internal potential function of the Martian crustal magnetic field, Journal of Geophysical Research: Planets, 108 (E2), doi:10.1029/2000JE001487.</p>
Variable stellar outflows as a probe to magnetic fields and other physical characteristics of hot, massive stars
<p>It is now clear that the radiatively driven outflows from hot, massive stars are far more complex than the simple homogeneous and spherically symmetric flows originally envisioned. With the advent of high resolution, high cadence observations of various types in the past decades, a myriad of phenomena have been uncovered that can help us reach a better understanding of the parameters and characteristics of the stars from which these winds originate. This in turn has important ramifications on the various phases of evolution of the star and on the way it will ultimately end its life. In this talk, I will review the many observational signatures of variable stellar outflows of massive stars and describe how they relate to physical characteristics of the underlying star, with a particular emphasis on magnetic fields.</p>
Raw data for 'Signature of spin triplet exciton condensations in LaCoO3 at ultrahigh magnetic fields up to 600 T'
<p>Raw data for the paper below</p> <p>Signature of spin triplet exciton condensations in LaCoO3 at ultrahigh magnetic fields up to 600 T<br> A. Ikeda, Y. H. Matsuda, K. Sato, Y. Ishii, H. Sawabe, D. Nakamura, S. Takeyama, J. Nasu<br> arXiv:2201.02704</p> <p> </p>
Data of homogeneity of the photocathode in the Hamamatsu R15458-02 PMT under different magnetic field orientations
<p>The Hamamatsu R15458-02 PMT's photocathode was scanned with a collimated beam at 777 different positions to determine the relative transit time, TTS and gain. This measurement was performed at 192 different magnetic field orientations with a strength of 54.7 microtesla. The analyzed data is available in a JSON file.<br> To access the results for example in Python, you can import the data to a dictionary, and retrieve the values as follows:</p> <ul> <li> <p>The relative transit time is stored in the "RelTransitTime" key, TTS in "TTS," and gain in "Gain." Each of these keys contains a list of 192 lists, with each list containing 777 values.</p> </li> <li> <p>The 192 lists for each key correspond to scans measured at different magnetic fields. The "B_field" key retrieves the corresponding normalized magnetic field direction, which is a list of 192x3 elements.</p> </li> <li> <p>The 777 values in each list correspond to the value at different positions on the photocathode. You can access these positions using the "x" and "y" keys.</p> </li> </ul> <p>For further details, you can refer to Chapter 7 of M. Unland thesis "Development, simulation, and characterisation of a novel multi-PMT optical module for IceCube Upgrade with emphasis on detailed understanding of photomultiplier performance parameters" published in 2023.</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>
Locomotor Responses of Utricular Mutants to High Magnetic Field Exposure
<p>Wild-type mice or head-tilt (het) or tilted (tlt) mutant mice were exposed to static 14.1 T magnetic field, or sham-exposed, for 30 min; locomotor activity was recorded for 2 minutes after exposure. The het and tlt mice lack otoconia in the inner ear, and are unresponsive to vestibular linear acceleration. After magnetic field exposure, wild-type mice and tlt mice show suppressed rearing and tight counter-clockwise circling. The het mutant mice do not show circling nor is their rearing suppressed. This suggests that otoconia, or a function that depends on otoconia, are required for full vestibular responsiveness to magnetic fields.</p>
Magnetic-field-free nonreciprocal transport in graphene multi-terminal Josephson junctions
<p>Dataset for "Magnetic-field-free nonreciprocal transport in graphene multi-terminal Josephson junctions" manuscript</p>
Data for: Magnetic-field-assisted molecular beam epitaxy: Engineering of Fe3O4 ultrathin films on MgO(111)
<p>Molecular beam epitaxy is widely used for engineering low-dimensional materials. Here, we present a novel extension of the capabilities of this method by assisting epitaxial growth with the presence of an external magnetic field (MF). MF-assisted epitaxial growth was implemented under ultra-high vacuum conditions thanks to specialized sample holders for generating in-plane or out-of-plane MF and dedicated manipulator stations with heating and cooling options. The significant impact of MF on the magnetic properties was shown for ultra-thin epitaxial magnetite films grown on MgO(111). Using in situ and ex situ characterization methods, scanning tunneling microscopy, conversion electron Mössbauer spectroscopy, and the magneto-optic Kerr effect, we showed that the in-plane MF applied during the reactive deposition of 10 nm Fe3O4(111)/MgO(111) heterostructures influenced the growth morphology of the magnetite films, which affects both in-plane and out-of-plane characteristics of the magnetization process. The observed changes are explained in terms of modification of the effective magnetic anisotropy.</p>
Unidirectional spin wave emission by travelling pair of magnetic field profiles
<p>This is the full data for this paper: https://arxiv.org/pdf/2307.12653.pdf</p> <p>G. P. anf J. W. K. would like to acknowledge the erasmus mundus MaMaSELF programm and the support from the National Science Center – Poland grant No. 2021/43/I/ST3/00550</p>
Simulation data for "Connection between Chorus Wave Amplitude and Background Magnetic Field Inhomogeneity: A Parametric Study" which will be submitted to Geophysical Research Letters
<p>Simulation data for "Connection between Chorus Wave Amplitude and Background Magnetic Field Inhomogeneity: A Parametric Study" which will be submitted to Geophysical Research Letters.</p> <p>Including the simulation input parameter file and the necessary output data for analysis described in the article. The output data consists of waveform data at certain locations (|MLAT| = 3 deg).</p>
Supplementary material and dataset for article "Structure-Function Relationship of Iron Oxide Nanoflowers: Optimal Sizes for Magnetic Hyperthermia Depending on Alternating Magnetic Field Conditions"
<p>The supporting information file contains additional measurements compared to the main manuscript of the related article: TEM size histograms, SAED and XRD patterns, absorption and fluorescence spectra, DC magnetization curves, AC hysteresis loops, HR-TEM, their FTT patterns and inverse FFT images after applying a mask in the reciprocal space, and various other plots of this multi-parametric study on the structure-properties relations of magnetic iron oxide nanoflowers. Whenever needed for comparison to other experimental results or theoretical fitting, the raw data of all DC magnetization curves, AC hysteresis loops, ZFC-FC magnetization curves vs. temperature (and their derivatives on temperature) are made freely available in this dataset.</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.