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691 results for “magnetic field”
Intermittent Lobe Reconnection under Prolonged Northward Interplanetary Magnetic Field Condition: Insights from Cusp Spot Event Observations
<p>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. <br>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. <br>The EISCAT dataset is available from the Madrigal database (http://millstonehill.haystack.mit.edu). <br>We acknowledge the use of DMSP/SSUSI data provided by the Johns Hopkins University Applied Physics Laboratory (https://cdaweb.gsfc.nasa.gov). <br>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/).</p>
Magnetic field enhancements in the interplanetary solar wind: Diverse processes manifesting a uniform observation type?
<p>Interlaced magnetic flux ropes are a subject of investigation in various space environments, including the solar corona, interplanetary solar wind, and magnetosheath. In this study, we utilize a Hall Magnetohydrodynamics (MHD) model to replicate these interactions within selected regions. By employing plasma flow to propel two flux ropes of various parameters towards each other, we examine the effect of their relative helicity on the ensuing process. Our simulations, coupled with vector analysis, found the existence of flux ropes with opposing helicity along their axes (counter-helical) in some of the resultant interactions. These findings underscore the need to identify and study counter-helical flux ropes in space. The study presented here contributes new comprehension of space plasma dynamics and new insights into the solar wind in control of space weather.</p>
"Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index" Figures, Scripts, and Data
<p>These tar files, scripts, and datasets were used in the paper "Nowcasting Solar EUV Irradiance with Photospheric Magnetic Fields and the MgII Index," submitted for publication to the Space Weather Journal. More information on what is included in this archive can be found the the ReadMe file. </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>
Magnetic Field Disorder May Explain Energetic Proton Diffusion through Heliosheath Plasma: Evidence from Voyager 2 Observations
<p>The spreadsheets of monthly data used for Figure 2 in the paper " <strong>Magnetic Field Disorder May Explain Energetic Proton Diffusion through Heliosheath Plasma: Evidence from Voyager 2 Observations</strong>" submitted to Geophysical Research Letters by the authors, and an explanatory text file named "Readme".</p>
Multispecies MHD study of ion escape at ancient Mars: effects of an intrinsic magnetic field and solar XUV radiation
<p>This dataset contains the simulation results in the paper "Multispecies MHD study of ion escape at ancient Mars: effects of an intrinsic magnetic field and solar XUV radiation" submitted to Journal of Geophysical Research: Space Physics.</p>
Spintronic terahertz emitters exploiting uniaxial magnetic anisotropy for field-free emission and polarization control
<p>Data for Figures 1-5</p>
Data and plotting code for "Energetic electron scattering by kinetic Alfvén waves at strong magnetic field gradients of dipolarization front"
<p>This publication includes the dataset and plotting code for reproducing results and figures of the manuscript "Energetic electron scattering by kinetic Alfvén waves at strong magnetic field gradients of dipolarization front", which was submitted to Physics of Plasma for potential publication. In this paper, we use test particle simulations to study energetic electron pitch angle and momentum scattering driven by kinetic Alfvén waves, at the magnetic field gradients associated with the dipolarization front, current sheet and plasma sheet fields in the magnetotail. </p> <p>The simulation data contains time history of 1000 test particle trajectories, momentum, energy, and KAW wave phases recorded every 0.001 second. Each simulation for different electron energies and pitch angles has a size of over 1 GB, so here we have only included one example of test particle simulation run associated with Figure 3. Only the final results of pitch angle diffusion coefficients are provided associated with Figure 4. A full set of time history results of all test particle simulation runs for Figure 4 will be available upon reasonable request (yshen@epss.ucla.edu). </p> <p>Detailed descriptions:</p> <p> PoP_figure_1.m --- Matlab plotting code for reproducing magnetic field model and geometry for Figure 1.</p> <p> PoP_figure_2.m --- Matlab plotting code for reproducing resonant energy as a function of wave normal angle, electron pitch angle, and field model parameters in Figure 2.</p> <p> PoP_figure_3.m --- Reading test particle simulation data and plotting code for reproducing Figure 3. Please ensure proper directory setting to read test particle data files. </p> <p> PoP_figure_4_5.m --- Reading saved bounce-averaged diffusion coefficient data and plotting Figure 4 and Figure 5.</p> <p> Daa_Energy_alpha_ad3xp15_e1.csv --- Electron diffusion coefficients driven by KAW scattering as a function of energy and pitch angle obtained from test particle simulations. KAW wave amplitude is set to 1 mV/m. Electrons are initiated from a position of x=150 km within the dipolarization front.</p> <p> Tau_Energy_alpha_xp15.csv --- Electron bounce periods as a function of energy and pitch angle based on numerical test particle simulations without KAW input.</p> <p> pKAW_1000p_dify_E100keV_PA5_Daa_E4_pop.zip --- Data files containing 1000 test particle trajectories, momentum and adiabatic invariant. This one single run is for electrons with an energy of 100 keV and a pitch angle of 5 degree, under influence of KAW wave electric field of 4 mV/m. This dataset is used to plot Figure 3. </p> <p> pKAW_1000p_dify_init_Ppara_mue_E100_PA4_Daa_E4_pop.dat --- initial parallel momentum and first adiabatic invariant of 1000 test particles. Read this file for plotting Figure 3. </p> <p> Bxyz.m --- calculate model magnetic field for given positions in x, y, and z</p> <p> FAC.m --- convert local x, y, z coordinates to field-aligned coordinates</p> <p> gradB.m --- calculate the gradient of magnetic field for given positions in x, y, and z</p> <p> E_to_pnorm_hsr.m --- calculate normalized momentum based on relativistic electron energy</p> <p> mysubplot.m --- plotting function to replace subplot routine of Matlab</p> <p> </p> <p> </p>
Magnetic field line information from sunspot simulation in 10.5281/zenodo.6385593
<p>This dataset contains magnetic field line information from the dataset corresponding to 10.5281/zenodo.6385593</p>
DATA - Modern manufacturing enables magnetic field cycling experiments and parahydrogen induced hyperpolarization with a benchtop NMR
<p>Datasets and software for the publication "Modern manufacturing enables magnetic field cycling experiments and parahydrogen induced hyperpolarization with a benchtop NMR"</p>
Simulation data : Triggering of whistler-mode rising and falling tone emissions in a homogeneous magnetic field
<p>This dataset is obtained from <a href="http://space.rish.kyoto-u.ac.jp/software/">KEMPO1</a> code with minor modifications. This dataset contains simulation data and Python3 code examples. For more details, please refer to README.md.</p>
Meridional composite pulses for low-field magnetic resonance
<p>We discuss procedures for error-tolerant spin control in environments that permit transient, large-angle reorientation of magnetic bias field. Short sequences of non-resonant magnetic field pulses in a laboratory-frame meridional plane are derived. These are shown to have band-pass excitation properties comparable to established amplitude-modulated, resonant pulses used in high, static-field magnetic resonance. Using these meridional pulses, we demonstrate robust z inversion in proton (<sup>1</sup>H) nuclear magnetic resonance near Earth’s field.</p>
Model generated open-closed field topology maps produced by ISSI team "Magnetic Open Flux And Solar Wind Structuring Of Interplanetary Space"
<p>Open and closed magnetic field topologies of the solar corona generated using four PFSS based coronal models (EUHFORIA, WSA, MULTI-VP, PSI-PFSS) and one full MHD coronal model (PSSI-MHD) using two different types of HMI-ADAPT magnetic field maps (with and without Active Regions (AR) added retrospectively). The magnetograms used are accessible here <a href="https://doi.org/10.5281/zenodo.10211762" target="_blank" rel="noopener">https://doi.org/10.5281/zenodo.10211762</a> (Henney, Carl. ‘ADAPT Global Solar Magnetic Maps - 2010 Sep 18-20 (w/ & W/o Farside Active Region Input)’. Zenodo, 28 November 2023).</p> <p>These model outputs were generated by the ISSI team "Magnetic Open Flux And Solar Wind Structuring Of Interplanetary Space" and were used for the paper accessible on Arxiv via this link: https://arxiv.org/abs/2311.04024</p>
Intermediate field-induced phase of the honeycomb magnet BaCo2(AsO4)2
Open the record for dataset details and reuse information.
A unified intensity of the magnetic field in the protoplanetary disk from the Winchcombe meteorite
<p>Alternating field demagentisation data for the Winchcombe meteorite, published in 'A unified intensity of the magnetic field in the protoplanetary disk from the Winchcombe meteorite' (2023) <em>Meteoritics and Planetary Science</em>, <strong>59</strong>, 1194-1215, 10.1111/maps.14079</p>
Weights for calculation of magnetic field at INTERMAGNET observatories for 3-D conductivity model of the Earth in the time domain
<p>Weights are calculated with time step of 1 hour and memory of 4320 hours for two cases.</p> <ol> <li>The source is parametrized by spherical harmonics up to degree 4 (<a href="../api/records/12802448/draft/files/MB_SHS_modes_up_to_24_at_obs.h5/content" target="_blank" rel="noopener noreferrer">MB_SHS_modes_up_to_24_at_obs.h5</a> )</li> <li>The source is parametrized by so-called periodic modes, obtained from the output of TIEGCM (<a href="../api/records/12802448/draft/files/MB_periodic_modes_16_24_at_obs.h5/content" target="_blank" rel="noopener noreferrer">MB_periodic_modes_16_24_at_obs.h5)</a></li> </ol> <p>The detailed desciption of the weights meaning and calculation can be found in Kruglyakov & Kuvshinov, 2024.</p> <ul> <li>Datasets M_B_r stand for radial (upward) component of the magnetic field at the ground;</li> <li>Datasets M_B_theta stand for southward component of the magnetic field at the ground;</li> <li>Datasets M_B_phi stand for eastward component of the magnetic field at the ground;</li> <li>Datasets Theta stand for the co-latitudes of the observatories in the geo-centric cooridnate system</li> <li>Datasets Phi stand for the longitudes of the observatories in the geo-centric cooridnate system</li> </ul> <p> </p>
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>
Underground measurement of magnetic field pulses during the early stage of rocket-triggered lightning
<p>raw data for the paper <em>Underground measurement of magnetic field pulses during the early stage of rocket-triggered lightning. </em></p>
Figure 2 in The orientation of earthworms is influenced by magnetic fields
Figure 2. Experimental design of the study: 20 earthworms were placed into each vivarium.
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by Keszthelyi et al. 2024
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by <a href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.tmp.1818K/abstract">Keszthelyi et al. 2024</a></p>
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