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38 results for “dynamo”
Datasets to "Compressible test-field method and its application to shear dynamos"
<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 "Compressible test-field method and its application to shear dynamos" by M. J. Kapyla, M. Rheinhardt, & A. Brandenburg (Astrophys. J., in press, arXiv:2106.01107). If anything turns out to be incomplete, please email maarit.kapyla@aalto.fi or brandenb@nordita.org. </pre>
Dynamo in weakly collisional non-magnetized plasmas impeded by Landau damping of magnetic fields
<p>This dataset contains a collection of simulation inputs and results used in the paper [I. Pusztai et al (2020) Phys. Rev. Lett., Dynamo in weakly collisional non-magnetized plasmas impeded by Landau damping of magnetic fields, https://arxiv.org/abs/2001.11929]. References to figures below refer to this publication. </p> <p>These simulations are performed using the kinetic-Vlasov solver Gkeyll [version: cd65328c077f+ 2228+ default], for more information on the code visit https://gkyl.readthedocs.io/en/latest/index.html, or consult [J. Juno et al (2018) J. Comp. Phys 353, 110].</p> <p>The input files are found with .lua extension in each simulation directory</p> <p>Content:</p> <p>* Galloway-Proctor-flow_Fig1-kinetic-and-Fig2 <br> Kinetic simulation of the Galloway-Proctor flow, corresponding to the solid lines in Fig. 1 and Fig. 2. </p> <p>* Cnu-and-k-scan_Fig3-and-Fig4a<br> This is a parameter scan in wavelength of the magnetic perturbations [ranging from L0 ("L0") to L0/8 ("L0per8"), with baseline domain size L0] and collision frequencies [ranging from 0.05 ("Cnu005") to 1 ("Cnu1") times the baseline values]. These results are presented in Fig. 3 and Fig. 4a.</p> <p>* Magnetization-scan_Fig4b<br> Scan in magnetization shown in Fig. 4 b. The magnetic field varies between 1 and 100 T ["B1" and "B100", respectively].</p> <p>* Roberts-flow_Fig5 <br> Kinetic simulations of the Roberts flow, shown in Fig. 5. The collision frequency is scaled to 0.3 the physical value (dashed lines, "Roberts_Cnu03_Fig5"), and zero (solid lines, "Roberts_Cnu00_Fig5"). </p> <p>* Pencil_Run_12x12x12.tar.gz<br> Input files for PENCIL CODE simulations.</p>
Planetesimal gradual accretion and thermal dynamo results
<p>Numerical modelling code used to produce data and figures in the publication Dodds et al., 2020 'The thermal evolution of planetesimals during accretion and differentiation: consequences for dynamo generation by thermally-driven convection.' </p> <p>Data used to produced figures in above publication also included here.</p> <p>Please contact Kathryn Dodds with any questions.</p>
Data for Dodds et al., The direction of core solidification in asteroids: implications for dynamo generation
<p>Numerical dataset for the data presented in Dodds et al., The direction of core solidification in asteroids: implications for dynamo generation, manuscript submitted to Icarus journal.</p>
Datasets for ``Dynamo effect in decaying helical turbulence''
<p>In this supplemental material to the paper ``Dynamo effect in decaying helical turbulence,'' Phys. Rev. Fluids, 4, 024608 (2019), DOI: <a href="https://doi.org/10.1103/PhysRevFluids.4.024608">10.1103/PhysRevFluids.4.024608</a>, <a href="http://arXiv.org/abs/1710.01628">(arXiv:1710.01628</a>) we provide the underlying data to most of the figures. The file decdynamo.tar.gz contains a gzipped tar file to the website</p> <p> https://www.nordita.org/~brandenb/projects/decdynamo/</p> <p>For each of the Runs A-H plus 3 addition ones of Figures 13 and 14, the original run directories are given. They contain secondary data such as time series and spectra. The full snapshots are not stored, but all the relevant files needed for rerunning any particular simulation exist. In each directory, the input files (*.in) exist and data are under the directory data (including time series and spectra). In some cases, data directly relevant for particular plots are available, for example the directory "spectra" contains selected spectra used in some plots.</p>
Results of the DYNAMO (Dynamic MEC Orchestration of Cellular Networks) experiment in the Fed4FIRE+ testbeds
<p>The main objective of the DYNAMO Fed4FIRE+ experiment was to perform Network Function Virtualization (NFV) Management and Network Orchestration (MANO) of a cellular network on top of cloud infrastructures, exploring one of the key enabling technologies for 5G systems and beyond. DYNAMO used cloud and radio access facilities at the IRIS testbed and cloud facilities at the University of Vigo (UVIGO) to deploy an end-to-end (E2E) cellular network and perform elastic changes on it if needed. The geographic distance in between facilitated the setup of a realistic Multi-Access Edge Computing (MEC) use case, where the virtual Evolved Packet Core (vEPC) was deployed at UVIGO (Spain) and the access network, i.e., the User Equipment (UE), the e-Node-B (eNB) and edge cloud, were implemented on IRIS testbed (Ireland).<br> <br> While the initial deployment of the E2E cellular network may be considered as static, DYNAMO showcases the elasticity that an E2E cellular network may need in runtime. Hence, we presented a use case consisting of a latency sensitive E2E cellular network (network slice), where the endpoint of the UE connection was initially located in the core (UVIGO) but then migrated to the edge (IRIS), in case the UE's latency ranges were unacceptable.<br> <br> In this regard, the UE reported the experienced latency to Open Network Automation Platform (ONAP), which is responsible to trigger specific policy-driven control actions if a predefined Service-Level Agreement (SLA) is violated.<strong> <em>This datased includes the reports provided by the UE to ONAP.</em></strong><br> <br> As a result, the endpoint of the data plane of the UE is automatically moved to the access network (IRIS) thus reducing significantly the latency for the UE. For the access part of the network, we implemented one srsLTE e-Node-B (eNB), one srsLTE User Equipment (UE) and a Devstack (Edge Cloud) in virtual machines on IRIS testbed. In addition, we also implemented an SDN switch controlled by an ONOS SDN controller. For the core part of the network, we considered a disaggregated vEPC from Open Air Interface (OAI) on a Devstack (Core Cloud) at UVIGO.<br> <br> DYNAMO has succeeded in the integration of a broad set of network elements and technologies between the two different domains (UVIGO and IRIS testbed) and fulfilled all initial objectives: (i) establishing communication between ONAP and IRIS testbed to deploy generic VNFs on core and edge clouds, (ii), deployment of an E2E cellular network with UE and eNB in IRIS and the vEPC at UVIGO, (iii), sending telemetry of the UE to ONAP and (iv) designing and testing closed-loop control actions in ONAP to migrate the data plane of the UE to the edge in case of unsatisfactorily SLA. DYNAMO paves the way to a broad set of future 5G experiments that will require resource orchestration, such as the deployment of network slices or the automatic scheduling of services in the limited resources of Edge Clouds.</p> <p>This repository contains the information sent from the UE to ONAP, in order to decide if the latency between the UE and the PGW is OK or if an action has to be considered to reduce such latency.<br> </p> <p> </p>
Magnetic field data for "Cosmic Rays in Intermittent Magnetic Fields" (magnetic fields produced by the small-scale dynamo)
<p>Magnetic field data for the kinematic dynamo generated magnetic fields (KS) employed in the cosmic ray test particle simulations of Shukurov et al. 2017, <em>ApJL</em>, <strong>839</strong>, L16 [<a href="https://doi.org/10.3847/2041-8213/aa6aa6">https://doi.org/10.3847/2041-8213/aa6aa6</a>]. One dataset was also used in "Relative distribution of cosmic rays and magnetic fields", Seta et al. 2018, <em>MNRAS</em>, <strong>473 </strong>(4), 4544-4557 [<a href="https://doi.org/10.1093/mnras/stx2606">https://doi.org/10.1093/mnras/stx2606</a>]. These studies investigated the effects of magnetic field structure on charged test particle transport and trapping. See the README file for more details.</p> <p> </p>
Datasets for "Dynamo effect in unstirred self-gravitating turbulence"
<pre>This directory contains an index.html file with links to the run directories with secondary data for Table I of the paper "Dynamo effect in unstirred self-gravitating turbulence" by Axel Brandenburg and Evangelia Ntormousi. If anything turns out to be incomplete, please email brandenb@nordita.org. </pre>
Datasets for ``Dissipative magnetic structures and scales in small-scale dynamos''
<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 "Dissipative magnetic structures and scales in small-scale dynamos" by A. Brandenburg, I. Rogachevskii, and J. Schober. If anything turns out to be incomplete, please email brandenb@nordita.org. </pre>
Data sets for " The nature of mean-field generation in three classes of optimal dynamos"
<pre>The tar archive Optimal_Dynamos.tar contains and index.html file with links to the run directories for each figure and the two tables of the paper "The nature of mean-field generation in three classes of optimal dynamos" by Axel Brandenburg (Nordita) and Long Chen (Durham University) with the temporary URL http://norlx51.nordita.org/~brandenb/tmp/long_chen. Corrections and updates are available on the active URL to this tar archive: https://www.nordita.org/~brandenb/projects/Optimal_Dynamos/</pre>
Datasets for ``Batchelor, Saffman, and Kazantsev spectra in the small-scale dynamo''
<pre>This directory contains Supplemental Material and an index.html file with links to the run directories and idl plotting routines with secondary data for the other figures for the paper "Batchelor, Saffman, and Kazantsev spectra in the small-scale dynamo" by A. Brandenburg, H. Zhou and R. Sharma. If anything turns out to be incomplete, please email brandenb@nordita.org. </pre>
Dataset for "Helical dynamo growth at modest versus extreme magnetic Reynolds numbers"
<p>This directory contains the dataset (data.tar) and the post-processing script (post_processing.nb) of the manuscript "Helical dynamo growth at modest versus extreme magnetic Reynolds numbers" by Hongzhe Zhou and Eric Blackman.</p>
Datasets for "Cross-helicity effect on alpha-type dynamo in non-equilibrium turbulence"
<p>This directory contains an index.html file with links to the run directories for Runs A-E and idl plotting routines with secondary data for the other figures for the paper "Cross-helicity effect on alpha-type dynamo in non-equilibrium turbulence" by Mizerski, Yokoi, & Brandenburg.</p>
Dataset for 'Rotational dependence of turbulent transport coefficients in global convective dynamo simulations of solar-like stars'
<p>For moderate and slow rotation, magnetic activity of solar-like stars is observed to strongly depend on rotation, while for rapid rotation, only a very weak or no dependency is detected. These observations do not yet have a solid explanation in terms of dynamo theory. To work towards such an explanation, we numerically investigated the rotational dependency of dynamo drivers in solar-like stars, that is, stars that have a convective envelope of similar thickness as in the Sun. We ran semi-global convection simulations of stars with rotation rates from 0 to 30 times the solar value, corresponding to Coriolis numbers, Co, of 0 to 110. We measured the turbulent transport coefficients describing the magnetic field evolution with the help of the test-field method, and compared with the dynamo effect arising from the differential rotation, self-consistently generated in the models. The trace of the <strong><span class="math-tex">\(\alpha\)</span></strong> tensor increases for moderate rotation rates with Co<sup>0.5</sup> and levels off for rapid rotation. This behavior is in agreement with the kinetic <span class="math-tex">\(\alpha\)</span> based on the kinetic helicity, if one takes into account the decrease of the convective scale with increasing rotation. The <strong><span class="math-tex">\(\alpha\)</span></strong> tensor becomes highly anisotropic for Co > 1, <span class="math-tex">\(\alpha_{rr}\)</span> dominates for moderate rotation (1<Co<10), and <span class="math-tex">\(\alpha_{\phi\phi}\)</span> for rapid rotation (Co > 10). The effective meridional flow, taking into account the turbulent pumping effects, is markedly different from the actual meridional circulation profile. Hence, the turbulent pumping effect is dominating the meridional transport of the magnetic field. Taking all dynamo effects into account, we find three distinct regimes. For slow rotation, the <span class="math-tex">\(\alpha\)</span> and Rädler effects are dominating in presence of anti-solar differential rotation. For moderate rotation, <span class="math-tex">\(\alpha\)</span> and <span class="math-tex">\(\Omega\)</span> effects are dominant, indicative of <span class="math-tex">\(\alpha\Omega\)</span> or <span class="math-tex">\(\alpha^2\Omega\)</span> dynamos in operation, producing equatorward-migrating dynamo waves with the qualitatively solar-like rotation profile. For rapid rotation, an <span class="math-tex">\(\alpha^2\)</span> mechanism, with an influence from the Rädler effect, appears to be the most probable driver of the dynamo. Our study reveals the presence of a large variety of dynamo effects beyond the classical <span class="math-tex">\(\alpha\Omega\)</span> mechanism, which need to be investigated further to fully understand the dynamos of solar-like stars. The highly anisotropic <strong><span class="math-tex">\(\alpha\)</span></strong> tensor might be the primary reason for the change of axisymmetric to non-axisymmetric dynamo solutions in the moderate rotation regime.</p> <p>For the full article see <a href="https://arxiv.org/abs/1910.06776">https://arxiv.org/abs/1910.06776</a></p>
Thermal and dynamo evolution of the lunar core based on transport properties of Fe-S-P alloys
<p>These data are our original measured resistivity data and calculation data. </p>
Supporting Data for Martian Dynamo Change at ~4.1 Ga: Evidence from the Magnetic Measurements of the Iota Crater
<p><a href="https://zenodo.org/api/records/14257490/draft/files/MAG_MAVEN_NIGHTTIME.txt/content" target="_blank" rel="noopener noreferrer">MAG_MAVEN_NIGHTTIME.txt</a> contains magnetic field from MAVEN nighttime tracks across the study area;</p> <p><a href="https://zenodo.org/uploads/14257490" target="_blank" rel="noopener noreferrer">TOPOGRAPHY_CRUST_AB.txt </a> contains the topography and crustal thickness data in Figure 2;</p> <p><a href="https://zenodo.org/api/records/14257490/draft/files/MAGNETIC_MODEL_CALCULATION.csv/content" target="_blank" rel="noopener noreferrer">MAGNETIC_MODEL_CALCULATION.csv</a> contains the <span>normalized circumferential averaged magnetic field upon the impact crater with different diameters and internal magnetizations, which are calculated randomly one hundred times in each case.</span></p>
Dataset: Dynamo models with a Mercury-like magnetic offset dipole
<p>Input and Output Data for reproducing figures and tables in the submitted publication Kolhey et al. (2024) "Dynamo models with a Mercury-like magnetic offset dipole".</p>
Dataset for ApJ Letter: Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior
<p>This dataset contains the input files (main_input and custom_reference_binary), basic simulation info (grid_info, jobinfo.txt, and equation_coefficients) and the last Rayleigh checkpoints for the two cases published in the ApJ Letter, Confinement of the Solar Tachocline by Dynamo Action in the Radiative Interior. The data for each case (the "HD case" and "MHD case" as referred to in the paper) are given in .zip files.</p> <p>NOTE: The MHD case has custom diagnostic outputs and the main_input file (as directly given here) can only be run using Loren Matilsky's personal branch of the code: https://github.com/illorenzo7/Rayleigh/tree/me_prod_subcurv (for full reproducibility, commit fcf1a7b81624a0af7866d52d5b7836549268044e). Otherwise, the MHD case should run using the current main branch of the Rayleigh code (https://github.com/geodynamics/Rayleigh), as long as the custom quantity codes (>2200) are removed.</p>
Pre-explosion dynamo in the cores of massive stars
<p>Inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.464.3249S">Soker & Gilkis (2017)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.1093/mnras/stw2546">10.1093/mnras/stw2546</a></p>
Dataset: Powering Earth's ancient dynamo with silicon 2 precipitation
<p>Collated experimental dataset used in this study. Study, temperature, pressure and normalised molar concentrations of Fe, Si, O, C, S, Mg, FeO, SiO2 and MgO in metal and silicate from partitioning experiments.</p>
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