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Dataset results
26 results for “Magnetic winding”
The impact of solar wind magnetic field fluctuations on the magnetospheric energetics
<p>This dataset provides the results and analysis tools of the manuscript by Ala-Laht et al. "The impact of solar wind magnetic field fluctuations on the magnetospheric energetics". In addition, relevant SWMF simulation input files are included. See ReadMe.txt for information.</p>
A Theoretical Window into the Wind Clumping Properties of Magnetic Hot Star Winds
<p>Winds from hot, massive OB stars are driven by scattering and absorption of the stellar radiation by spectral lines. The standard line-driven wind theory of CAK predicts a smooth, steady outflow but neglects a strong radiation instability, resulting in strong shocks and a highly structured, clumped wind. Treating clumping arising from this line-deshadowing instability (LDI) is of key importance in accurately interpreting observed spectral diagnostics of massive star winds. Indeed, if not correctly accounted for, such wind clumping may lead to quite dramatic errors in inferred mass-loss properties and to correspondingly large errors in massive-star evolution predictions. So far theory and observation of the LDI have only investigated wind clumping for non-magnetic OB stars. Meanwhile, quantitative wind clumping behaviour for magnetic massive stars has not been established. However, by now there is ample evidence from spectropolarimetric surveys that a subset of OB stars in our Galaxy possesses strong, global surface magnetic fields believed to be of primordial origin. This magnetic field leads to a quenching of mass loss and can significantly alter stellar evolution, with speculations that it may even lead to formation of high stellar mass black holes. Such mass-loss rates have up until now relied on smooth wind predictions, hence do not take into account the intrinsic clumpy structures. In this contribution I present the first results of 2D numerical simulations on magnetic LDI winds that self-consistently predict the wind clumping phenomenon. I show the possible pathways to structure formation and discuss this in light of our recently carried out analytical perturbation analysis. Finally, I discuss the resulting wind clumping properties and the possible effects on observational diagnostics.</p>
Solar wind plasma, magnetic field parameters and geomagnetic storm index SYM-H from 2000 to 2020
<p>SYM-H index is used to quantify the intensity of geomagnetic storm. Its temporal variation is related to the solar wind plasma and magnetic field parameters. This dataset offers time series of solar wind density, solar wind velocity and solar wind magnetic field, SYM-H index. The python and matlab code files for processing and plotting data are also included. </p>
Solar wind plasma, magnetic field parameters and geomagnetic storm index SYM-H from 2000 to 2020
Open the record for dataset details and reuse information.
On the Fourier Contribution of Strong Current Sheets to the High-Frequency Magnetic Power Spectral Density of the Solar Wind
<p>These two tab-delimited files list the Universal Times at which the WIND spacecraft and the MMS spacecraft encounter strong current sheets in the solar wind.</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>
Dynamics of the Young Solar Wind: Weakened Magnetization and Onset of Large Scale Turbulence (Simulation Data)
<p>Simulation data used in "Dynamics of the Young Solar Wind: Weakened Magnetization and Onset of Large Scale Turbulence", submitted to Geophysical Research Letters.</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>
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>
Magnetic field enhancements in the solar wind: Diverse processes manifesting a uniform observation type?
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Dataset for for manuscript "Solar wind magnetic holes can cross the bow shock and enter the magnetosheath"
<p>This data set contains event times and basic properties of magnetic holes analysed in the manuscript "Solar wind magnetic holes can cross the bow shock and enter the magnetosheath".</p>
Ground Magnetic Disturbances due to Neutral-wind-driven Ionospheric Currents
<p>This dataset includes GITM outputs of an idealized event. This dataset is used to analyze the geomagnetic disturbances due to neutral-wind-driven ionospheric currents, and their relative importance compared to the geomagnetic disturbances driven by magnetospheric convection electric field.</p>
The Dayside Ionosphere of Mars as controlled by the Game Between Solar Wind Dynamic Pressure and Crustal Magnetic Field Strength
<p>Including all 276 profiles like those shown in Figure 2.</p>
VOYAGER 2 SOLAR WIND MAGNETIC FIELD HGCOORDS HOUR AVGS V1.0
This dataset contains Voyager 2 magnetometer data from the interplanetary cruise averaged to 1 hour samples in Heliographic coordinates.
VOYAGER 1 SOLAR WIND MAGNETIC FIELD HGCOORDS 48SEC AVG V1.0
This dataset contains Voyager 1 magnetometer data from the interplanetary cruise averaged to 48 second samples in Heliographic coordinates.
OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 5 min Data
Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 5 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005
Wind Magnetic Fields Instrument (MFI) Magnetic Field Vector and Spacecraft Position, Key Parameter (K0), 92 s Data
Wind Magnetic Fields Investigation, MFI, Key Parameter magnetic field data in GSE and GSM coordinates.References:* 1. Panetta P, GSFC, GGS Wind MFI Operators Manual, September 15, 1992.* 2. Computer Sciences Corporation, Data Format Control Document, DFCD, between the International Solar-Terrestrial Physics, ISTP, program information investigators, CSC/TR-91/6014, 560-1DFD/0190, July 1992.* 3. Behannon, K.W., International Solar Terrestrial Physics, ISTP, program investigator data analysis requirements for Wind and Geotail spacecraft magnetometer experiment, September 1987.
OMNI, Combined Solar Wind Plasma Moments and Interplanetary Magnetic Field (IMF) Time-Shifted to the Nose of the Earth's Bow Shock, plus Geomagnetic Indices, 1 min Data
Near-Earth Heliospheric Data, OMNI, Definitive Multispacecraft Interplanetary Parameters Data, 1 min averagedAdditional information for all parameters are available from OMNI Data Documentation: https://omniweb..sci.gsfc.nasa.gov/html/HROdocum.htmlNew data may be accesible via the Space Physics Data Facility, SPDF, OMNIWeb Service: https://omniweb.gsfc.nasa.gov/ow_min.htmlThe Modified (Level-3) High Resolution OMNI data files are made in the same format as the OMNI files based on SWE Key Parameter data. There are a few differences between old and new high resolution OMNI data sets:* 1) In the newly modified Level-3 OMNI data files, we used the Wind SWE plasma definitive data rather than the Wind SWE plasma KP-despiked data. Using the definitive data give us possibility to include the Alpha/Proton Density Ratio and to use more accurate plasma parameters. However, the time coverage in the new OMNI data was decreased by from 2% to 10%. See the data description at https://spdf.gsfc.nasa.gov/pub/data/omni/high_res_omni/modified/. For detail comparison 1 min SWE definitive and cross-normalized SWE Key Parameter data sets, see https://omniweb.gsfc.nasa.gov/ftpbrowser/wind_pla_def_kp_norm.html.* 2) To keep the number of words and the record lengths the same as in the old OMNI high resolution data set, we replaced the PCN Index (word #45) in the ASCII records with the new Alpha/Proton Density Ratio parameter.* 3) The latest date for these new data is usually behind of the OMNI based on SWE_KP data.Modifications:* 1) Conversion to ISTP/IACG CDFs via SKTEditor, February 2000* 2) Time tags in CDAWeb version were modified to use the CDAWeb convention of having mid-average time tags rather than OMNI original convention of start-of-average time tags, March 2005
VOYAGER 2 SOLAR WIND MAGNETIC FIELD HGCOORDS 48SEC AVG V1.0
This dataset contains Voyager 2 magnetometer data from the interplanetary cruise averaged to 48 second samples in Heliographic coordinates.
Wind Magnetic Field Investigation (MFI) 15-sec magnetic field data, solar wind only
Data consist of 15-sec averages of magnetic field magnitude and GSE Cartesian components, from the MFI magnetometer on Wind. Data are for only the solar wind phases of the Wind orbit.
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OpenNeuro
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