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11 results for “Solar energetic particles”
Spatial distributions of Solar Energetic Particle Fe ions at t=12 h
<p>These images are supplementary to Figure 2 of the publication entitled "Solar Energetic Particle drifts and the energy dependence of 1 AU charge states" by S. Dalla, M.S. Marsh, M. Battarbee, accepted by Astrophysical Journal (2016). The paper is also available at https://arxiv.org/abs/1610.05104.</p> <p>In each figure contour plots of locations of Fe ions of charges Q=20, 16, 12 and 8 at time t=12 hr are shown. The first image gives z vs r_xy projections and the second figure y vs x projections, with only particles within 20 degrees of the heliographic equator included in the x-y projections.</p>
SERPENTINE catalog of solar energetic particle events observed by Helios
<p>This catalog contains multi-spacecraft solar energetic particle (SEP) events, which were observed by Helios. It has been created within the European Union’s Horizon 2020 project <em>SERPENTINE</em> (Solar energetic particle analysis platform for the inner heliosphere). This catalogue is based on data from the Helios mission provided by the previous European project <a href="https://sepserver.eu/index.php?page=catalogue">SEPServer</a>. In addition, technical reports of the University of Kiel from the time of Helios observation (printed version) were used, but the final judgement was done on the basis of the data from SEPServer.</p> <div> <p>It is not the first time that data from this historical mission are included in a statistical study. In Lario et al., 2006 (<a href="https://doi.org/10.1086/508982">https://doi.org/10.1086/508982</a>) some events observed by two or more spacecraft were analyzed from the point of view of their longitudinal and radial spread. The events where protons with energies above 13 MeV were observed by the Helios spacecraft when they were located at less than ~0.85 AU from the Sun were in the focus of the ESA SOL2UP project (for details see Pacheco, 2019, PhD Thesis, <a href="http://hdl.handle.net/10803/667033">http://hdl.handle.net/10803/667033</a>). The events from our catalogue which overlap with these previous studies are marked by letters L or P, correspondingly. At the same time, the data related to the overlapping events (same as for all other events), either characterizing the solar source, location of the observer (spacecraft) or relating to the properties of the particle fluxes were identified independently for the present catalogue. Nevertheless, we would like to acknowledge the authors of the previous SOL2UP project for providing us with the results of their studies.</p> <p>In the majority of the cases the identification of the location of the solar source was based on the available X-ray data of the related solar flare, published in (<a href="https://www.ngdc.noaa.gov">Solar Geophysical Data</a>). In addition, we used information from a previous study of Helios events (Kallenrode 1997, private communication), marked with the “K” sign. The radial distance of the spacecraft from the Sun, the solar wind speed and the Earth-Sun-spacecraft angle were taken from (<a href="https://cdaweb.gsfc.nasa.gov">CDAweb</a>). If there were no data for the solar wind speed during the time of the event, a standard value of 400 km/s was used (in the list itself and in the calculation of the longitude of the magnetic footpoint of the spacecraft). If there was, e.g., a high speed stream of the solar wind close to the time of the event then the average value of the solar wind stream was used. In both cases we used the “~” sign to denote such uncertainties. The location of the footpoint of the spacecraft of the solar disc was obtained by using a simple ballistic back mapping. The proton onset times are based on the SEPServer data.</p> <p> </p> </div> <p>The csv files provided here are archived versions of the <strong>dynamic catalog available at <a href="https://data.serpentine-h2020.eu/catalogs/sep-helios/">https://data.serpentine-h2020.eu/catalogs/sep-helios/</a></strong></p> <p> </p>
On the seed population of solar energetic particles in the inner heliosphere : simulation data
<p>Figures and simulation data of the paper titled 'On the seed population of solar energetic particles in the inner heliosphere', which is submitted to the <em>Journal of Geophysical Research: Space Physic</em>s. The simulation data consist of all the output from the EUHFORIA model and the PARADISE model that was used in the paper. The abstract of the paper is:</p> <p><em>Particles measured in large gradual solar energetic particle (SEP) events are believed to be predominantly accelerated at shocks driven by coronal mass ejections (CMEs). Ion charge state and composition analyses suggest that the origin of the seed particle population for the mechanisms of particle acceleration at CME-driven shocks is not the bulk solar wind thermal material, but rather a suprathermal population present in the solar wind. This suprathermal population could result from remnant material accelerated in prior solar flares and/or preceding CME-driven shocks. In this work, we examine the distribution of this suprathermal particle population in the inner heliosphere by combining a magnetohydrodynamic (MHD) simulation of the solar wind and a Monte-Carlo simulation of particle acceleration and transport. Assuming that the seed particles are uniformly distributed near the Sun by solar flares of various magnitudes, we study the longitudinal distribution of the seed population at multiple heliocentric distances. We consider a non-uniform background solar wind, consisting of fast and slow streams that lead to compression and rarefaction regions within the solar wind. Our simulation shows that the seed population at a particular location (e.g., 1 au) is strongly modulated by the underlying solar wind configuration. Corotating interaction regions (CIRs) and merged interactions regions (MIRs) can strongly alter the energy spectra of the seed particle populations. In addition, cross-field diffusion plays an important role in mitigating strong variations of the seed population in both space and energy. </em></p>
Dataset of Numerical prediction of changes in atmospheric chemical compositions during a solar energetic particle event on Mars
<p>This dataset contains the input parameters and the simulated results used for figures in the paper "Numerical prediction of changes in atmospheric chemical compositions during a solar energetic particle event on Mars" by Y. Nakamura, F. Leblanc, N. Terada, S. Hiruba, I. Murata, H. Nakagawa, S. Sakai, S. Aoki, A. Piccialli, Y. Willame, L. Neary, A. C. Vandaele, K. Murase, and R. Kataoka.</p> <p>Detailed informations about the data files can be found in "README.txt".</p>
SERPENTINE catalog of solar cycle 25 multi-spacecraft solar energetic particle events
<p>This catalog contains multi-spacecraft solar energetic particle (SEP) events, which were observed with the new heliospheric spacecraft fleet in solar cycle 25. It has been created within the European Union’s Horizon 2020 project <em>SERPENTINE</em> (Solar energetic particle analysis platform for the inner heliosphere). The catalog comprises key SEP characteristics observed by five different observer locations as provided by <em>Solar Orbiter, Parker Solar Probe, STEREO A, Wind</em> and <em>SOHO</em> (at the Lagrangian point 1), and <em>BepiColombo</em>. It focuses on large events, which show energetic proton increases above 25 MeV observed at least at two spacecraft. The catalog provides not only key parameters of the proton event but also the same parameters for 1 MeV and 100 keV electrons, respectively.</p> <p>For more information, and if you use this catalog, please refer to the corresponding publication:</p> <blockquote> <p>The solar cycle 25 multi-spacecraft solar energetic particle event catalog of the SERPENTINE project<br>N. Dresing, A. Yli-Laurila, S. Valkila, J. Gieseler, D. E. Morosan, G. U. Farwa, Y. Kartavykh, C. Palmroos, I. Jebaraj, S. Jensen, P. Kühl, B. Heber, F. Espinosa, R. Gómez-Herrero, E. Kilpua, V.-V. Linho, P. Oleynik, L. A. Hayes, A. Warmuth, F. Schuller, H. Collier, H. Xiao, E. Asvestari, D. Trotta, J. G. Mitchell, C. M. S. Cohen, A. W. Labrador, M. E. Hill and R. Vainio<br>A&A, 687 (2024) A72<br>DOI: <a href="https://doi.org/10.1051/0004-6361/202449831">10.1051/0004-6361/202449831</a>, arXiv:<a href="https://arxiv.org/abs/2403.00658">2403.00658</a>. </p> </blockquote> <p>The csv files provided here are archived versions of the dynamic catalog available at <a href="https://data.serpentine-h2020.eu/catalogs/sep-sc25/">https://data.serpentine-h2020.eu/catalogs/sep-sc25/</a></p> <p>Provided are two semicolon-separated csv files containing the same data. The only difference is that the file <em>sep-sc25_extended_header.csv </em>includes an extensive header.</p> <ul> <li>Field descriptions <ul> <li>id: ID</li> <li>science_case: Science case</li> <li>date: Event date [UTC]</li> <li>flare_time: Flare time [UTC]</li> <li>flare_lat: Flare Carrington latitude [deg]</li> <li>flare_lon: Flare Carrington longitude [deg]</li> <li>flare_class: Flare class (GOES)</li> <li>flare_comments: Flare Comments</li> <li>radio_type2: Radio type II bursts</li> <li>decametric_type2_start: Decametric type II burst start time [UT]</li> <li>decametric_type2_stop: Decametric type II burst end time [UT]</li> <li>decametric_type2_freq_range: Decametric type II frequency range [MHz]</li> <li>radio_type2_start: Metric radio type II burst start time [UT]</li> <li>radio_type2_stop: Metric radio type II burst end time [UT]</li> <li>radio_type2_freq_range: Frequency range of metric type II burst [MHz]</li> <li>radio_imaging_available: Metric radio imaging available</li> <li>radio_comments: Radio comments</li> <li>cme_id: Associated CMEs</li> <li>solar_mach_link: Solar-Mach link</li> </ul> </li> </ul> <ul> <li>S/C codes <ul> <li>BepiC: BepiColombo</li> <li>L1: L1 (SOHO/Wind)</li> <li>PSP: Parker Solar Probe</li> <li>STA: STEREO A</li> <li>SolO: Solar Orbiter</li> </ul> </li> </ul> <ul> <li>S/C related field descriptions <ul> <li>{sc}_sc_lat: S/C Carrington latitude [deg]</li> <li>{sc}_sc_lon: S/C Carrington longitude [deg]</li> <li>{sc}_dist: S/C radial distance [au]</li> <li>{sc}_ip_shock_id: Associated IP shocks</li> <li>{sc}_p25MeV_onset_date: S/C protons 25 MeV onset date [UTC]</li> <li>{sc}_p25MeV_onset_time: S/C protons 25 MeV onset time [UTC]</li> <li>{sc}_p25MeV_onset_time_formatted: S/C protons 25 MeV onset time [UTC] (Formatted)</li> <li>{sc}_p25MeV_onset_averaging: S/C protons 25 MeV averaging used for onset [min]</li> <li>{sc}_p25MeV_onset_sector: S/C protons 25 MeV sector used for onset</li> <li>{sc}_p25MeV_peak_date: S/C protons 25 MeV peak date [UTC]</li> <li>{sc}_p25MeV_peak_time: S/C protons 25 MeV peak time [UTC]</li> <li>{sc}_p25MeV_peak_time_formatted: S/C protons 25 MeV peak time [UTC] (Formatted)</li> <li>{sc}_p25MeV_peak_flux: S/C protons 25 MeV peak flux [cm^-2 s^-1 sr^-1 MeV^-1]</li> <li>{sc}_p25MeV_peak_flux_formatted: S/C protons 25 MeV peak flux [cm^-2 s^-1 sr^-1 MeV^-1] (Formatted)</li> <li>{sc}_p25MeV_peak_averaging: S/C protons 25 MeV averaging used for peak [min]</li> <li>{sc}_p25MeV_peak_sector: S/C protons 25 MeV sector used for peak</li> <li>{sc}_p25MeV_injection_date: S/C protons 25 MeV inferred injection date [UTC]</li> <li>{sc}_p25MeV_injection_time: S/C protons 25 MeV inferred injection time [UTC]</li> <li>{sc}_p25MeV_pathlength: S/C protons 25 MeV path length used for inferred injection time [au]</li> <li>{sc}_p25MeV_sw_speed: S/C protons 25 MeV onset solar wind speed [km/s]</li> <li>{sc}_p25MeV_comments: S/C protons 25 MeV comments</li> <li>{sc}_e100keV_onset_date: S/C electrons 100 keV onset date [UTC]</li> <li>{sc}_e100keV_onset_time: S/C electrons 100 keV onset time [UTC]</li> <li>{sc}_e100keV_onset_time_formatted: S/C electrons 100 keV onset time [UTC] (Formatted)</li> <li>{sc}_e100keV_onset_averaging: S/C electrons 100 keV averaging used for onset [min]</li> <li>{sc}_e100keV_onset_sector: S/C electrons 100 keV sector used for onset</li> <li>{sc}_e100keV_peak_date: S/C electrons 100 keV peak date [UTC]</li> <li>{sc}_e100keV_peak_time: S/C electrons 100 keV peak time [UTC]</li> <li>{sc}_e100keV_peak_time_formatted: S/C electrons 100 keV peak time [UTC] (Formatted)</li> <li>{sc}_e100keV_peak_flux: S/C electrons 100 keV peak flux [cm^-2 s^-1 sr^-1 MeV^-1]</li> <li>{sc}_e100keV_peak_flux_formatted: S/C electrons 100 keV peak flux [cm^-2 s^-1 sr^-1 MeV^-1] (Formatted)</li> <li>{sc}_e100keV_peak_averaging: S/C electrons 100 keV averaging used for peak [min]</li> <li>{sc}_e100keV_peak_sector: S/C electrons 100 keV sector used for peak</li> <li>{sc}_e100keV_injection_date: S/C electrons 100 keV inferred injection date [UTC]</li> <li>{sc}_e100keV_injection_time: S/C electrons 100 keV inferred injection time [UTC]</li> <li>{sc}_e100keV_pathlength: S/C electrons 100 keV path length used for inferred injection time [au]</li> <li>{sc}_e100keV_sw_speed: S/C electrons 100 keV onset solar wind speed [km/s]</li> <li>{sc}_e100keV_comments: S/C electrons 100 keV comments</li> <li>{sc}_e1MeV_onset_date: S/C electrons 1 MeV onset date [UTC]</li> <li>{sc}_e1MeV_onset_time: S/C electrons 1 MeV onset time [UTC]</li> <li>{sc}_e1MeV_onset_time_formatted: S/C electrons 1 MeV onset time [UTC] (Formatted)</li> <li>{sc}_e1MeV_onset_averaging: S/C electrons 1 MeV averaging used for onset [min]</li> <li>{sc}_e1MeV_onset_sector: S/C electrons 1 MeV sector used for onset</li> <li>{sc}_e1MeV_peak_date: S/C electrons 1 MeV peak date [UTC]</li> <li>{sc}_e1MeV_peak_time: S/C electrons 1 MeV peak time [UTC]</li> <li>{sc}_e1MeV_peak_time_formatted: S/C electrons 1 MeV peak time [UTC] (Formatted)</li> <li>{sc}_e1MeV_peak_flux: S/C electrons 1 MeV peak flux [cm^-2 s^-1 sr^-1 MeV^-1]</li> <li>{sc}_e1MeV_peak_flux_formatted: S/C electrons 1 MeV peak flux [cm^-2 s^-1 sr^-1 MeV^-1] (Formatted)</li> <li>{sc}_e1MeV_peak_averaging: S/C electrons 1 MeV averaging used for peak [min]</li> <li>{sc}_e1MeV_peak_sector: S/C electrons 1 MeV sector used for peak</li> <li>{sc}_e1MeV_injection_date: S/C electrons 1 MeV inferred injection date [UTC]</li> <li>{sc}_e1MeV_injection_time: S/C electrons 1 MeV inferred injection time [UTC]</li> <li>{sc}_e1MeV_pathlength: S/C electrons 1 MeV path length used for inferred injection time [au]</li> <li>{sc}_e1MeV_sw_speed: S/C electrons 1 MeV onset solar wind speed [km/s]</li> <li>{sc}_e1MeV_comments: S/C electrons 1 MeV comments</li> <li>{sc}_ep_ratio: Ratio of Electrons (~1MeV) / Protons (25-40 MeV)</li> </ul> </li> </ul> <div> </div> <div><strong>CHANGELOG:</strong></div> <div> <ul> <li>2025-06-05 <ul> <li>Updated peak fluxes and peak times of PSP 1 MeV electrons, as well as PSP's e/p ratios (the previous flux values are erroneous!)</li> </ul> </li> <li>2024-09-06 <ul> <li>Flare information has been updated</li> <li>Updated cme_id info corresponding to updated CME catalog</li> <li>(Zenodo version only: change file format from "semicolon separated" to "comma separated, with fields containing commas surrounded by quotes")</li> </ul> </li> <li>2024-05-24<br> <ul> <li>Events 35, 36: flare times (GOES) were incorrectly provided as peak times. They have been changed to start times (like for all flares).</li> <li>All 8 events where SOLO/STIX has been used for flare determination had been time shifted to the Sun. Now they are shifted to 1 AU to be consistent with the GOES times.</li> </ul> </li> </ul> </div>
Dataset for "Extreme Energetic Particle Events by Superflare Associated CMEs from Solar-like Stars"
<p>Here we present the simulation results (time-intensity profiles and event integrated fluence spectra) for the paper "Extreme Energetic Particle Events by Superflare Associated CMEs from Solar-like Stars". Detailed descriptions of the simulation settings can be found in the manuscript. </p>
SEP list and effective dose of paper "The radiation impact of Solar Energetic Particle Events on the Moon: A statistical study using data-based modeling results"
Open the record for dataset details and reuse information.
ACE Electron, Proton, and Alpha Monitor (EPAM) Solar Wind Plasma Energetic Particle Fluxes, Key Parameter (K1), 1 h Data
ACE Browse Data are designed for monitoring large-scale Particle and Field Behavior and for selecting interesting Time Periods. The Data are automatically generated from the Spacecraft Data Stream using simple Algorithms provided by the Instrument Teams. It is not routinely checked for Accuracy and is subject to Revision. Use this Data at your own Risk, and consult with the appropriate Instrument Teams about citing it. EPAM Browse Data are not validated by the Experimenters and should not be used except for Preliminary Examination prior to detailed Studies. ACE Electron, Proton, and Alpha Monitor (EPAM) References: http://www.srl.caltech.edu/ACE/.
ACE Electron, Proton, and Alpha Monitor (EPAM) Solar Wind Plasma Energetic Particle Fluxes, Key Parameter (K0), 5 min Data
ACE Browse Data are designed for monitoring large-scale Particle and Field Behavior and for selecting interesting Time Periods. The Data are automatically generated from the Spacecraft Data Stream using simple Algorithms provided by the Instrument Teams. It is not routinely checked for Accuracy and is subject to Revision. Use this Data at your own Risk, and consult with the appropriate Instrument Teams about citing it. EPAM Browse Data are not validated by the Experimenters and should not be used except for Preliminary Examination prior to detailed Studies. ACE Electron, Proton, and Alpha Monitor (EPAM) References: http://www.srl.caltech.edu/ACE/.
ACE Solar Energetic Particle Ionic Charge Analyzer (SEPICA) Energetic Ion Flux Intensities Values and Uncertainties, Level 2 (H2), 1 h Data
This Data Product contains Measurements from the ACE Solar Energetic Particle Ionic Charge Analyzer (SEPICA) Instrument. SEPICA is used to determine the Charge State Distribution of Energetic Particle Distributions. SEPICA is designed to measure the Ionic Charge State, Q, the Kinetic Energy, E, and the Nuclear Charge, Z, of Energetic Ions above 0.2 MeV/n. This includes Ions accelerated in Solar Flares as well as in Interplanetary Space during Energetic Storm Particle (ESP) Events and Co-rotating Interaction Region (CIR) Events. For low Mass Numbers, SEPICA also separates Isotopes such as 3He and 4He. The Quality of the ACE Level 2 Data are such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication.
Wind EPACT/LEMT 1-Hr He,C,O,Ne,Si,Fe Solar Energetic Particle Intensities Level 2 Data
Hourly-averaged fluxes of He, C, O Ne,Si, Fe nuclei in the general range 2-11 MeV/n. Poisson uncertainties are given for each flux.
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