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SEPSTER2D (v1)SEP prediction inspired by STEREO observations 2DModel DescriptionSEPSTER2D is an empirical model to predict SEP event-integrated and peak intensity spectra between 10 and 130 MeV at 1AU, assuming an energy-dependent 2D Gaussian spatial distribution, and accounting for the correlation between the intensity and the speed of the parent CME, and the magnetic-field-line connection angle. The magnetic footpoints of the IMF field lines passing through the observer (Earth, STEREO-A and -B) are estimated at CME first appearance time and at a 2.5 Rs radial distance based on a simple IMF Parker spiral model. Model Figure(s) :Model Inputs DescriptionCME speed, direction and first appearance time from DONKI; solar wind speed from ACE/DSCOVR/STEREO Model Outputs DescriptionSEP peak and event-integrated intensities (both differential and energy-integrated) above 10 MeV, along with corresponding uncertainties. Time of peak intensity (added in version 1.1 and later) Model CaveatsPredicted intensities are expected to overestimate the observations for relatively slow (<600km/s) CMEs and narrow SEP events. SEP intensities above 130 MeV are based on spectral extrapolations and are characterized by large uncertainties. Change LogUpgraded to Version 1.1 on March 21, 2022 at the CCMC. List of changes includes: - Calculation of peak intensity times added Upgraded to Version 1.2 on July 3, 2023 at the CCMC. List of changes includes: - Solar wind speed is now calculated individually for each CME, paying attention to data gaps. - For historical events, the OMNI dataset via CDAWEB HAPI API is now being used. - For real-time runs, the iSWA HAPI API is now being used to fetch real-time solar wind data. - A correction factor has been implemented to fix the model prediction overestimate for relatively slow CMEs. - Added calculation of SEP event end times. Version 1.3 includes a fix to filter out and prevent invalid, elevated solar wind speeds from being used for the predictions, and a change to use the Leading Edge (LE) CME measurements only for SEPSTER2D predictions. Model Acknowledgement/Publication Policy (if any)Bruno, A., Richardson, I.G. Empirical Model of 10-30 MeV Solar Energetic Particle Spectra at 1 AU Based on Coronal Mass Ejection Speed and Direction. Sol Phys 296, 36 (2021). https://doi.org/10.1007/s11207-021-01779-4 Model Domains:Heliosphere.Inner_HeliosphereSpace Weather Impacts:Solar energetic particles - SEPs (human exploration, aviation safety, aerospace assets functionality)Phenomena :Solar_Energetic_ParticlesSimulation Type(s):EmpiricalTemporal Dependence Possible? (whether the code results depend on physical time?)falseModel is available at?CCMCSource code of the model is publicly available?falseCCMC Model Status (e.g. onboarding, use in production, retired, only hosting output, only source is available):productionCode Language:C/C++Regions (this is automatically mapped based on model domain):Heliosphere.InnerContacts :Alessandro.Bruno, ModelDeveloperIan.Richardson, ModelDeveloper M.Leila.Mays, ModelHostContact Acknowledgement/Institution :Relevant Links :SRAG one-pager description: https://ccmc.gsfc.nasa.gov/static/files/SEPSB/SEP-one-pager_SEPSTER.pdfPublications :Model Access Information :Access URL: https://iswa.gsfc.nasa.gov/iswa_data_tree/model/heliosphere/sep_scoreboard/SEPSTER2D/1.X/Access URL Name: Continuous/RT Run (ISWA data tree) Repository ID: spase://CCMC/Repository/NASA/GSFC/CCMC Availability: online AccessRights: OPEN Format: HTML Encoding: None Access URL: https://sep.ccmc.gsfc.nasa.gov/intensity/ Access URL Name: Continuous/RT Run (SEP Scoreboard Intensity) Repository ID: spase://CCMC/Repository/NASA/GSFC/CCMC Availability: online AccessRights: OPEN Format: HTML Encoding: None Linked to Other Spase Resource(s) (example: another SimulationModel) : |
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