Welcome to the new CCMC website!

Please note that some pages may have moved during the migration. If you experience any issues with the new website, please reach out to gsfc-ccmc-support@lists.hq.nasa.gov.

Last Updated: 05/26/2022

UMASEP

Version: v2.0

In general, the UMASEP scheme makes use of the lag-correlation of solar electromagnetic flux with the particle flux at near-earth. If the correlation is high, the model infers that there is a magnetic connection through which particles are arriving. If, additionally, the intensity of the flux of the associated solar event is also high, then the UMASEP scheme issues an SEP event prediction. UMASEP analyzes soft X-ray, differential and integral proton flux data in order to recognize precursors of three different proton flux situations: well-connected SEP events, poorly-connected SEP events, and "all-clear" situations.

There are five variations of the UMASEP model:

  • UMASEP-10 for predicting >10 MeV proton events (Núñez, 2011)
  • UMASEP-30 for predicting >30 MeV proton events
  • UMASEP-50 for predicting >50 MeV proton events
  • UMASEP-100 for predicting >100 MeV proton events (Núñez, 2015)
  • HESPERIA UMASEP-500 predicting GLE and >500 MeV proton events (Núñez et al, 2017)

These models correlate X-ray flux with each of the differential proton fluxes measured by the GOES satellites. When the correlation estimation surpasses a threshold, and the associated flare is greater than a specific X-ray peak flux, they predict SEP events in the aforementioned energies.

Inputs

GOES soft x-ray flux, GOES differential and integral proton flux.

The temporal cadence of the analyzed input data is 5 minutes in the case of UMASEP-10 and UMASEP-100, and 1 minute in the case of HESPERIA UMASEP-500.

Outputs

The five models predict SEP/GLE event occurrences. UMASEP-10, UMASEP-30, UMASEP-50 and UMASEP-100 also predict the peak SEP flux (HESPERIA UMASEP_500 does not predict the peak flux). The forecast window of these predictions are: 7 hours for >10 MeV protons (UMASEP-10), 6 hours for >30 MeV protons (UMASEP-30), 5 hours for >50 MeV protons (UMASEP-50), 3 hours for >100 MeV protons (UMASEP-100), and 1 hour for GLE/>500 MeV events (HESPERIA UMASEP-500).

Model is time-dependant.

Domains

  • Heliosphere / Inner Heliosphere

Space Weather Impacts

  • Near-earth radiation and plasma environment (aerospace assets functionality)
  • Solar energetic particles - SEPs (human exploration, aviation safety, aerospace assets functionality)

Publications

Code

Code Languages: Java

Contacts

Publication Policy

In addition to any model-specific policy, please refer to the General Publication Policy.