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We present a new empirical model to predict solar energetic particle (SEP)event-integrated and peak intensity spectra between 10 and 130 MeV at 1 AU,based on multi-point spacecraft measurements from the Solar TErrestrialRElations Observatory (STEREO), the Geostationary Operational EnvironmentalSatellites (GOES) and the Payload for Antimatter Matter Exploration andLight-nuclei Astrophysics (PAMELA) satellite experiment. The analyzed datasample includes 32 SEP events occurring between 2010 and 2014, with astatistically significant proton signal at energies in excess of a few tens ofMeV, unambiguously recorded at three spacecraft locations. The spatialdistributions of SEP intensities are reconstructed by assuming anenergy-dependent 2D Gaussian functional form, and accounting for thecorrelation between the intensity and the speed of the parent coronal massejection (CME), and the magnetic field line connection angle. The CMEmeasurements used are from the Space Weather Database Of Notifications,Knowledge, Information (DONKI). The model performance, including itsextrapolations to lower/higher energies, is tested by comparing with thespectra of 20 SEP events not used to derive the model parameters. Despite thesimplicity of the model, the observed and predicted event-integrated and peakintensities at Earth and at the STEREO spacecraft for these events showremarkable agreement, both in the spectral shapes and their absolute values.

Empirical Model of 10-130 MeV Solar Energetic Particle Spectra at 1 AU Based on Coronal Mass Ejection Speed and Direction