Mike Marsh; S. Dalla; T. Laitinen; M. Dierckxsens; N. B. Crosby Jeremiah Horrocks Institute, University of Central Lancashire, Preston,

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Mike Marsh; S. Dalla; T. Laitinen; M. Dierckxsens; N. B. Crosby Jeremiah Horrocks Institute, University of Central Lancashire, Preston, UK See Marsh et al., 2014, SpWea, submitted, arXiv:

SPARX: Test particle SEP modelling Advantages: ‣ Physics based modelling ‣ Particle propagation determined by solution of equations of motion alone, for large number of test particles. ‣ Naturally 3D: describes cross-field transport and includes drifts ‣ No assumption of field line tied propagation. Model setup: Initial shock-like spatial and power law energy distributions are specified. Simple Parker IMF. Solar rotation included. Scattering determined by prescribed mean free path =0.3 AU.

Operational running Part of the COMESEP Alert System ( Triggered by automated detection of a solar eruptive event Output database of pre-made runs of unit ‘tiles’ at given longitude/ latitude are combined to construct shock-like injection region at 2 AU

SPARX Output ‣ Uses empirical scaling with SXR flare peak flux to ‘normalise’ particle counts ‣ Simulated X10-class flare ‣ Source region N20 ‣ 3 observers at 1 AU with relative views of source at W60, W20, E20 ‣ Use information on location and velocity to build synthetic flux profiles at 1 AU t = 1 hrt = 24 hrs t = 48 hrs t = 72 hrs

E20W20 W60 E>10 MeV E>60 MeV SPARX Output SPARX output products: Flux profile vs time Time of maximum flux Peak flux Event duration Synthetic flux profiles are calculated at 3 observer locations at 1 AU to simulate the event originating at locations relative to the Sun-Observer line (60W, 20W, 20E). Note the change in profile morphology with observer longitude due to the corotating energetic particle stream.