We have recently studied the development of an eruptive filament-driven,
large-scale off-limb coronal bright front (OCBF) in the low solar corona
(Kozarev et al. 2015), using remote observations from Solar Dynamics
Observatory's Advanced Imaging Assembly EUV telescopes. In that study, we
obtained high-temporal resolution estimates of the OCBF parameters regulating
the efficiency of charged particle acceleration within the theoretical
framework of diffusive shock acceleration (DSA). These parameters include the
time-dependent front size, speed, and strength, as well as the upstream coronal
magnetic field orientations with respect to the front's surface normal
direction. Here we present an analytical particle acceleration model,
specifically developed to incorporate the coronal shock/compressive front
properties described above, derived from remote observations. We verify the
model's performance through a grid of idealized case runs using input
parameters typical for large-scale coronal shocks, and demonstrate that the
results approach the expected DSA steady-state behavior. We then apply the
model to the event of May 11, 2011 using the OCBF time-dependent parameters
derived in Kozarev et al. (2015). We find that the compressive front likely
produced energetic particles as low as 1.3 solar radii in the corona. Comparing
the modeled and observed fluences near Earth, we also find that the bulk of the
acceleration during this event must have occurred above 1.5 solar radii. With
this study we have taken a first step in using direct observations of shocks
and compressions in the innermost corona to predict the onsets and intensities
of SEP events.
