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\begin{document}

\title{Solar Wind with Field Lines and Energetic Particles (SOFIE) Model:
Application to Historical Solar Energetic Particle Events}



\author[1]{Lulu Zhao}%
\author[1]{Igor V. Sokolov}%
\author[2]{Tamas I. Gombosi}%
\author[3]{David Lario}%
\author[4]{Kathryn Whitman}%
\author[2]{Zhenguang Huang}%
\author[2]{Gabor Toth}%
\author[2]{Ward Beecher Manchester  IV}%
\author[2]{Bartholomeus van der Holst}%
\author[5]{Nishtha Sachdeva}%
\affil[1]{University of Michigan}%
\affil[2]{University of Michigan-Ann Arbor}%
\affil[3]{Johns Hopkins University}%
\affil[4]{U. Houston}%
\affil[5]{U. Michigan}%


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  \date{June 14, 2024}


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\begin{abstract}
In this paper, we demonstrate the applicability of the data-driven and
self-consistent solar energetic particle model, Solar-wind with
FIeld-lines and Energetic-particles (SOFIE), to simulate acceleration
and transport processes of solar energetic particles. SOFIE model is
built upon the Space Weather Modeling Framework (SWMF) developed at the
University of Michigan. In SOFIE, the background solar wind plasma in
the solar corona and interplanetary space is calculated by the
Aflv\textbackslash{}'en Wave Solar-atmosphere Model(-Realtime) (AWSoM-R)
driven by the near-real-time hourly updated Global Oscillation Network
Group (GONG) solar magnetograms. In the background solar wind, coronal
mass ejections (CMEs) are launched by placing an imbalanced magnetic
flux rope on top of the parent active region, using the Eruptive Event
Generator using Gibson-Low model (EEGGL). The acceleration and transport
processes are modeled by the Multiple-Field-Line Advection Model for
Particle Acceleration (M-FLAMPA). In this work, nine solar energetic
particle events (Solar Heliospheric and INterplanetary Environment
(SHINE) challenge/campaign events) are modeled. The three modules in
SOFIE are validated and evaluated by comparing with observations,
including the steady-state background solar wind properties, the
white-light image of the CME, and the flux of solar energetic protons,
at energies of \$\textbackslash{}ge\$ 10 MeV.%
\end{abstract}%



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