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\begin{document}

\title{Red Line Diffuse-Like Aurora Driven by Time Domain Structures Associated
with Braking Magnetotail Flow Bursts}



\author[1]{Yangyang Shen}%
\author[2]{Jun Liang}%
\author[3]{Anton V Artemyev}%
\author[1]{Vassilis Angelopoulos}%
\author[4]{Qianli Ma}%
\author[1]{Larry R. Lyons}%
\author[5]{Jiang Liu}%
\author[6]{Yukitoshi (Toshi) Nishimura}%
\author[7]{Xiao-Jia Zhang}%
\author[8]{Ivan Vasko}%
\author[9]{Donald L. Hampton}%
\affil[1]{University of California Los Angeles}%
\affil[2]{University of Calgary}%
\affil[3]{UCLA IGPP}%
\affil[4]{Center for Space Physics, Boston University, Boston, Massachusetts, USA}%
\affil[5]{IGPP, UCLA}%
\affil[6]{Boston University}%
\affil[7]{The University of Texas at Dallas}%
\affil[8]{University of Texas at Dallas}%
\affil[9]{University of Alaska Fairbanks}%


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  \date{May 21, 2024}


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\begin{abstract}
Magnetotail earthward-propagating fast plasma flows provide important
pathways for magnetosphere-ionosphere coupling. This study reexamines a
flow-related red-line diffuse-like aurora event previously reported by
Liang et al., (2011), utilizing THEMIS and ground-based auroral
observations from Poker Flat. We find that time domain structures (TDSs)
within the flow bursts efficiently drive electron precipitation below a
few keV, aligning with predominantly red-line auroral intensifications
in this non-substorm event. The diffuse-like auroras sometimes coexisted
with or potentially evolved from discrete forms. We forward model
red-line diffuse-like auroras due to TDS-driven precipitation, employing
the time-dependent TREx-ATM auroral transport code. The good correlation
(0.77) between our modeled and observed red line emissions underscores
that TDSs are a primary driver of the red-line diffuse-like auroras,
though whistler-mode wave contributions are needed to fully explain the
most intense red-line emissions.%
\end{abstract}%



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