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\begin{document}

\title{Fully Kinetic Simulations of Radio Emission from a Propagating Electron
Beam}



\author[1]{Tien Vo}%
\author[2]{Vadim Roytershteyn}%
\author[3]{Cynthia Cattell}%
\affil[1]{University of Minnesota Twin Cities}%
\affil[2]{Space Science Institute}%
\affil[3]{University of Minnesota}%


\vspace{-1em}



  
  \date{June 18, 2024}


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\begin{abstract}
Type III radio bursts are associated with energetic electrons
accelerated by solar flares from the lower corona. The standard theory
links these emissions to a conversion of plasma oscillations excited by
the bump-on-tail instability into electromagnetic waves. Since electron
beams can propagate to large heliospheric distances and continue to emit
radio waves, the instability must be finely balanced, not to disrupt
their propagation (so-called Sturrock's dilemma). To explain this, many
models invoking contrasting processes have been proposed (e.g.
quasilinear vs strong turbulence description of interactions between
various plasma modes). In this study, we perform 2D PIC simulations of
beam injection, propagation, and emissions in a large system without
periodic boundary conditions. Results demonstrate that the beam
decouples from the excited electrostatic oscillations near the injection
site and propagates through the background plasma with relatively small
energy loss. Downstream, the instability continues to operate only at
the beam front. The main body of the beam between downstream and
upstream reaches a quasi-steady state. It may become unstable again
where the background plasma is colder or less dense. Background
temperature variations affect the beam instability more than background
density fluctuations. Radio emissions at plasma frequency and its second
harmonic are primarily generated upstream in the region of intense
fluctuations, where both classical signatures of three-wave conversion
processes and those associated with modulational instability are
detected. Our results are consistent with satellite data showing that
electron beams often continue to generate type III radio bursts even
beyond 1 AU. They illustrate in a first-principle model how a beam state
consistent with subsequent quasilinear relaxation emerges shortly after
beam injection.%
\end{abstract}%



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