  One of the most prominent sources for energetic particles in our solar system
are huge eruptions of magnetised plasma from the Sun called coronal mass
ejections (CMEs), which usually drive shocks that accelerate charged particles
up to relativistic energies. In particular, energetic electron beams can
generate radio bursts through the plasma emission mechanism, for example, type
II and accompanying herringbone bursts. Here, we investigate the acceleration
location, escape, and propagation directions of various electron beams in the
solar corona and compare them to the arrival of electrons at spacecraft. To
track energetic electron beams, we use a synthesis of remote and direct
observations combined with coronal modelling. Remote observations include
ground-based radio observations from the Nancay Radioheliograph (NRH) combined
with space-based extreme-ultraviolet and white-light observations from the
Solar Dynamics Observatory (SDO), the Solar Terrestrial Relations Observatory
(STEREO) and Solar Orbiter (SolO). We also use direct observations of energetic
electrons from the STEREO and Wind spacecraft. These observations are then
combined with a three-dimensional (3D) representation of the electron
acceleration locations that combined with results from magneto-hydrodynamic
models of the solar corona is used to investigate the origin and link of
electrons observed remotely at the Sun to in situ electrons. We observed a type
II radio burst followed by herringbone bursts that show single-frequency
movement through time in NRH images. The movement of the type II burst and
herringbone radio sources seems to be influenced by the regions in the corona
where the CME is more capable of driving a shock. We also found similar
inferred injection times of near-relativistic electrons at spacecraft to the
emission time of the type II and herringbone bursts.
