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One of the most prominent sources for energetic particles in our solar systemare huge eruptions of magnetised plasma from the Sun called coronal massejections (CMEs), which usually drive shocks that accelerate charged particlesup to relativistic energies. In particular, energetic electron beams cangenerate radio bursts through the plasma emission mechanism, for example, typeII and accompanying herringbone bursts. Here, we investigate the accelerationlocation, escape, and propagation directions of various electron beams in thesolar corona and compare them to the arrival of electrons at spacecraft. Totrack energetic electron beams, we use a synthesis of remote and directobservations combined with coronal modelling. Remote observations includeground-based radio observations from the Nancay Radioheliograph (NRH) combinedwith space-based extreme-ultraviolet and white-light observations from theSolar Dynamics Observatory (SDO), the Solar Terrestrial Relations Observatory(STEREO) and Solar Orbiter (SolO). We also use direct observations of energeticelectrons from the STEREO and Wind spacecraft. These observations are thencombined with a three-dimensional (3D) representation of the electronacceleration locations that combined with results from magneto-hydrodynamicmodels of the solar corona is used to investigate the origin and link ofelectrons observed remotely at the Sun to in situ electrons. We observed a typeII radio burst followed by herringbone bursts that show single-frequencymovement through time in NRH images. The movement of the type II burst andherringbone radio sources seems to be influenced by the regions in the coronawhere the CME is more capable of driving a shock. We also found similarinferred injection times of near-relativistic electrons at spacecraft to theemission time of the type II and herringbone bursts.

Connecting remote and in situ observations of shock-accelerated electrons associated with a coronal mass ejection