Tuesday

Solar electrons beams are accelerated in the corona and into the solar wind through mechanisms such as flares. These beams of non-thermal electrons evolve as a function of distance from the Sun, interacting with Langmuir waves as they propagate. Insight into electron beam transport effects allows us to disentangle them from the acceleration properties and provides a framework for using in situ measurements to diagnose coronal acceleration characteristics. Through beam-plasma structure simulations we study the interactions between these electron beams and the background plasma of the solar corona at different distances from the Sun. This allows us to determine what is the maximum electron velocity responsible for Langmuir wave production and growth, and consequently which electron energies that are. Understanding the mechanisms driving the change in the maximum electron velocity will permit more accurate predictions in electron onset times, relevant for space weather applications. Moreover, our radial predictions can be tested by in situ plasma measurements on-board Solar Orbiter and Parker Solar Probe.