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Electron beams accelerated in solar flares and escaping from the Sun alongopen magnetic field lines can trigger intense radio emissions known as type IIIsolar radio bursts. Utilizing observations by Parker Solar Probe (PSP),STEREO-A (STA), Solar Orbiter (SolO), and Wind spacecrafts, the speeds andaccelerations of type III exciters are derived for simple and isolated type IIIsolar bursts. For the first time, simultaneous four spacecraft observationsallow to determine positions, and correct the resulting velocities andaccelerations for the location between the spacecraft and the apparent source.We observe velocities and acceleration to change as $u(r) \propto r^{-0.37 \pm0.14}$ and $a(r) \propto r^{-1.71 \pm 0.20}$ with radial distance from the Sun$r$. To explain the electron beam deceleration, we develop a simple gas-dynamicdescription of the electron beam moving through plasma with monotonicallydecreasing density. The model predicts that the beam velocity decreases as$u(f)\propto f^{1/4}(r)$, so the acceleration changes $\propto r^{-1.58}$ (andspeed as $\propto r^{-0.29}$) for the plasma density profile $n(r)\proptor^{-2.3}$. The deceleration is consistent with the average observation valuescorrected for the type III source locations. Intriguingly, the observationsalso show differences in velocity and acceleration of the same type IIIobserved by different spacecrafts. We suggest the difference could be relatedto the additional time delay caused by radio-wave scattering between thespacecraft and the source.

A Multi-Spacecraft Analysis of Type III Radio Burst Electron Beam Deceleration and electron deceleration model in the inhomegeneous plasma