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Acceleration and Storage of Energetic Electrons in Magnetic Loops in the Course of Electric Current Oscillations by V.V. Zaitsev and A.V. Stepanov

31 Oct 2017, 11:02 UTC
Acceleration and Storage of Energetic Electrons in Magnetic Loops in the Course of Electric Current Oscillations  by V.V. Zaitsev and A.V. Stepanov
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There are long-lived radio events on the Sun and stars like in type IV solar radio bursts with sudden reductions and pulsating type III bursts (Slottje, 1972; Huang et al. 2016) as well as intriguing intense radio emission from ultracool stars that lasts for several rotation periods (Hallinan et al. 2007). This can be the result of the multiple injections of accelerated electrons into the coronal magnetic loops. The idea of the acceleration and storage of energetic electrons in the magnetic loops in the course of electric current oscillations was suggested by Zlotnik et al. (2003). This idea is developed here on the base of the analogy of the coronal loop with a RLC-circuit and on the modern observations.
Excitation of Induced Electric Field
Convective motions of the photosphere matter interacting with the magnetic field near the loop legs generate the electric current in the loop. The current-carrying coronal loop can be presented as an electric (RLC) circuit whose eigen frequency depends on the magnitude of the electric current $I_0$, the electron density $n$, the loop radius $r_0$, and the length $l$ of the loop (Zaitsev et al. 1998):
\[
\nu_{\rm{RLC}}=\frac{c}{2\pi \sqrt{LC(I_0)}} \approx \frac{1}{2\pi \sqrt{2\pi \zeta}} \frac{I_0}{c r_0^2 \sqrt{nm_i}}, \zeta=\ln ...

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