http://arxiv.org/abs/1511.03123
During solar flares a large amount of electrons with energies greater than 20 keV is generated with a production rate of typically $10^{36}$ s$^{-1}$. A part of them is able to propagate along open magnetic field lines through the corona into interplanetary space. During their travel they emit radio radiation which is observed as type III radio bursts in the frequency range from 100 MHz down to 10 kHz by the WAVES radio spectrometer aboard the spacecraft WIND, for instance. From the drift rates of these bursts in dynamic radio spectra the radial propagation velocity $V_r$ of the type III burst exciting electrons is derived by employing a newly developed density model of the heliosphere. Calculations show that the radio radiation is emitted by electrons with different $V_r$ and therefore by different electrons of the initially produced electron distribution.
F. Breitling, G. Mann and C. Vocks
Wed, 11 Nov 15
8/72
Comments: 8 pages, 7 figures, conference; submitted Nov 26, 2010; accepted Mar 14, 2011; published Dec 2011
You must be logged in to post a comment.