Abstract
Abstract. In this study, we report on the occurrence of solar Type III radio bursts recorded by radio and plasma wave experiment (RPWS) experiment onboard Cassini spacecraft. This instrument is designed to investigate the Saturn's plasma environment and sub-auroral radio missions. RPWS/Cassini experiment allows to measure electric field over a frequency range from 1 Hz to 16 MHz (Gurnett et al., 2004). The essential observed emission is associated to the Saturnian Kilometric Radiation (SKR) which is generated in the sub-auroral regions of the magnetosphere. The capability of this experiment leads to detect Solar Type III radio bursts recorded during the increase phase of the solar activity, i.e. January 2008 to December 2014. Hence we have found more than 300 Type III solar bursts when the distance of Cassini to the Sun was about 10 AU. Observational parameters like the time occurrence, the emission frequency and the relative intensity are considered in this analysis. Those features lead us to characterize the detection conditions and to estimate the occurrence variabilities of Type III bursts.
Highlights
The solar Type III radio bursts are generated by fast electron streams following opened magnetic field lines
In this work we investigate solar Type III bursts recorded by the radio and plasma wave experiment (RPWS) onboard Cassini spacecraft
We have investigated the occurrence of Type III radio bursts recorded by Cassini/RPWS experiment during seven years, i.e. from 2008 to 2014
Summary
The solar Type III radio bursts are generated by fast electron streams following opened magnetic field lines. It should be mentioned that the harmonic emission can better escape to the receiver in the interplanetary space than the fundamental one Those radio bursts allow the remote sensing of the plasma environment in the vicinity of the Sun. A simple way to estimate the plasma frequency is to use the well-known relation between the electron density de (cm−3) and the local plasma frequency fp (kHz), i.e. de ≈ 9fp1/2. They begin at a few hundred of megahertz and rapidly drift to low frequencies (i.e. about 30 kHz) which can be only observed from space This drift from high to low frequencies when the time increases is directly related to the electron density decrease from the solar corona to the interplanetary medium.
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