We investigate the solar Type III radio bursts recorded at about 10 AU by Cassini spacecraft. More than 300 bursts have been recorded by the RPWS experiment in the time interval from 01 Jan. 2008 to 31 Dec. 2014. We show that the solar Type III occurrence is mainly depending on the solar activity and also exhibits maxima and minima of detection. The source location of such solar bursts is the interplanetary medium because the dominant emission appears at frequency lower than 2.3 MHz.

Raw output of spacecraft magnetometers has to be converted into meaningful units and coordinate systems before it is usable for scientific applications. This conversion is defined by 12 calibration parameters, 8 of which are more easily determined in flight if the spacecraft is spinning. We present theory and advanced algorithms to determine these eight parameters. They take into account the physical magnetometer and spacecraft behavior, making them superior to previously published algorithms.

This paper describes frequency and timing calibration, modeling and data processing and calibration for MMS magnetometers, resulting in a merged search choil and fluxgate data product.

The solar wind magnetic field drapes around the active nucleus of comet 67P/CG, creating a magnetosphere. The solar wind density increases and with that the pressure, which compresses the magnetosphere, increasing the magnetic field strength near Rosetta. The higher solar wind density also creates more ionization through collisions with the gas from the comet. The new ions are picked-up by the magnetic field and generate mirror-mode waves, creating low-field high-density "bottles" near 67P/CG.