STEREO-Wind Radio Positioning of an Unusually Slow Drifting Event

Abstract

On 13 March 2010 an unusually long duration event was observed by radio spectrographs onboard the STEREO-B and Wind spacecraft. The event started at about 13:00 UT and ended at approximately 06:00 UT on 14 March. The event presents itself as slow drifting, quasi-continuous emission in a very narrow frequency interval, with an apparent frequency drift from about 625 kHz to approximately 425 kHz. Using the Leblanc, Dulk, and Bougeret (1998) interplanetary density model we determined that the drift velocities of the radio source are $\approx$33km s${}^{-1}$ and $\approx$52km s${}^{-1}$ for 0.2 and 0.5 times the densities of Leblanc model, respectively with a normalization density of 7.2cm${}^{-3}$ at 1AU and assuming harmonic emission. A joint analysis of the radio direction finding data, coronograph white-light observations and modeling revealed that the radio sources appear to be localized in regions of interaction with relatively high density and slow solar wind speed.

arXiv comment12 pages, 4 figures, Accepted in Solar Physics

References in corpus (4)

• Geometric Triangulation of Imaging Observations to Track Coronal Mass Ejections Continuously Out to 1 AU
• On Sun-to-Earth Propagation of Coronal Mass Ejections
• STEREO and Wind observations of a fast ICME flank triggering a prolonged geomagnetic storm on 5-7 April 2010
• Determination of Electromagnetic Source Direction as an Eigenvalue Problem

Cited by in corpus (4)

• Sun-to-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-effectiveness
• Using radio triangulation to understand the origin of two subsequent type II radio bursts
• Multipoint study of successive coronal mass ejections driving moderate disturbances at 1 AU
• An analysis of interplanetary solar radio emissions associated with a coronal mass ejection