Quantitative prediction of type II solar radio emission from the Sun to 1 AU

• Published in: Geophysical research letters 2016-01, Vol.43 (1), p.50-57
• Main Authors: Schmidt, J. M., Cairns, Iver H.
• Format: Article
• Language: English
• Subjects: Boundary conditions; Bursts; Computational fluid dynamics; Computer simulation; Coronal mass ejection; Data; Dimensional analysis; Emission analysis; Emissions; Gamma rays; Magnetohydrodynamic simulation; Mass; Modulation; Photovoltaic cells; Physics; Plasma physics; Radio; Radio bursts; Radio emission; Simulation; Solar flares; Solar physics; Solar radio bursts; Solar radio emission; solar‐terrestrial relations; Space weather; Spacecraft; Sun; Sun: coronal mass ejections (CMEs); Sun: radio radiation; Three dimensional
• ISSN: 0094-8276; 1944-8007
• DOI: 10.1002/2015GL067271

Coronal mass ejections (CMEs) are frequently associated with shocks and type II solar radio bursts. Despite involving fundamental plasma physics and being the archetype for collective radio emission from shocks, type II bursts have resisted detailed explanation for over 60 years. Between 29 November and 1 December 2013 the two widely separated spacecraft STEREO A and B observed a long lasting, intermittent, type II radio burst from ≈4 MHz to 30 kHz (harmonic), including an intensification when the CME‐driven shock reached STEREO A. We demonstrate the first accurate and quantitative simulation of a type II burst from the high corona (near 11 solar radii) to 1 AU for this event with a combination of a data‐driven three‐dimensional magnetohydrodynamic simulation for the CME and plasma background and an analytic quantitative kinetic model for the radio emission. Key Points Interplanetary type II radio bursts are modulated by structures in the solar wind This modulation is different in the solar corona and the interplanetary space Event‐specific type II bursts simulations can also yield boundary conditions for space weather