Temporal and Spatial Association Between a Solar Flare, CME, and Radio Burst on 19 November 2013

Abstract

We present multi-wavelength and multi-instrument observations and analysis of a major X 1.0 class flare, radio burst, halo coronal mass ejection (CME), and loop eruption from the solar active region NOAA 11893 on 19 November 2013 (SOL2013-11-19T10:26). The aim of this work is twofold: The first aim to study the evolution of the loop eruption and the second is to find the link between this eruption and radio emissions. Initial signatures of eruption from the solar source region are confirmed using observations from the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory in the hot channel at 94\xa0A wavelength. These observations confirm that the source of the CME was associated with a magnetic-loop eruption, which was visible before the flare initiation. The photospheric magnetic configuration displayed a complex network of $\\upbeta \\updelta $\n sunspots. After the eruption, a\xa0CME was observed by the Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph with linear speed and acceleration of $740~\\text{km}\\,\\text{s}^{-1}$\n and $-2~\\text{m}\\,\\text{s}^{-2}$\n , respectively. Dynamic radio-spectrum observation from the Learmonth Observatory in the metric frequency range shows Type-III and Type-II radio emissions that reveal the field-line opening and coronal-shock formation closely associated with the CME. From the metric Type-II radio observation and assuming Newkirk’s density model, we estimate the shock formation height range of $1.14\\,\\text{--}\\,1.54~\\text{R}_{\\odot }$\n with the corresponding shock speed (\n $\\approx650~\\text{km}\\,\\text{s}^{-1}$\n ). With the heliographic observations from the Nancay heliograph at different frequencies we could disentangle Type-II bursts from Type-III bursts. Likely, the Type-III burst would correspond to the loop eruption while the Type-II comes from the northern flank of the CME.