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Imaging and Spectral Observations of a Type-II Radio Burst Revealing the Section of the CME-Driven Shock That Accelerates Electrons

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Abstract

We report on a multi-wavelength analysis of the 26 January 2014 solar eruption involving a coronal mass ejection (CME) and a Type-II radio burst, performed by combining data from various space and ground-based instruments. An increasing standoff distance with height shows the presence of a strong shock, which further manifests itself in the continuation of the metric Type-II burst into the decameter–hectometric (DH) domain. A plot of speed versus position angle (PA) shows different points on the CME leading edge traveled with different speeds. From the starting frequency of the Type-II burst and white-light data, we find that the shock signature producing the Type-II burst might be coming from the flanks of the CME. Measuring the speeds of the CME flanks, we find the southern flank to be at a higher speed than the northern flank; further the radio contours from Type-II imaging data showed that the burst source was coming from the southern flank of the CME. From the standoff distance at the CME nose, we find that the local Alfv́en speed is close to the white-light shock speed, thus causing the Mach number to be small there. Also, the presence of a streamer near the southern flank appears to have provided additional favorable conditions for the generation of shock-associated radio emission. These results provide conclusive evidence that the Type-II emission could originate from the flanks of the CME, which in our study is from the southern flank of the CME.

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Acknowledgments

We thank the anonymous reviewer for valuable comments that have improved the manuscript. This work was done during the hands-on data sessions of the COSPAR Capacity Building Workshop on Coronal and Interplanetary Shocks: Analysis of Data from Space and Ground Based Instruments held at the Kodaikanal Solar Observatory, Tamil Nadu, India during 6 – 17 January 2020. The authors thank the organizers of the workshop for providing the opportunity to learn and work with experts in the field. We also extend our gratitude to Christian Monstein, Seiji Yashiro, and Indrajit V. Barve for developing the Python codes, which helped us during the data analysis part of the workshop. We also take this opportunity to thank the local organizers who took care of the local logistics, which enabled a smooth running of the workshop. We would like to express our gratitude to the Gauribidanur Radio Observatory staff for providing the radio heliograph data. The SOHO/LASCO data used here are produced by a consortium of the Naval Research Laboratory (USA), Max-Planck-Institut für Aeronomie (Germany), Laboratoire d’Astronomie (France), and the University of Birmingham (UK). SOHO is a project of international cooperation between ESA and NASA. The SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liège (Belgium), Institut d’Optique Théorique et Appliquée (France), Institut d’Astrophysique Spatiale (France). We also acknowledge the SDO team for making the AIA data available. SDO is a mission for NASA’s Living With a Star (LWS) program. S. Majumdar acknowledges Dipankar Banerjee for his constant support and motivation to participate in this workshop. A. Kumari acknowledges the ERC under the European Union’s Horizon 2020 Research and Innovation Programme Project SolMAG 724391. N. Gopalswamy was supported by NASA’s Living With a Star program.

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Majumdar, S., Tadepalli, S.P., Maity, S.S. et al. Imaging and Spectral Observations of a Type-II Radio Burst Revealing the Section of the CME-Driven Shock That Accelerates Electrons. Sol Phys 296, 62 (2021). https://doi.org/10.1007/s11207-021-01810-8

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