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Solar Physics

, 294:56 | Cite as

Kinematics and Energetics of the EUV Waves on 11 April 2013

  • Aarti FularaEmail author
  • Ramesh Chandra
  • P. F. Chen
  • Ivan Zhelyazkov
  • A. K. Srivastava
  • Wahab Uddin
Article

Abstract

In this study, we present the observations of extreme-ultraviolet (EUV) waves associated with an M6.5 flare on 2013 April 11. The event was observed by Solar Dynamics Observatory (SDO) in different EUV channels. The flare was also associated with a halo CME and type II radio bursts. We observed both fast and slow components of the EUV wave. The speed of the fast component, which is identified as a fast-mode MHD wave, varies in the range from \(600\mbox{ to }640~\mbox{km}\,\mbox{s}^{-1}\), whereas the speed of the slow-component is \({\approx}\,140~\mbox{km}\,\mbox{s}^{-1}\). We observed the unusual phenomenon that, as the fast-component EUV wave passes through two successive magnetic quasi-separatrix layers (QSLs), two stationary wave fronts are formed locally. We propose that part of the outward-propagating fast-mode EUV wave is converted into slow-mode magnetohydrodynamic waves, which are trapped in local magnetic field structures, forming successive stationary fronts. Along the other direction, the fast-component EUV wave also creates oscillations in a coronal loop lying \({\approx}\,225~\mbox{Mm}\) away from the flare site. We have computed the energy of the EUV wave to be of the order of \(10^{20}~\mbox{J}\).

Keywords

Waves, magnetohydrodynamic Waves, propagation Corona, radio emission 

Notes

Acknowledgements

We would like to thank the referee for the useful comments and suggestions that helped us to improve the manuscript. We also acknowledge the use of SDO and GONG data. PFC was supported by the Chinese grants NSFC 11533005, U1731241 and Jiangsu 333 Project (No. BRA2017359). AF and RC acknowledge the support from the ISRO/RESPOND project. The work of IZh and RC was supported by the Bulgarian Science Fund under Indo–Bulgarian bilateral project DNTS/INDIA 01/7.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.

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© Springer Nature B.V. 2019

Authors and Affiliations

  1. 1.Department of Physics, DSB CampusKumaun UniversityNainitalIndia
  2. 2.School of Astronomy & Space ScienceNanjing UniversityNanjingChina
  3. 3.Key Laboratory of Modern Astronomy & Astrophysics (Nanjing University)Ministry of EducationNanjingChina
  4. 4.Faculty of PhysicsSofia UniversitySofiaBulgaria
  5. 5.Department of PhysicsIndian Institute of Technology (BHU)VaranasiIndia
  6. 6.Aryabhatta Research Institute of Observational SciencesNainitalIndia

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