CME Expansion as the Driver of Metric Type II Shock Emission as Revealed by Self-consistent Analysis of High-Cadence EUV Images and Radio Spectrograms

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• 作者：A. Kouloumvakos (1) (2)
  S. Patsourakos (2)
  A. Hillaris (1)
  A. Vourlidas (3)
  P. Preka-Papadema (1)
  X. Moussas (1)
  C. Caroubalos (4)
  P. Tsitsipis (5)
  A. Kontogeorgos (5)
  
• 关键词：Coronal mass ejections ; low coronal signatures ; Corona ; radio emission ; Radio bursts ; meter ; wavelengths and longer (m ; dkm ; hm ; km) ; Radio bursts ; type II
• 刊名：Solar Physics
• 出版年：2014
• 出版时间：June 2014
• 年：2014
• 卷：289
• 期：6
• 页码：2123-2139
• 全文大小：1,422 KB
• 作者单位：A. Kouloumvakos (1) (2)
  S. Patsourakos (2)
  A. Hillaris (1)
  A. Vourlidas (3)
  P. Preka-Papadema (1)
  X. Moussas (1)
  C. Caroubalos (4)
  P. Tsitsipis (5)
  A. Kontogeorgos (5)
  
  1. Section of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens, Zografos (Athens), 15783, Greece
  2. Department of Physics, Section of Astrogeophysics, University of Ioannina, Ioannina, Greece
  3. Space Science Division, Naval Research Laboratory, Washington, DC, USA
  4. Department of Informatics, University of Athens, Zografos (Athens), 15783, Greece
  5. Department of Electronics, Technological Educational Institute of Lamia, Lamia, 35100, Greece
  
• ISSN：1573-093X

文摘

On 13 June 2010, an eruptive event occurred near the solar limb. It included a small filament eruption and the onset of a relatively narrow coronal mass ejection (CME) surrounded by an extreme ultraviolet (EUV) wave front recorded by the Solar Dynamics Observatory’s (SDO) Atmospheric Imaging Assembly (AIA) at high cadence. The ejection was accompanied by a GOES M1.0 soft X-ray flare and a Type-II radio burst; high-resolution dynamic spectra of the latter were obtained by the Appareil de Routine pour le Traitement et l’Enregistrement Magnetique de l’Information Spectral (ARTEMIS IV) radio spectrograph. The combined observations enabled a study of the evolution of the ejecta and the EUV wave front and its relationship with the coronal shock manifesting itself as metric Type-II burst. By introducing a novel technique, which deduces a proxy of the EUV compression ratio from AIA imaging data and compares it with the compression ratio deduced from the band-split of the Type-II metric radio burst, we are able to infer the potential source locations of the radio emission of the shock on that AIA images. Our results indicate that the expansion of the CME ejecta is the source for both EUV and radio shock emissions. Early in the CME expansion phase, the Type-II burst seems to originate in the sheath region between the EUV bubble and the EUV shock front in both radial and lateral directions. This suggests that both the nose and the flanks of the expanding bubble could have driven the shock.