Partial Reflection and Trapping of a Fast-mode Wave in Solar Coronal Arcade Loops

Abstract

We report on the first direct observation of a fast-mode wave propagating along and perpendicular to cool (171 Å) arcade loops observed by the SDO/AIA. The wave was associated with an impulsive/compact flare, near the edge of a sunspot. The EUV wavefront expanded radially outward from the flare center and decelerated in the corona from 1060-760 km/s within ~3-4 minute. Part of the EUV wave propagated along a large-scale arcade of cool loops and was partially reflected back to the flare site. The phase speed of the wave was about 1450 km/s, which is interpreted as a fast-mode wave. A second overlying loop arcade, orientated perpendicular to the cool arcade, is heated and becomes visible in the AIA hot channels. These hot loops sway in time with the EUV wave, as it propagated to and fro along the lower loop arcade. We suggest that an impulsive energy release at one of the footpoints of the arcade loops causes the onset of an EUV shock wave that propagates along and perpendicular to the magnetic field.

ApJ letters (in press), 8 pages, 5 figures

References in corpus (3)

• Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review)
• First Evidence of Coexisting EIT Wave and Coronal Moreton Wave from SDO/AIA Observations
• SDO/AIA Observations of a Reflecting Longitudinal Wave in a Coronal Loop

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• Coronal Quasi-periodic Fast-mode Propagating Wave Trains
• First Unambiguous Imaging of Large-Scale Quasi-Periodic Extreme-Ultraviolet Wave or Shock
• Total reflection of a flare-driven quasi-periodic EUV wave train at a coronal hole boundary
• Cross-loop propagation of a quasi-periodic extreme-ultraviolet wave train triggered by successive stretching of magnetic field structures during a solar eruption
• Quantifying the Magnetic Structure of a Coronal Shock Producing a Type II Radio Burst