SDO/AIA OBSERVATIONS OF SECONDARY WAVES GENERATED BY INTERACTION OF THE 2011 JUNE 7 GLOBAL EUV WAVE WITH SOLAR CORONAL STRUCTURES
- Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)
We present Solar Dynamics Observatory/Atmospheric Imaging Assembly observations of the interaction of a global EUV wave on 2011 June 7 with active regions (ARs), coronal holes (CHs), and coronal bright structures. The primary global wave has a three-dimensional dome shape, with propagation speeds ranging from 430 to 780 km s{sup -1} in different directions. The primary coronal wave runs in front of the expanding loops involved in the coronal mass ejection (CME) and its propagation speeds are approximately constant within 10-20 minutes. Upon arrival at an AR on its path, the primary EUV wave apparently disappears and a secondary wave rapidly reemerges within 75 Mm of the AR boundary at a similar speed. When the EUV wave encounters a coronal bright structure, an additional wave front appears there and propagates in front of it at a velocity nearly a factor of two faster. Reflected waves from a polar CH and a coronal bright structure are observed and propagate fractionally slower than the primary waves. Some of these phenomena can be equally explained by either a wave or a non-wave model alone. However, taken together, these observations provide new evidence for the multitudes of global EUV waves, in which a true MHD fast-mode wave or shock propagates in front of an expanding CME bubble.
- OSTI ID:
- 22011851
- Journal Information:
- Astrophysical Journal, Vol. 746, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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