| Authors : | Ramesh Chandra1, P. F. Chen2, P. Devi1, R. Joshi1, B. Schmieder3, Y. J. Moon4, W. Uddin5
1 Department of Physics, DSB Campus, Kumaun University, Nainital – 263 001, India
2 School of Astronomy & Space Science, Nanjing University, Nanjing 210023, China
3 Observatoire de Paris, LESIA, UMR8109 (CNRS), F-92195 Meudon Principal Cedex, France
4 School of Space Research, Kyung Hee University, Yongin, Gyeonggi-Do, 446-701, Korea
5Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital 263 001, India
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| Abstract : | Here, we perform an analysis of an extreme ultraviolet (EUV) wave event on 2010 February 11. The event was observed by the STEREO–B and Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) in various EUV channels. The event was associated with partial prominence eruption. The EUV wave event contains a faster wave with a speed of ∼445 km s −1 , which we name coronal Moreton wave, and a slower wave with a speed of ∼298 km s−1 , which we call “EIT wave”. The coronal Moreton wave is identified as a fast-mode wave and the “EIT wave” is identified as an apparent propagation due to successive field-line stretching. In addition to above, we also observe a stationary front associated with the fast mode EUV wave. This stationary front is explained as mode conversion from the coronal Moreton wave to a slow-mode wave. |
