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Extremely Large EUV Late Phase of Solar Flares
Time：May4, 2014，Sunday, 16: 00-17:00
Normal07.8 磅02falsefalsefalseEN-USZH-CNX-NONE EUV late phase (Woods et al. 2011) is a new observation feature during solar flare made by EUV Variability Experiment (EVE) onboard of Solar Dynamic Observatory (SDO). The main characteristic of EUV late phase is a second peak after the flare's main phase peak (tens of minutes to few hours) in the irradiance profile of 'warm' Fe XIV line (335Å, ~2.5 MK). The late phase peak is often lower than the main phase peak, and has been proved to be originated from a long cooling process of the big loop arcade inside the same active region as the flare's main region (Liu et al. 2013). However, there are some flares have a late phase peak even larger than the main flare's. What is the physical nature of this kind of late phase events? In this presentation, we will give a detailed case study.
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Name: Liu Kai
Address: School of Earth and Space Sciences
Universityof Science and Technology of China
96 Jinzhai Road
Hefei, Anhui 230026, China
Phone: +86-551-63607045 (Office)
Fax: +86-551-63607615
Email: kailiu@ustc.edu.cn
Current status:
Post-Doctor July 2013- Present
Schoolof Earthand Space Science
Universityof Science and Technology of China
Hefei, 230026, P.R.China
Education
PhD in Earth Science June 2013
Schoolof Earthand Space Science
Universityof Science and Technology of China
Hefei, 230026, P.R.China
MA.Sc in Earth Science June 2009
Schoolof Earthand Space Science
Universityof Science and Technology of China
Hefei, 230026, P.R.China
BS in Earth Science July 2005
Schoolof Earthand Space Science
Universityof Science and Technology of China
Hefei, 230026, P.R.China
Memberships,Committees, and Societies:
Member, American Geophysical Union (AGU), 2010-2014
Refereed Publications:
1)KaiLiu, Jie Zhang, Yuming Wang, and Xin Cheng, On the Origin of the Extreme-UltraViolet Late Phase of Solar Flares,Astrophys. J., V768, I2,P150– 162, 2013
2)Kai Liu, Yuming Wang, Chenglong Shen, and Shui Wang, Critical Height for the Destabilization of Solar Prominences: Statistical Results from STEREO Observations,Astrophys. J., V744, I2, P168 – 177, 2012
3)Kai Liu,LiDong Xia, Yao Chen, and HongQiang Song, Statistical study on the relationship between halo CME and coronal dimming,Science China Technological Sciences, V53, I7, pp 2020-2024, 2010
Normal07.8 磅02falsefalsefalseEN-USZH-CNX-NONEMicrosoftInternetExplorer44) Jiajia Liu, Yuming Wang, Rui Liu, Quanhao Zhang,Kai Liu, Chenglong Shen, and S. Wang, When and how does a prominence-like jet gain kinetic energy?,Astrophys. J., V782, I2, P94 – 100, 20145) Aschwanden, Markus J., Zhang, Jie, andLiu Kai, Multi-wavelength Observations of the Spatio-temporal Evolution of Solar Flares with AIA/SDO. I. Universal Scaling Laws of Space and Time Parameters,Astrophys. J., V775, I1, P23 – 44, 2013
6) H. Q. Song, Y. Chen,K. Liu, S. W. Feng, and L. D. Xia, Quasi-Periodic Releases of Streamer Blobs and Velocity Variability of the Slow Solar Wind near the Sun,Solar Physics, V258, I1, pp 129-140, 2009.
