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Prominence Activation by Coronal Fast Mode Shock View all abstracts by submitter

Takuya Takahashi   Submitted: 2015-01-07 23:46

An X5.4 class flare occurred in active region (AR) NOAA11429 on 2012 March 7. The flare was associated with very fast coronal mass ejection (CME) with its velocity of over 2500 km s-1. In the images taken with STEREO-B/COR1, a dome-like disturbance was seen to detach from expanding CME bubble and propagated further. A Type-II radio burst was also observed at the same time. On the other hand, in EUV images obtained by SDO/AIA, expanding dome-like structure and its foot print propagating to the north were observed. The foot print propagated with its average speed of about 670 km s-1 and hit a prominence located at the north pole and activated it. While the activation, the prominence was strongly brightened. On the basis of some observational evidence, we concluded that the foot print in AIA images and the ones in COR1 images are the same, that is MHD fast mode shock front. With the help of a linear theory, the fast mode mach number of the coronal shock is estimated to be between 1.11 and 1.29 using the initial velocity of the activated prominence. Also, the plasma compression ratio of the shock is enhanced to be between 1.18 and 2.11 in the prominence material, which we consider to be the reason of the strong brightening of the activated prominence. The applicability of linear theory to the shock problem is tested with nonlinear MHD simulation.

Authors: Takuya Takahashi, Ayumi Asai, Kazunari Shibata
Projects: SDO-AIA

Publication Status: accepted
Last Modified: 2015-01-09 12:49
Go to main E-Print page  The energetics of a global shock wave in the low solar corona  New analytical and numerical models of solar coronal loop: I. Application to forced vertical kink oscillations  Edit Entry  Download Preprint  Delete Entry 

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