Objectives:
1: To study the spectroscopic characters of magnetic flux rope, especially prior to its eruption.
2: To find the location of heating of the flux rope.
Magnetic flux ropes are twisted magnetic field line structures. It has been widely accepted that the flux rope is the critical structure of coronal mass ejections (CMEs) that are most energetic events in the solar system and cause severe space weather. Zhang et al. (2012) and Cheng et al. (2013) found that the flux rope shows an elongated EUV channel structure in the AIA high temperature passbands (e.g., 131 A and 94 A). However, where and how the flux rope is heated are unknown. In addition, what is the signature of flux rope in the lower solar atmosphere? And how is the flux rope activated and erupted? These questions are not fully resolved. The high-resolution observations from the three instruments on board Hinode cover the photosphere, chromosphere, and corona, and will shed light on the formation, heating, and initiation of the magnetic flux rope. |
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