We aim to understand how magnetic loops evolve to produce small-scale reconnection events and their dynamics at different temperatures (i.e, from chromosphere to corona).
Small-scale activities of magnetic loops observed in the lower solar atmosphere, including Ellerman bombs, IRIS bombs and explosive events, are crucial as they might describe how magnetic energy is released in the lower solar atmosphere and heat the plasma therein. The proposed coordinated observations aim to understand how magnetic loops evolve to produce these small-scale reconnection events and their dynamics at different temperatures (i.e, from chromosphere to corona). We plan the joint observations with BBSO/NST, IRIS and Hinode. Our proposal to NST and IRIS has been already accepted and arranged in the interval of August 26-31. The plasma beta in and above the solar chromosphere is mostly less than 1, which suggests the plasmas therein are mostly frozen-in magnetic field lines. Magnetic loops, therefore, are one of the fundamental building blocks in the solar atmosphere. Magnetic loops in the chromosphere and transition region might include the fibril and cool loops (e.g. Chae et al. 2000; Huang et al. 2015, etc.). Some fascinate phenomena have been found to be associated with evolution of these loops. A historical one is Ellerman bombs (Ellerman 1917; Fang et al. 2006) that are identified by enhanced Ha wings together with normal line centre and are believed to be signatures of magnetic reconnection in the photosphere (e.g., Watanabe et al. 2007; Vissers et al. 2013; Rutten et al. 2013; Tian et al. 2016; etc.). A popular one is IRIS bombs firstly identify in IRIS spectral data (Peter et al. 2014; Tian et al. 2016; etc.) occurring while magnetic loops are emerging as serpentine (Peter et al. 2014). Transition region explosive events (Brueckner et al. 1983; Dere et al. 1989; Ning et al. 2004; Huang et al. 2014), which have been suggested to be signatures of magnetic reconnection (Dere et al. 1989; Innes et al. 1997), can also be found to closely associate with interaction between magnetic loops (e.g. Huang et al. 2015, 2017). These phenomena are crucial as they might describe how magnetic energy is released in the lower solar atmosphere and heat the plasma therein. Here, we propose a coordinated observing campaign using BBSO/NST, IRIS and Hinode to obtain magnetic field, spectral and imaging data, which covering observations from the solar photosphere to corona. With these data, we aim to understand how magnetic loops evolve to produce these small-scale reconnection events and their dynamics at different temperatures (i.e, from chromosphere to corona). |
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