Abstract
Large-scale Globally Propagating Coronal Waves
Highlights
The solar corona consists of a magnetized plasma, with typical temperatures of 1 – 2 MK
The first spectroscopic observation of an Extreme Ultraviolet (EUV) wave was made by Harra and Sterling (2003) who reported on an EUV wave seen with Transition Region and Coronal Explorer (TRACE) that passed through the field of view of SOHO/CDS
Thompson and Myers, 2009) and within one wave event (Wills-Davey and Thompson, 1999), ii) the fact that a significant fraction of these speeds is below the coronal sound speed (i.e., < 185 km s–1 for a coronal temperature of 1.5 MK), and iii) the observation that Extreme Ultraviolet Imaging Telescope (EIT) waves retain their coherence over large distances
Summary
The solar corona consists of a magnetized plasma, with typical temperatures of 1 – 2 MK. These postulated coronal disturbances were observed in 1997 with the Extreme Ultraviolet Imaging Telescope (EIT; Delaboudiniere et al, 1995) aboard the SOHO spacecraft They take the form of spectacular wave-like features propagating globally through the corona (Moses et al, 1997; Thompson et al, 1998). These perturbations have become known under a bewildering multitude of names, including “EIT waves” and the more generic coronal waves (for a discussion of terminology, see Section 1.3). The recently discovered phenomena of small-scale EUV waves (Innes et al, 2009; Podladchikova et al, 2010) and quasi-periodic fast propagating wave trains (Liu et al, 2010, 2011) are beyond the scope of this review, and the reader is referred to Liu and Ofman (2014) for a discussion
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