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Abstract
Evidence of flare-induced, large-amplitude, decay-less transverse oscillations is presented. A system of multithermal coronal loops, as observed with the Atmospheric Imaging Assembly (AIA), exhibit decay-less transverse oscillations after a flare erupts nearby one of the loop footpoints. Measured oscillation periods lie between 4.2 min and 6.9 min wherein the displacement amplitudes range from 0.17 Mm to 1.16 Mm. A motion-magnification technique has been employed to detect the preflare decay-less oscillations. These oscillations have similar periods (between 3.7 min and 5.0 min) similar to the previous ones, but their amplitudes (0.04 Mm to 0.12 Mm) are found to be significantly smaller. No phase difference is found among oscillating threads of a loop when observed through a particular AIA channel or when their multichannel signatures are compared. These features suggest that the occurrence of a flare in this case neither changed the nature of these oscillations (decaying versus decay-less), nor the oscillation periods. The only effect the flare has is to increase the oscillation amplitudes.
Highlights
The solar corona, a highly structured million Kelvin hot and dynamic upper atmosphere of the Sun, accommodates a wide variety of magnetic structures including coronal loops.These loops act as wave guides for a range of magnetohydrodynamical (MHD) waves that are observed in the corona (Nakariakov & Verwichte 2005)
In this Letter, we present a unique event where several multithermal coronal loops exhibit decay-less transverse oscillations that are triggered by a nearby flare
In this Letter, we study the properties of decay-less transverse oscillations that are triggered by a nearby flaring event
Summary
The solar corona, a highly structured million Kelvin hot and dynamic upper atmosphere of the Sun, accommodates a wide variety of magnetic structures including coronal loops. These are small amplitude (≤0.5 Mm), transverse oscillations with periods between and 7 min and they show no apparent decay in their amplitudes over a large number of wave periods These waves are rather omnipresent in active region coronal loops and seem to have no apparent connection with any transient events such as a flare (Anfinogentov et al 2015). This is different from the traditionally observed, rapidly decaying kink waves which are always associated with an impulsive driver. Two vertical dotted lines in every panel mark the onset time of the two flares
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