Decayless low-amplitude kink oscillations: a common phenomenon in the solar corona?⋆
1 Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick, Coventry CV4 7AL, UK
2 Institute of Solar-Terrestrial Physics, Lermontov st., 126a, 664033 Irkutsk, Russia
3 School of Space Research, Kyung Hee University, Yongin, 446-701 Gyeonggi, Korea
4 Central Astronomical Observatory at Pulkovo of the Russian Academy of Sciences, 196140 St. Petersburg, Russia
Received: 27 March 2015
Accepted: 18 August 2015
Context. We investigate the decayless regime of coronal kink oscillations recently discovered in the Solar Dynamics Observatory (SDO)/AIA data. In contrast to decaying kink oscillations that are excited by impulsive dynamical processes, this type of transverse oscillations is not connected to any external impulsive impact, such as a flare or coronal mass ejection, and does not show any significant decay. Moreover the amplitude of these decayless oscillations is typically lower than that of decaying oscillations.
Aims. The aim of this research is to estimate the prevalence of this phenomenon and its characteristic signatures.
Methods. We analysed 21 active regions (NOAA 11637–11657) observed in January 2013 in the 171 Å channel of SDO/AIA. For each active region we inspected six hours of observations, constructing time-distance plots for the slits positioned across pronounced bright loops. The oscillatory patterns in time-distance plots were visually identified and the oscillation periods and amplitudes were measured. We also estimated the length of each oscillating loop.
Results. Low-amplitude decayless kink oscillations are found to be present in the majority of the analysed active regions. The oscillation periods lie in the range from 1.5 to 10 min. In two active regions with insufficient observation conditions we did not identify any oscillation patterns. The oscillation periods are found to increase with the length of the oscillating loop.
Conclusions. The considered type of coronal oscillations is a common phenomenon in the corona. The established dependence of the oscillation period on the loop length is consistent with their interpretation in terms of standing kink waves.
Key words: Sun: corona - Sun: oscillations - methods: observational
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2015