1. 14.12.20151ISSI, Beijing, China

2. The famous example of the decaying kink oscillations of coronal loops observed with the TRACE 14.12.2015ISSI, Beijing, China2 Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Schrijver et al., (SolPhys, 1999) 14 July 1998

3. 14.12.2015ISSI, Beijing, China3 The object of the study Decaying kink oscillations of coronal loops Nakariakov et al. (A&A, 2009)

4. 14.12.2015ISSI, Beijing, China4 The object of the study Decaying kink oscillations of coronal loops “Decay-less” oscillations of coronal loops Nakariakov et al. (A&A, 2009) Nistico et al. (A&A, 2013) Time [min]

5. 14.12.2015ISSI, Beijing, China5 The object of the study Decaying kink oscillations of coronal loops “Decay-less” oscillations of coronal loops Nakariakov et al. (A&A, 2009) Nistico et al. (A&A, 2013) Time [min]

6. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) 14.12.2015ISSI, Beijing, China6

7. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) 14.12.2015ISSI, Beijing, China7

8. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) EUV waves Zheng et al. (MNRAS, 2013) 14.12.2015ISSI, Beijing, China8

9. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) EUV waves Zheng et al. (MNRAS, 2013) Vortex shedding in plasma upflows Nakariakov et al. (A&A, 2009); Gruszecki et al. (PRL, 2010) 14.12.2015ISSI, Beijing, China9

10. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) EUV waves Zheng et al. (MNRAS, 2013) Vortex shedding in plasma upflows Nakariakov et al. (A&A, 2009); Gruszecki et al. (PRL, 2010) Flux-rope & filament eruptions (full/partial/failed) Mrozek (SolPhys, 2011) 14.12.2015ISSI, Beijing, China10

11. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) EUV waves Zheng et al. (MNRAS, 2013) Vortex shedding in plasma upflows Nakariakov et al. (A&A, 2009); Gruszecki et al. (PRL, 2010) Flux-rope & filament eruptions (full/partial/failed) Mrozek (SolPhys, 2011) Magnetic reconfiguration (reconnection) in vicinity of singular magnetic points Schrijver & Brown (ApJL, 2000); White et al. (A&A, 2012; ApJ, 2013) 14.12.2015ISSI, Beijing, China11

12. Possible excitation mechanisms of the decaying kink oscillations of coronal loops discussed in literature Blast shock (or not shocked) wave produced by flare Aschwanden et al. (ApJ, 1999); Nakariakov et al. (Sci, 1999); Ofman (ApJ, 2007) Piston shock wave produced by CMEs Hudson & Warmuth (ApJL, 2004) EUV waves Zheng et al. (MNRAS, 2013) Vortex shedding in plasma upflows Nakariakov et al. (A&A, 2009); Gruszecki et al. (PRL, 2010) Flux-rope & filament eruptions (full/partial/failed) Mrozek (SolPhys, 2011) Magnetic reconfiguration (reconnection) in vicinity of singular magnetic points Schrijver & Brown (ApJL, 2000); White et al. (A&A, 2012; ApJ, 2013) Removal of magnetic energy from the corona / loop contraction Russell et al. (A&A, 2015) 14.12.2015ISSI, Beijing, China12

13. To try to find the main physical mechanism(s) of excitation of decaying kink oscillations of coronal loops on the base of the SDO/AIA (statistical) data analysis 14.12.2015ISSI, Beijing, China13 Major goal of the work

14. Continuity of observations (95% of total time) Stable, quite high cadence (≈12 s; up to  2 s in the special mode) 7 EUV channels covering broad temperature range (6×10 4 - 2×10 7 К) High angular resolution (≈1.5”; ≈0.6”/pixel) Broad field-of-view (≈1.5Rs) Good stabilization system (≈0.2”) Abundant data base since May 2010 14.12.2015ISSI, Beijing, China14 Advantages of the SDO/AIA (Lemen et al., SolPhys, 2012) This all together allows to obtain a lot of new interesting & useful information in addition to the previous solar EUV imagers such as TRACE, SOHO/EIT, CORONAS-F/TESIS, etc.

15. 14.12.2015ISSI, Beijing, China15 Selection of events for analysis Resources for events selection 1.Heliophysics Events Knowledgebase (HEK) 2.Published papers: White & Verwichte (A&A, 2012) Verwichte et al. (ApJ, 2013) White et al. (ApJ, 2013) Nistico et al. (A&A, 2013) Selected events for analysis Considered time interval May 2010 – May 2014 Type of selected events Oscillations Total number of selected events 96 Number of obvious decaying kink oscillation events 58 Number of analyzed loops 169 http://www.lmsal.com/hek/

16. 14.12.2015ISSI, Beijing, China16 Jhelioviewer - the main tool for our analysis Mueller et al. (CSE, 2009); http://www.jhelioviewer.org/

17. Solar flares NGDC/NOAA solar flare catalog Solar Monitor Original time profiles of soft X-ray emission detected by the GOES/XRS 14.12.2015ISSI, Beijing, China17 Additional information Coronal type II radio bursts Published catalogues (NGDC/NOAA, SWS (IPS), Monstein’s list, …) Original radio spectrograms (e-Callisto, RSTN, HiRAS, …) CMEs SOHO/LASCO CME Catalog CACTUS CME Catalog (SOHO/LASCO + STEREO/COR2)

18. 14.12.2015ISSI, Beijing, China18 Created catalog of loop oscillation events

19. 14.12.2015ISSI, Beijing, China19 Statistics Loop Oscillation Events N=58 CMEs (white light) N=44 (76%) Flares (SXR) N=53 (91%) + 5 behind limb LCE (EUV) N=57 (98%) Type II radio bursts N=23 (40%) * LCE – low coronal eruptions/ejections (detected by the SDO/AIA in the EUV range)

20. 14.12.2015ISSI, Beijing, China20 Statistics Loop Oscillation Events N=58 CMEs (white light) N=44 (76%) Flares (SXR) N=53 (91%) + 5 behind limb LCE (EUV) N=57 (98%) Type II radio bursts N=23 (40%) * LCE – low coronal eruptions/ejections (detected by the SDO/AIA in the EUV range) Shock waves

21. 14.12.2015ISSI, Beijing, China21 Distributions of speeds of hypothetical driver of oscillations

22. 14.12.2015ISSI, Beijing, China22 Associated product of the study Chicken/egg – flare/CME (?) Distribution of delays between CME start & flare start =1-2 мин Start almost simultaneously

23. 14.12.2015ISSI, Beijing, China23 The major observational finding of the study: in 50 out of 58 events (86%) LCEs push loops from their equilibrium and cause their oscillations SDO/AIA 211 A SDO/AIA 171 We called these events as Type-1 events

24. 14.12.2015ISSI, Beijing, China24 Cartoon of the most common situation Type-1 event Before LCE During LCE After LCE

25. 14.12.2015ISSI, Beijing, China25 Type-2 event: LCE is also present, but its role is not obvious 6 out of 58 events (10%) SDO/AIA 211 A SDO/AIA 171

26. It is found that in 56 out of 58 events (96%) the excitation mechanisms of decaying kink oscillations of coronal loops are related to the Lower Coronal Eruptions / Ejections (LCEs). In the majority of cases (86%) LCEs pushed loops from their equilibrium and caused their decay oscillations after LCEs went away from region of interaction. In rare cases (4%) other mechanisms are not excluded. The observational data did not allow to determine excitation mechanism unambiguously. It is also found that all LCEs are accompanied by increase of SXR emission, i.e. by flares. 1-2 mins delay between LCE and flare onsets is found statistically that is comparable to the error. It is not possible to give unambiguous general answer, whether LCEs drive flare or flares drive LCEs. 14.12.2015ISSI, Beijing, China26 Conclusions

27. Thank you! 14.12.2015ISSI, Beijing, China27 Mueller et al. (arXiv e-print, 2009); http://jhelioviewer.org