Volume 600, April 2017
|Number of page(s)||12|
|Published online||31 March 2017|
Quasi-oscillatory dynamics observed in ascending phase of the flare on March 6, 2012
1 Centre for Mathematical Plasma Astrophysics, Celestijnenlaan 200B, 3001 Leuven, Belgium
2 Abastumani Astrophysical Observatory at Ilia State University, Kakutsa Cholokashvili Ave 3/5, 0162 Tbilisi, Georgia
3 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
4 Institute of Physics, IGAM, University of Graz, Universitätsplatz 5, 8010 Graz, Austria
5 Combinatorial Optomization and Decision Support, KU Leuven campus Kortrijk, E. Sabbelaan 53, 8500 Kortrijk, Belgium
6 Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics (MSU SINP) Leninskie Gory, 119992 Moscow, Russia
Received: 6 August 2016
Accepted: 8 December 2016
Context. The dynamics of the flaring loops in active region (AR) 11429 are studied. The observed dynamics consist of several evolution stages of the flaring loop system during both the ascending and descending phases of the registered M-class flare. The dynamical properties can also be classified by different types of magnetic reconnection, related plasma ejection and aperiodic flows, quasi-periodic oscillatory motions, and rapid temperature and density changes, among others. The focus of the present paper is on a specific time interval during the ascending (pre-flare) phase.
Aims. The goal is to understand the quasi-periodic behavior in both space and time of the magnetic loop structures during the considered time interval.
Methods. We have studied the characteristic location, motion, and periodicity properties of the flaring loops by examining space-time diagrams and intensity variation analysis along the coronal magnetic loops using AIA intensity and HMI magnetogram images (from the Solar Dynamics Observatory).
Results. We detected bright plasma blobs along the coronal loop during the ascending phase of the solar flare, the intensity variations of which clearly show quasi-periodic behavior. We also determined the periods of these oscillations.
Conclusions. Two different interpretations are presented for the observed dynamics. Firstly, the oscillations are interpreted as the manifestation of non-fundamental harmonics of longitudinal standing acoustic oscillations driven by the thermodynamically non-equilibrium background (with time variable density and temperature). The second possible interpretation we provide is that the observed bright blobs could be a signature of a strongly twisted coronal loop that is kink unstable.
Key words: Sun: atmosphere / Sun: flares / methods: data analysis / waves / instabilities
© ESO, 2017
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