Bibliographic Metadata

Quasi-oscillatory dynamics observed in ascending phase of the flare on March 6, 2012
AuthorZaqarashvili, Teimuraz
Published in
Astronomy & Astrophysics, 2017, Vol. 600, A67-1-A67-12
Document typeJournal Article
Keywords (EN)Sun: atmosphere / Sun: flares / methods: data analysis / waves / instabilities
URNurn:nbn:at:at-ubg:3-5325 Persistent Identifier (URN)
 The work is publicly available
Quasi-oscillatory dynamics observed in ascending phase of the flare on March 6, 2012 [2.25 mb]
Abstract (English)

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.

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