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Large-Amplitude Longitudinal Oscillations Triggered by the Merging of Two Solar Filaments: Observations and Magnetic Field Analysis View all abstracts by submitter

Manuel Luna   Submitted: 2017-11-06 03:48

We follow the eruption of two related intermediate filaments observed in Hα (from GONG) and in EUV (from SDO/AIA) and the resulting large-amplitude longitudinal oscillations of the plasma in the filament channels. The events occurred in and around the decayed active region AR12486 on 2016 January 26. Our detailed study of the oscillation reveals that the periods of the oscillations are about one hour. In Hα the period decreases with time and exhibits strong damping. The analysis of 171A images shows that the oscillation has two phases, an initial long period phase and a subsequent oscillation with a shorter period. In this wavelength the damping appears weaker than in Hα. The velocity is the largest ever detected in a prominence oscillation, approximately 100 km s-1. Using SDO/HMI magnetograms we reconstruct the magnetic field of the filaments modeled as flux ropes by using a flux-rope insertion method. Applying seismological techniques we determine that the radii of curvature of the field lines in which cool plasma is condensed are in the range 75-120 Mm, in agreement with the reconstructed field. In addition, we infer a field strength of ≥7 to 30 Gauss, depending on the electron density assumed; that is also in agreement with the values from the reconstruction (8-20 Gauss). The poloidal flux is zero and the axis flux is of the order of 1020 to 1021 Mx, confirming the high shear existing even in a non-active filament.

Authors: M. Luna, Y. Su, B. Schmieder, R. Chandra, T. A. Kucera
Projects: None

Publication Status: Accepted for publication in ApJ
Last Modified: 2017-11-06 11:34
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