Yingna Su

Large-amplitude Longitudinal Oscillations Triggered by the Merging of Two Solar Filaments: Observations and Magnetic Field Analysis

We follow the eruption of two related intermediate filaments observed in H

Structure and Topology of Magnetic Fields in Solar Prominences

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High-resolution Observations of Sympathetic Filament Eruptions by NVST

(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 H

Column Density Measurements of a Prominence Observed by AIA

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High-resolution He i 10830 Å Narrowband Imaging for an M-class Flare. II. Multiple Hot Channels: Their Origin and Destination

the period decreases with time and exhibits strong damping. The analysis of 171~AA 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 H

A Kinematic Study of Eruptive Prominences

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Magnetic Nonpotentiality Accumulation Prior to a

. The velocity is the largest ever detected in a prominence oscillation, approximately 100

Observations Of Filament Channels By Hinode/XRT And STEREO/EUVI

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Observations and NLFFF Modeling of Active Region 10953

. 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

Observations and analysis of the April 9, 2008 CME using STEREO, Hinode TRACE and SoHO data

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