Large-amplitude Oscillations of a Quiescent Filament Excited by an Extreme-ultravioletWave

TL;DR

This study observes large-amplitude longitudinal and transverse oscillations in a quiescent solar filament triggered by an EUV wave, providing insights into magnetic field properties and filament dynamics.

Contribution

It presents detailed multiwavelength observations of filament oscillations induced by an EUV wave, estimating magnetic field strengths and curvature radii using the pendulum model.

Findings

Longitudinal oscillations lasted nearly two cycles with an amplitude of ~4.7 Mm.

Transverse oscillations lasted 2-3 cycles with an amplitude of ~1.8 Mm.

Magnetic field strengths in the filament dips were estimated to be 4.6-5.6 G (longitudinal) and 6.6-7.4 G (transverse).

Abstract

In this paper, we carry out multiwavelength observations of simultaneous longitudinal and transverse oscillations of a quiescent filament excited by an extreme-ultraviolet (EUV) wave on 2023 February 17. A hot channel eruption generates an X2.3 class flare and a fast coronal mass ejection (CME) in active region (AR) NOAA 13229 close to the eastern limb. The CME drives an EUV wave, which propagates westward at a speed of ~459 km s-1. After arriving at the filament ~340.3 Mm away from the flare site, the filament is disturbed and starts large-amplitude oscillations, which are mainly observed in 171 {\AA}.The longitudinal oscillations last for nearly two cycles. The average initial amplitude, velocity, period, and damping time are ~4.7 Mm, ~26.5 km s-1, ~1099.1 s, and ~2760.3 s, respectively. According to the pendulum model, the curvature radius and minimum horizontal magnetic field strength of the dips are estimated to be 6.7-9.9 Mm and 4.6-5.6 G. The transverse oscillations last for 2-3 cycles. The average initial amplitude, velocity, period, and damping time are ~1.8 Mm, ~11.2 km s-1, ~994.4 s, and ~3576.2 s, respectively. The radial magnetic field strength of the dips are estimated to be 6.6-7.4 G.