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Simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament induced by a single shock wave

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TLDR
In this paper, the authors present the first stereoscopic and Doppler observations of simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament launched by a single shock wave.
Abstract
We present the first stereoscopic and Doppler observations of simultaneous transverse oscillations of a prominence and a filament and longitudinal oscillation of another filament launched by a single shock wave. Using H alpha Doppler observations, we derive the three-dimensional oscillation velocities at different heights along the prominence axis. The results indicate that the prominence has a larger oscillation amplitude and damping time at higher altitude, but the periods at different heights are the same (i.e., 13.5 minutes). This suggests that the prominence oscillates like a linear vertical rigid body with one end anchored on the Sun. One of the filaments shows weak transverse oscillation after the passing of the shock, which is possibly due to the low altitude of the filament and the weakening (due to reflection) of the shock wave before the interaction. Large-amplitude longitudinal oscillation is observed in the other filament after the passing of the shock wave. The velocity amplitude and period are about 26.8 kms(-1) and 80.3 minutes, respectively. We propose that the orientation of a filament or prominence relative to the normal vector of the incoming shock should be an important factor for launching transverse or longitudinal filament oscillations. In addition, the restoring forces of the transverse prominence are most likely due to the coupling of gravity and magnetic tension of the supporting magnetic field, while that for the longitudinal filament oscillation is probably the resultant force of gravity and magnetic pressure.

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Citations
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Multiwavelength observations of a partially eruptive filament on 2011 september 8

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Magnetic flux ropes in the solar corona: structure and evolution toward eruption

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Observation and Modeling of Solar Jets

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A quasi-periodic fast-propagating magnetosonic wave associated with the eruption of a magnetic flux rope

TL;DR: In this paper, a detailed observational analysis of a high-quality quasi-periodic fast-propagating (QFP) magnetosonic wave that was associated with the eruption of a magnetic flux rope and a GOES C5.0 flare is presented.
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Three-dimensional MHD Simulations of Solar Prominence Oscillations in a Magnetic Flux Rope

TL;DR: In this paper, a three-dimensional ideal magnetohydrodynamic simulation of prominence oscillations along a magnetic flux rope was performed, with the aim to compare the oscillation periods with those predicted by various simplified models and to examine the restoring force.
References
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The Solar Dynamics Observatory (SDO)

TL;DR: The Solar Dynamics Observatory (SDO) was launched on 11 February 2010 at 15:23 UT from Kennedy Space Center aboard an Atlas V 401 (AV-021) launch vehicle as mentioned in this paper.
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The Reuven Ramaty High-Energy Solar Spectroscopic Imager (Rhessi)

TL;DR: RHESSI as discussed by the authors is a Principal Investigator (PI) mission, where the PI is responsible for all aspects of the mission except the launch vehicle, and is designed to investigate particle acceleration and energy release in solar flares, through imaging and spectroscopy of hard X-ray/gamma-ray continua emitted by energetic electrons, and of gamma-ray lines produced by energetic ions.
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The STEREO Mission: An Introduction

TL;DR: The twin STEREO spacecraft were launched on October 26, 2006, at 00:52 UT from Kennedy Space Center aboard a Delta 7925 launch vehicle to understand the causes and mechanisms of coronal mass ejection (CME) initiation and follow the propagation of CMEs through the inner heliosphere to Earth as mentioned in this paper.
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Photospheric and heliospheric magnetic fields

TL;DR: In this article, the authors assimilated SOHO/MDI magnetograms into a flux-dispersal model, showing the evolving field on the full sphere with an unprecedented duration of 5.5 years and temporal resolution of 6 hours.
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