Case 84

Joarder, Rita; Crundwell, Neil

doi:10.1007/978-0-85729-838-6_84

Cited by 5 publications

(10 citation statements)

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“…The average magnetic field intensity is set to 7.5 Gauss. We have made a time dependent simulation of the system described by Joarder & Roberts (1992b). The model consists of a vertical prominence slab with a horizontal magnetic field transverse to the prominence slab.…”

Section: Model Of Wavesmentioning

confidence: 99%

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Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

Schmieder

Kucera

Knizhnik

et al. 2013

ApJ

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We report an unusual set of observations of waves in a large prominence pillar which consist of pulses propagating perpendicular to the prominence magnetic field. We observe a huge quiescent prominence with the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) in EUV on 2012 October 10 and only a part of it, the pillar, which is a foot or barb of the prominence, with the Hinode Solar Optical Telescope (SOT) (in Ca II and Hα lines), Sac Peak (in Hα, Hβ and Na-D lines), THEMIS ("Télescope Héliographique pour l' Etude du Magnétisme et des Instabilités Solaires") with the MTR (MulTi-Raies) spectropolarimeter (in He D 3 line). The THEMIS/MTR data indicates that the magnetic field in the pillar is essentially horizontal and the observations in the optical domain show a large number of horizontally aligned features on a much smaller scale than the pillar as a whole. The data is consistent with a model of cool prominence plasma trapped in the dips of horizontal field lines. The SOT and Sac Peak data over the 4 hour observing period show vertical oscillations appearing as wave pulses. These pulses, which include a Doppler signature, move vertically, perpendicular to the field direction, along thin quasi-vertical columns in the much broader pillar. The pulses have a velocity of propagation of about 10 km s −1 , a period about 300 sec, and a wavelength around 2000 km. We interpret these waves in terms of fast magneto-sonic waves and discuss possible wave drivers.

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Section: Model Of Wavesmentioning

confidence: 99%

“…The top and bottom boundaries of the simulation box are opened in order to mimic the infinite extension of the prominence in the vertical direction. We refer the reader to Joarder & Roberts (1992b) for the equilibrium configuration and the equations describing the evolution.…”

Section: Model Of Wavesmentioning

confidence: 99%

Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

Schmieder

Kucera

Knizhnik

et al. 2013

ApJ

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“…The first model we can use for the comparison is the infinite straight slab with a transverse constant magnetic field. If the prominence body has a length L p , and the total length of the field lines is L T , then for the situation L p ≪ L T the period is (see for example Joarder & Roberts 1992;Díaz et al 2010;Soler et al 2010)…”

Section: Vertical Oscillationsmentioning

confidence: 99%

Magnetohydrodynamic Waves in Two-Dimensional Prominences Embedded in Coronal Arcades

Terradas

Soler

Díaz

et al. 2013

ApJ

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Solar prominence models used so far in the analysis of MHD waves in such structures are quite elementary. In this work, we calculate numerically magnetohydrostatic models in two-dimensional configurations under the presence of gravity. Our interest is in models that connect the magnetic field to the photosphere and include an overlying arcade. The method used here is based on a relaxation process and requires solving the time-dependent nonlinear ideal MHD equations. Once a prominence model is obtained, we investigate the properties of MHD waves superimposed on the structure. We concentrate on motions purely two-dimensional neglecting propagation in the ignorable direction. We demonstrate how by using different numerical tools we can determine the period of oscillation of stable waves. We find that vertical oscillations, linked to fast MHD waves, are always stable and have periods in the 4-10 min range. Longitudinal oscillations, related to slow magnetoacoustic-gravity waves, have longer periods in the range of 28-40 min. These longitudinal oscillations are strongly influenced by the gravity force and become unstable for short magnetic arcades.

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“…On the other hand, different models have been used to compare analytical expressions to the transverse simulated periods. For example, Terradas et al (2013) and Zhou et al (2018), in their simulations of vertical oscillations, used the slab and string model of Joarder & Roberts (1992b), respectively, and obtained large differences between the analytical and numerical results. Both studies obtained better correlations with the results of Díaz et al (2001), however.…”

Section: Introductionmentioning

confidence: 99%

3D numerical simulations of oscillations in solar prominences

Adrover-González

Terradas

2020

A&A

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Context. Oscillations in solar prominences are a frequent phenomenon, and they have been the subject of many studies. A full understanding of the mechanisms that drive them and their attenuation has not been reached yet, however. Aims. We numerically investigate the periodicity and damping of transverse and longitudinal oscillations in a 3D model of a curtain-shaped prominence. Methods. We carried out a set of numerical simulations of vertical, transverse and longitudinal oscillations with the high-order finite-difference Pencil Code. We solved the ideal magnetohydrodynamic (MHD) equations for a wide range of parameters, including the width (wx) and density (ρp0) of the prominence, and the magnetic field strength (B) of the solar corona. We studied the periodicity and attenuation of the induced oscillations. Results. We found that longitudinal oscillations can be fit with the pendulum model, whose restoring force is the fieldaligned component of gravity, but other mechanisms such as pressure gradients may contribute to the movement. On the other hand, transverse oscillations are subject to magnetic forces. The analysis of the parametric survey shows, in agreement with observational studies, that the oscillation period (P ) increases with the prominence width. For transverse oscillations we obtained that P increases with density and decreases with B. For longitudinal oscillations we also found that P increases with ρp0, but there are no variations with B. The attenuation of transverse oscillations was investigated by analysing the velocity distribution and computing the Alfvén continuum modes. We conclude that resonant absorption is the mean cause. Damping of longitudinal oscillations is due to some kind of shear numerical viscosity. Conclusions. Our model is a good approximation of a prominence body that nearly reproduces the observed oscillations. However, more realistic simulations that include other terms such as non-adiabatic processes or partially ionised plasmas are necessary to obtain better results.

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Case 84

Cited by 5 publications

References 0 publications

Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

Propagating Waves Transverse to the Magnetic Field in a Solar Prominence

Magnetohydrodynamic Waves in Two-Dimensional Prominences Embedded in Coronal Arcades

3D numerical simulations of oscillations in solar prominences

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