Large-amplitude longitudinal oscillations in solar prominences simulated with different resolutions

Liakh, Valeriia; Luna, Manuel; Khomenko, Elena

doi:10.48550/arxiv.2108.01143

Cited by 4 publications

(6 citation statements)

References 32 publications

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“…An additional degree of freedom has influenced the observed damping in particular. We can expect a third direction to additionally add to the possibility of transverse oscillations in the vertical plane and transferring energy in that direction (as was already shown for the vertical plane by Liakh et al 2021).…”

Section: Discussionmentioning

confidence: 57%

“…Considering the high resolution we employ, we can exclude the role of numerical viscosity on damping (cf. Liakh et al 2021). Prevailing causes of damping include: the conversion of the initial energy transferred from the shock wave to the threads and the resulting redistribution of the prominence mass to the corona.…”

Section: Discussionmentioning

confidence: 99%

“…Our resolution is significantly finer (36×7.5 km) than their highest resolution, thus ensuring that is not an issue here. In addition, Liakh et al (2021) showed that with the dimension of the grid cell of about 30 km, it is sufficient to avoid numerical damping and it is possible to investigate the real physics causes. Moreover, our conservative shock-capturing method does not rely on any added artificial viscosity (but has numerical dissipation which is on a very low order as this scales with the grid size).…”

Section: Energy Analysismentioning

confidence: 99%

“…As a result of the jet's impact, the monolithic prominence experienced both transverse and longitudinal oscillations. Liakh et al (2021) conducted a 2D adiabatic simulation of prominence oscillations to investigate the amplification and attenuation mechanisms of large-amplitude longitudinal oscillations. Additionally, they wanted to find out how grid resolution affects the results of such a study.…”

Section: Introductionmentioning

confidence: 99%

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Multi-threaded prominence oscillations triggered by a coronal shock wave

Jerčić

Keppens

Zhou

2022

A&A

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Context. Understanding the interplay between ubiquitous coronal shock waves and the resulting prominence oscillations is a key factor in improving our knowledge of prominences and the solar corona overall. In particular, prominences are a key element of the solar corona and represent a window into an as yet unexplained processes in the Sun’s atmosphere. Aims. To date, most studies on oscillations of prominences have ignored their finer structure and analyzed them strictly as monolithic bodies. In this work, we study the causal relations between a localised energy release and a remote prominence oscillation, where the prominence has a realistic thread-like structure. Methods. In our work, we used an open source magnetohydrodynamic code known as MPI-AMRVAC to create a multi-threaded prominence body. In this domain, we introduced an additional energy source from which a shock wave originates, thereby inducing prominence oscillation. We studied two cases with different source amplitudes to analyze its effect on the oscillations. Results. Our results show that the frequently used pendulum model does not suffice to fully estimate the period of the prominence oscillation, in addition to showing that the influence of the source and the thread-like prominence structure needs to be taken into account. Repeated reflections and transmissions of the initial shock wave occur at the specific locations of multiple high-temperature and high-density gradients in the domain. This includes the left and right transition region located at the footpoints of the magnetic arcade, as well as the various transition regions between the prominence and the corona. This results in numerous interferences of compressional waves propagating within and surrounding the prominence plasma. They contribute to the restoring forces of the oscillation, causing the period to deviate from the expected pendulum model, in addition to leading to differences in attributed damping or even growth in amplitude between the various threads. Along with the global longitudinal motion that result from the shock impact, small-scale transverse oscillations are also evident. Multiple high-frequency oscillations represent the propagation of magnetoacoustic waves. The damping we see is linked to the conversion of energy and its exchange with the surrounding corona. Our simulations demonstrate the exchange of energy between different threads and their different modes of oscillation.

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Section: Discussionmentioning

confidence: 57%

Section: Discussionmentioning

confidence: 99%

Section: Energy Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Multi-threaded prominence oscillations triggered by a coronal shock wave

Jerčić

Keppens

Zhou

2022

A&A

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“…A simulation shows that mass drainage reduces the damping time considerably in one strong perturbation (Zhang et al 2013). Recent numerical simulations have shed light on the nature of large-amplitude longitudinal oscillations (e.g., Terradas et al 2015;Zhou et al 2018;Adrover-González & Terradas 2020;Liakh et al 2020Liakh et al , 2021.…”

Section: Introductionmentioning

confidence: 99%

Oscillations and mass-draining that lead to a sympathetic eruption of a quiescent filament

Dai,

Zhang,

Zhang

et al. 2021

Preprint

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In this paper, we present a multi-wavelength analysis to mass-draining and oscillations in a large quiescent filament prior to its successful eruption on 2015 April 28. The eruption of a smaller filament that was parallel and in close, ∼350 proximity was observed to induce longitudinal oscillations and enhance mass-draining within the filament of interest. The longitudinal oscillation with an amplitude of ∼25 Mm and ∼23 km s −1 underwent no damping during its observable cycle. Subsequently the slightly enhanced draining may have excited a eruption behind the limb, leading to a feedback that further enhanced the draining and induced simultaneous oscillations within the filament of interest. We find significant damping for these simultaneous oscillations, where the transverse oscillations proceeded with the amplitudes of ∼15 Mm and ∼14 km s −1 , while the longitudinal oscillations involved a larger displacement and velocity amplitude (∼57 Mm, ∼43 km s −1 ). The second grouping of oscillations lasted for ∼2 cycles and had the similar period of ∼2 hours. From this, the curvature radius and transverse magnetic field strength of the magnetic dips supporting the filaments can be estimated to be ∼355 Mm and ≥34 G. The mass-draining within the filament of interest lasted for ∼14 hours. The apparent velocity grew from ∼35 km s −1 to ∼85 km s −1 , with the transition being coincident with the occurrence of the oscillations. We conclude that two filament eruptions are sympathetic, i.e. the eruption of the quiescent filament was triggered by the eruption of the nearby smaller filament.

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The influence of flux rope heating models on solar prominence formation

Jenkins

Keppens

2022

A&A

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Context. Prominences are cool, dense clouds suspended within the solar corona. Their in situ formation through the levitation-condensation mechanism is a textbook example of the thermal instability, where a slight energy imbalance leads to a runaway process resulting in condensed filamentary structures embedded within the concave-up portions of a flux rope. The detailed interplay between local radiative losses and the global heating of the solar corona is investigated here for prominence-forming flux rope structures. Aims. We begin by exploring the influence of two classes of commonly adopted heating models on the formation behaviour of solar prominences. These models consider either an exponential variation dependent on height alone, or local density and magnetic field conditions. We highlight and address some of the limitations inherent to these early approximations by proposing a new, dynamic 2D flux rope heating model that qualitatively accounts for the 3D topology of the twisted flux rope field. Methods. We performed 2.5D grid-adaptive numerical simulations of prominence formation via the levitationcondensation mechanism. A linear force-free arcade is subjected to shearing and converging motions, leading to the formation of a flux rope containing material that may succumb to thermal instability. The eventual formation and subsequent evolution of prominence condensations was then quantified as a function of the specific background heating prescription adopted. For the simulations that consider the topology of the flux rope, reduced heating was considered within a dynamically evolving ellipse that traces the flux rope cross-section. This ellipse is centred on the flux rope axis and tracked during runtime using an approach based on the instantaneous magnetic field curvature. Results. We find that the nature of the heating model is clearly imprinted on the evolution and morphology of any resulting prominences: one large, low-altitude condensation is obtained for the heating model based on local parameters, while the exponential model leads to the additional formation of smaller blobs throughout the flux rope which then relocate as they tend towards achieving hydrostatic equilibrium. Finally, a study of the condensation process in phase space reveals a non-isobaric evolution with an eventual recovery of uniform pressure balance along flux surfaces.

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Large-amplitude longitudinal oscillations in solar prominences simulated with different resolutions

Cited by 4 publications

References 32 publications

Multi-threaded prominence oscillations triggered by a coronal shock wave

Multi-threaded prominence oscillations triggered by a coronal shock wave

Oscillations and mass-draining that lead to a sympathetic eruption of a quiescent filament

The influence of flux rope heating models on solar prominence formation

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