Numerical simulations of large-amplitude oscillations in flux rope solar prominences

Liakh, Valeriia; Luna, M.; Khomenko, E.

doi:10.1051/0004-6361/201937083

Cited by 26 publications

(36 citation statements)

References 106 publications

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“…This model suggests that the period is defined by the radius of curvature of the magnetic field (see also Roberts 2019, for another description of the model). The following studies, based on the analytical calculations or the 2D and 3D simulations, confirmed that the pendulum model describes quite well the periods of longitudinal oscillations under typical prominence conditions (e.g., Luna et al , 2016Zhou et al 2018;Zhang et al 2019;Liakh et al 2020;Fan 2020). Zhou et al (2018) found a systematic discrepancy of some 10% with respect to the pendulum model.…”

Section: Introductionsupporting

confidence: 53%

“…These numerical simulations showed significant damping which might be partly contributed by numerical diffusivity. Liakh et al (2020) studied the convergence of a 2.5D experiment of LALOs excited in a magnetic flux rope. The authors performed an experiment with a spatial resolution of 60 km and compared it to the one with a spatial resolution of 240 km.…”

Section: Introductionmentioning

confidence: 99%

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

Liakh,

Luna,

Khomenko

2021

Preprint

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Context. Large-amplitude longitudinal oscillations (LALOs) in solar prominences have been widely studied in the last decades. However, their damping and amplification mechanisms are not well understood. Aims. In this study, we investigate the attenuation and amplification of LALOs using high-resolution numerical simulations with progressively increasing spatial resolutions. Methods. We performed time-dependent numerical simulations of LALOs using the 2D magnetic configuration that contains a dipped region. After the prominence mass loading in the magnetic dips, we triggered LALOs by perturbing the prominence mass along the magnetic field. We performed the experiments with four values of spatial resolution. Results. In the simulations with the highest resolution, the period shows a good agreement with the pendulum model. The convergence experiment revealed that the damping time saturates at the bottom prominence region with improving the resolution, indicating the existence of a physical reason for the damping of oscillations. At the prominence top, the oscillations are amplified during the first minutes and then are slowly attenuated. The characteristic time suggests more significant amplification in the experiments with the highest spatial resolution. The analysis revealed that the energy exchange between the bottom and top prominence regions is responsible for the attenuation and amplification of LALOs. Conclusions. The high-resolution experiments are crucial for the study of the periods and the damping mechanism of LALOs. The period agrees with the pendulum model only when using high enough spatial resolution. The results suggest that numerical diffusion in simulations with insufficient spatial resolution can hide important physical mechanisms, such as amplification of oscillations.

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Section: Introductionsupporting

confidence: 53%

Section: Introductionmentioning

confidence: 99%

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

Liakh,

Luna,

Khomenko

2021

Preprint

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“…For example, the particularly large amplitude oscillations are reserved for those filaments in the vicinity of a flare, wherein the filaments are subjected to the expanding magnetic pressure bubble of the nearby eruption. The amplitudes of such dynamics are also significantly larger than those at the smaller scales, with velocities and displacements in the region of 30 -100 km s −1 and 110 Mm, respectively (e.g., Luna & Karpen 2012;Luna et al 2014;Liakh et al 2020). More recently, similarly large-scale and correlated mass motions occurring in the lead-up to a filament eruption have been added to the conditions for global flux rope stability (e.g., Bi et al 2014;Reva et al 2017;Jenkins et al 2018Jenkins et al , 2019Fan 2020), alongside the more commonly-considered stability conditions (e.g., torus/kink instability, breakout reconnection, tether cutting, etc.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Structure of an Erupting Filament

Wang

Jenkins

Pillet

et al. 2020

ApJ

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The full 3-D vector magnetic field of a solar filament prior to eruption is presented. The filament was observed with the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope in the chromospheric He i line at 10830Å on May 29 and 30, 2017. We inverted the spectropolarimetric observations with the HAnle and ZEeman Light (HAZEL) code to obtain the chromospheric magnetic field. A bimodal distribution of field strength was found in or near the filament. The average field strength was 24 Gauss, but prior to the eruption we find the 90th percentile of field strength was 435 Gauss for the observations on May 29. The field inclination was about 67 degree from the solar vertical. The field azimuth made an angle of about 47 to 65 degree to the spine axis. The results suggest an inverse configuration indicative of a flux rope topology. He i intensity threads were found to be co-aligned with the magnetic field direction. The filament had a sinistral configuration as expected for the southern hemisphere. The filament was stable on May 29, 2017 and started to rise during two observations on May 30, before erupting and causing a minor coronal mass ejection. There was no obvious change of the magnetic topology during the eruption process. Such information on the magnetic topology of erupting filaments could improve the prediction of the geoeffectiveness of solar storms.

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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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Numerical simulations of large-amplitude oscillations in flux rope solar prominences

Cited by 26 publications

References 106 publications

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

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

Magnetic Structure of an Erupting Filament

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

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