Prominence oscillations

Arregui, I.; Oliver, R.; Ballester, J. L.

doi:10.1007/s41116-018-0012-6

Cited by 89 publications

(100 citation statements)

References 214 publications

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“…They oscillate in response to any perturbations, which are ubiquitous in the solar atmosphere. From the physical point of view, filament oscillations can be divided into transverse and longitudinal modes (Shen et al 2014;Zhang et al 2017;Arregui et al 2018), where the oscillation direction is perpendicular and parallel to the local magnetic field, respectively. Similar to other oscillating phenomena, filament oscillations, characterized by oscillation period and decay time, can also be utilized to estimate some physical parameters, mainly the magnetic field.…”

Section: Introductionmentioning

confidence: 99%

“…Similar to other oscillating phenomena, filament oscillations, characterized by oscillation period and decay time, can also be utilized to estimate some physical parameters, mainly the magnetic field. This is called prominence seismology (Arregui et al 2018). Hence, it is important to understand what determines the oscillation period and what determines the decay time.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Damping Mechanisms of the Solar Filament Longitudinal Oscillations in the Weak Magnetic Field

Zhang

Fang

Chen

2019

ApJ

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Longitudinal oscillations of solar filament have been investigated via numerical simulations continuously, but mainly in one dimension (1D), where the magnetic field line is treated as a rigid flux tube. Whereas those one-dimensional simulations can roughly reproduce the observed oscillation periods, implying that gravity is the main restoring force for filament longitudinal oscillations, the decay time in one-dimensional simulations is generally longer than in observations. In this paper, we perform a twodimensional (2D) non-adiabatic magnetohydrodynamic simulation of filament longitudinal oscillations, and compare it with the 2D adiabatic case and 1D adiabatic and non-adiabatic cases. It is found that, whereas both non-adiabatic processes (radiation and heat conduction) can significantly reduce the decay time, wave leakage is another important mechanism to dissipate the kinetic energy of the oscillating filament when the magnetic field is weak so that gravity is comparable to Lorentz force. In this case, our simulations indicate that the pendulum model might lead to an error of ∼100% in determining the curvature radius of the dipped magnetic field using the longitudinal oscillation period when the gravity to Lorentz force ratio is close to unity.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Damping Mechanisms of the Solar Filament Longitudinal Oscillations in the Weak Magnetic Field

Zhang

Fang

Chen

2019

ApJ

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“…In using the validity condition of oscillatory motion, it is easy to show that our analysis is valid provided the wavelength of waves is larger than 1.28 Mm or k < 4.9 × 10 −6 m −1 (wavenumbers and wavelengths that are currently observed in solar prominences, see, e.g. Arregui et al 2012) . However, this wavelength is larger than the gravitational scale-height corresponding to T = 10 4 K, meaning that for a more accurate description of torsional Alfvén waves observed by Kohutova et.…”

Section: Partial Ionisation Diagnosticsmentioning

confidence: 94%

Diagnostics of plasma ionisation using torsional Alfén waves

Ballai

2020

A&A

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Aims. Using the recently observed torsional Alfvén waves in solar prominences, we determine the ionisation state of the plasma by taking into account that Alfvén waves propagate in a partially ionised prominence plasma. We derive the evolutionary equation of waves and compare the analytical solutions to observations to determine the number density of neutrals. Methods. Using a single fluid plasma approximation, where the wave damping is provided by the Cowling resistivity, we study the temporal evolution of waves. By comparing the solution of equations with observational data (period, amplitude, propagation speed), we determined the value of the Cowling resistivity that led us to draw a conclusion on the amount of neutrals in the partially ionised plasma, a quantity that cannot be measured directly or indirectly. Results. Our results show that damped torsional Alfvén waves are an ideal diagnostic tool for the ionisation state of the plasma. Using a simple model, we find that at the observational temperature of torsional Alfvén waves, the number of neutrals, is of the order of 5 × 10 10 cm −3 .

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“…Both LALOs and LATOs are damped oscillations (see reviews by Tripathi et al 2009;Arregui et al 2018). Several mechanisms for strong damping in LALOs are have been proposed (see review by Tripathi et al (2009)) but the matter is still under debate.…”

Section: Introductionmentioning

confidence: 99%

Simultaneous longitudinal and transverse oscillations in filament threads after a failed eruption

Mazumder¹,

Pant²,

Luna³

et al. 2019

A&A

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Context. Longitudinal and transverse oscillations are frequently observed in the solar prominences and/or filaments. These oscillations are excited by a large scale shock wave, impulsive flares at one leg of the filament threads, or due to any low coronal eruptions. We report simultaneous longitudinal and transverse oscillations in the filament threads of a quiescent region filament. We observe a big filament in the north-west of the solar disk on 6 th July 2017. On 7 th July 2017 it starts rising around 13:00 UT. Then we observe a failed eruption and subsequently, the filament threads start to oscillate around 16 UT. Aims. We observe both transverse and longitudinal oscillations in a filament thread. The oscillations damp down and filament threads almost disappear. Methods. We place horizontal and vertical artificial slits on the filament threads to capture the longitudinal and transverse oscillations of the threads. Data from Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO) is used to detect the oscillations. Results. We find the signatures of large amplitude longitudinal oscillations (LALOs). We also detect damping in LALOs. In one thread of the filament, we observe transverse oscillations (LATOs). Using the pendulum model we estimate the lower limit of magnetic field strength and radius of curvature from the observed parameter of LALOs. Conclusions. We show the co-existence of two different wave modes in the same filament threads. We estimate magnetic field from LALOs and hence suggest a possible range of the length of the filament threads using LATOs.

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Prominence oscillations

Cited by 89 publications

References 214 publications

Damping Mechanisms of the Solar Filament Longitudinal Oscillations in the Weak Magnetic Field

Damping Mechanisms of the Solar Filament Longitudinal Oscillations in the Weak Magnetic Field

Diagnostics of plasma ionisation using torsional Alfén waves

Simultaneous longitudinal and transverse oscillations in filament threads after a failed eruption

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