Formation and Evolution of a Multi-Threaded Solar Prominence

Luna, M.; Karpen, J. T.; DeVore, C. R.

doi:10.1088/0004-637x/746/1/30

Cited by 133 publications

(135 citation statements)

References 63 publications

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“…Due to the strong strapping field (cyan field lines) overhead, the expanding sheared field increasingly stretches out to develop a quite flat midsection above the PIL (see also Antiochos et al 1994;DeVore & Antiochos 2000Aulanier et al 2002). Using 1D models with comprehensive descriptions of the thermodynamics, Karpen et al (2001Karpen et al ( , 2005 have shown that such regions can host long-lived condensations that resemble cool, counterstreaming filament plasma (see also Luna et al 2012). Over time, the null point above the strapping field becomes increasingly compressed, and a breakout current sheet (BCS; Figure 4(b)) forms there.…”

Section: Jet Mechanismmentioning

confidence: 99%

A Breakout Model for Solar Coronal Jets with Filaments

Wyper

DeVore²,

Antiochos³

2018

ApJ

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129

162

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractRecent observations have revealed that many solar coronal jets involve the eruption of miniature versions of largescale filaments. Such "mini-filaments" are observed to form along the polarity inversion lines of strong, magnetically bipolar regions embedded in open (or distantly closing) unipolar field. During the generation of the jet, the filament becomes unstable and erupts. Recently we described a model for these mini-filament jets, in which the well-known magnetic-breakout mechanism for large-scale coronal mass ejections is extended to these smaller events. In this work we use 3D magnetohydrodynamic simulations to study in detail three realizations of the model. We show that the breakout-jet generation mechanism is robust and that different realizations of the model can explain different observational features. The results are discussed in relation to recent observations and previous jet models.

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Section: Jet Mechanismmentioning

confidence: 99%

A Breakout Model for Solar Coronal Jets with Filaments

Wyper

DeVore²,

Antiochos³

2018

ApJ

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129

162

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“…Three kinds of models have been proposed. Filament plasma can be formed by condensation of coronal material along magnetic field lines, which may be accumulated in coronal cavities (Karpen et al 2005;Luna et al 2012;Berger et al 2010Berger et al , 2012. A filament may be lifted Two movies are available in electronic form at http://www.aanda.org through the photosphere by a levitation process (Okamoto et al 2008;Lites et al 2010) or formed by successive reconnections between magnetic field lines (van Ballegooijen & Martens 1989;Schmieder et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Proper horizontal photospheric flows in a filament channel

Schmieder

Roudier

Mein

et al. 2014

A&A

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Context. An extended filament in the central part of the active region NOAA 11106 crossed the central meridian on Sept. 17, 2010 in the southern hemisphere. It has been observed in Hα with the THEMIS telescope in the Canary Islands and in 304 Å with the EUV imager (AIA) onboard the Solar Dynamic Observatory (SDO). Counterstreaming along the Hα threads and bright moving blobs (jets) along the 304 Å filament channel were observed during 10 h before the filament erupted at 17:03 UT. Aims. The aim of the paper is to understand the coupling between magnetic field and convection in filament channels and relate the horizontal photospheric motions to the activity of the filament.Methods. An analysis of the proper photospheric motions using SDO/HMI continuum images with the new version of the coherent structure tracking (CST) algorithm developed to track granules, as well as the large scale photospheric flows, was performed for three hours. Using corks, we derived the passive scalar points and produced a map of the cork distribution in the filament channel. Averaging the velocity vectors in the southern hemisphere in each latitude in steps of 3.5 arcsec, we defined a profile of the differential rotation. Results. Supergranules are clearly identified in the filament channel. Diverging flows inside the supergranules are similar in and out of the filament channel. Converging flows corresponding to the accumulation of corks are identified well around the Hα filament feet and at the edges of the EUV filament channel. At these convergence points, the horizontal photospheric velocity may reach 1 km s −1 , but with a mean velocity of 0.35 km s −1 . In some locations, horizontal flows crossing the channel are detected, indicating eventually large scale vorticity. Conclusions. The coupling between convection and magnetic field in the photosphere is relatively strong. The filament experienced the convection motions through its anchorage points with the photosphere, which are magnetized areas (ends, feet, lateral extensions of the EUV filament channel). From a large scale point-of-view, the differential rotation induced a shear of 0.1 km s −1 in the filament. From a small scale point-of-view, any convective motions favored the interaction of the parasitic polarities responsible for the anchorages of the filament to the photosphere with the surrounding network and may explain the activity of the filament.

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“…Karpen et al 2003). Based on the simulations by Luna et al (2012b) and the results by Karpen et al (2005) we can estimate that the speed of the hot flows is of the order of 30 km s −1 . We also take a typical value of ζ = 100 (see Labrosse et al 2010).…”

Section: Prominence Oscillations In a Magnetic Tube With Two Straightmentioning

confidence: 88%

Damping of prominence longitudinal oscillations due to mass accretion

Luna

2016

A&A

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We study the damping of longitudinal oscillations of a prominence thread caused by the mass accretion. We suggested a simple model describing this phenomenon. In this model we considered a thin curved magnetic tube filled with the plasma. The prominence thread is in the central part of the tube and it consists of dense cold plasma. The parts of the tube at the two sides of the thread are filled with hot rarefied plasma. We assume that there are flows of rarefied plasma toward the thread caused by the plasma evaporation at the magnetic tube footpoints. Our main assumption is that the hot plasma is instantaneously accommodated by the thread when it arrives at the thread, and its temperature and density become equal to those of the thread. Then we derive the system of ordinary differential equations describing the thread dynamics. We solve this system of ordinary differential equations in two particular cases. In the first case we assume that the magnetic tube is composed of an arc of a circle with two straight lines attached to its ends such that the whole curve is smooth. A very important property of this model is that the equations describing the thread oscillations are linear for any oscillation amplitude. We obtain the analytical solution of the governing equations. Then we obtain the analytical expressions for the oscillation damping time and periods. We find that the damping time is inversely proportional to the accretion rate. The oscillation periods increase with time. We conclude that the oscillations can damp in a few periods if the inclination angle is sufficiently small, not larger that 10 • , and the flow speed is sufficiently large, not less that 30 km s −1 . In the second model we consider the tube with the shape of an arc of a circle. The thread oscillates with the pendulum frequency dependent exclusively on the radius of curvature of the arc. The damping depends on the mass accretion rate and the initial mass of the threads, that is the mass of the thread at the moment when it is perturbed. First we consider small amplitude oscillations and use the linear description. Then we consider nonlinear oscillations and assume that the damping is slow, meaning that the damping time is much larger that the characteristic oscillation time. The thread oscillations are described by the solution of the nonlinear pendulum problem with slowly varying amplitude. The nonlinearity reduces the damping time, however this reduction is small. Again the damping time is inversely proportional to the accretion rate. We also obtain that the oscillation periods decrease with time. However even for the largest initial oscillation amplitude considered in our article the period reduction does not exceed 20%. We conclude that the mass accretion can damp the motion of the threads rapidly. Thus, this mechanism can explain the observed strong damping of large-amplitude longitudinal oscillations. In addition, the damping time can be used to determine the mass accretion rate and indirectly the coronal heating.

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Formation and Evolution of a Multi-Threaded Solar Prominence

Cited by 133 publications

References 63 publications

A Breakout Model for Solar Coronal Jets with Filaments

A Breakout Model for Solar Coronal Jets with Filaments

Proper horizontal photospheric flows in a filament channel

Damping of prominence longitudinal oscillations due to mass accretion

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