Eruptive Instability of the Magnetic-Flux Rope: Gravitational Force and Mass-Unloading

Tsap, Yu. T.; Filippov, B. P.; Kopylova, Yu. G.

doi:10.1007/s11207-019-1423-9

Cited by 9 publications

(3 citation statements)

References 39 publications

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“…The most reasonable force that can terminate ascending of the flux rope and balance the Lorenz force seems gravity. The gravity force can be negligible at a low height compared with any component of the Lorenz force and not influence on initial equilibrium and stability of the flux rope, although under certain condition it can increase the value of n c (Tsap et al 2019). The situation is quite different at greater heights.…”

Section: Discussionmentioning

confidence: 99%

Failed prominence eruptions near 24 cycle maximum

Filippov

2020

Monthly Notices of the Royal Astronomical Society

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We analyze 16 failed filament eruptions observed near 24 solar cycle maximum from May 2013 to July 2014. No significant rotation of filament spines is observed during the ascent in all studied failed eruptions, which does not support kink-instability mechanism of triggering the eruptions. We calculate potential magnetic field distributions in the corona above the initial locations of the filaments to study their height dependence. In seven events, the vertical profiles of the decay index n are monotonic. The other nine events occur in the regions with the switchback or saddle-like n-profiles. The direction of the horizontal field near the saddle bottom is turned through more than 100 • relative its direction at the initial filament position, which reveals the quadrupolar magnetic configuration with null points in these regions. The eruptive filaments stop above the null points where the total Lorenz force is directed upward. The most reasonable force that can terminate filament ascending and balance the Lorenz force seems the gravity.

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Section: Discussionmentioning

confidence: 99%

Failed prominence eruptions near 24 cycle maximum

Filippov

2020

Monthly Notices of the Royal Astronomical Society

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“…Previous numerical studies mainly focus on flux rope catastrophes associated with the magnetic parameters of the rope; whether the variation of the mass could cause flux rope catastrophes, however, has hardly been touched upon previously. In fact, as concluded by Low (1996), the total mass of a flux rope should play an important role in stabilizing the rope, which is further confirmed by some recent studies (Hillier & van Ballegooijen 2013;Jenkins et al 2019;Tsap et al 2019;Fan 2020). Moreover, the total mass of a flux rope is usually not conserved but highly dynamic Gibson 2018): it either accumulates via, e.g., coronal condensation (Liu et al 2012;Xia & Keppens 2016;Jenkins & Keppens 2021), or decreases as a result of, e.g., mass unloading (Low 1996) and mass drainage processes (Bi et al 2014;Jenkins et al 2019).…”

Section: Introductionmentioning

confidence: 57%

Confined and eruptive catastrophes of solar magnetic flux ropes caused by mass loading and unloading

Zhang,

Liu,

Wang

et al. 2021

Preprint

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It is widely accepted that coronal magnetic flux ropes are the core structures of large-scale solar eruptive activities, which inflict dramatic impacts on the solarterrestrial system. Previous studies have demonstrated that varying magnetic properties of a coronal flux rope system could result in a catastrophe of the rope, which may trigger solar eruptive activities. Since the total mass of a flux rope also plays an important role in stabilizing the rope, we use 2.5-dimensional magnetohydrodynamic (MHD) numerical simulations in this letter to investigate how a flux rope evolves as its total mass varies. It is found that an unloading process that decreases the total mass of the rope could result in an upward (eruptive) catastrophe in the flux rope system, during which the rope jumps upward and the magnetic energy is released. This indicates that mass unloading processes could initiate the eruption of the flux rope. Moreover, when the system is not too diffusive, there is also a downward (confined) catastrophe that could be caused by mass loading processes, via which the total mass accumulates. The magnetic energy, however, is increased during the downward catastrophe, indicating that mass loading processes could cause confined activities that may contribute to the storage of energy before the onset of coronal eruptions.

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“…Later there were found magnetic configurations that can provide equilibrium of coronal structures without taking into account their weight, and that this equilibrium can be suddenly lost leading to eruption (van Tend & Kuperus, 1978;Molodenskii & Filippov, 1987;Priest & Forbes, 1990;Forbes & Isenberg, 1991;Lin et al, 1998;Schmieder et al, 2013). On the other hand, resent researches showed that mass may be able to influence the local and global properties of coronal magnetic configuration (Low et al, 2003;Petrie et al, 2007;Seaton et al, 2011;Gunár et al, 2013;Bi et al, 2014;Reva et al, 2017;Jenkins et al, 2018;Tsap et al, 2019). Therefore, estimation of prominence mass and its role in equilibrium and initiation of an eruption is significant for theory, modeling, and prediction of eruptive events on the Sun.…”

Section: Introductionmentioning

confidence: 99%

Mass of prominences experiencing failed eruptions

Filippov

2021

Preprint

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A number of solar filaments/prominences demonstrate failed eruptions, when a filament at first suddenly starts to ascend and then decelerates and stops at some greater height in the corona. The mechanism of the termination of eruptions is not clear yet. One of the confining forces able to stop the eruption is the gravity force. Using a simple model of a partial current-carrying torus loop anchored to the photosphere and photospheric magnetic field measurements as the boundary condition for the potential magnetic field extrapolation into the corona, we estimated masses of 15 eruptive filaments. The values of the filament mass show rather wide distribution in the range of 4 × 10 15 -270 × 10 16 g. Masses of the most of filaments, laying in the middle of the range, are in accordance with estimations made earlier on the basis of spectroscopic and white-light observations.

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Eruptive Instability of the Magnetic-Flux Rope: Gravitational Force and Mass-Unloading

Cited by 9 publications

References 39 publications

Failed prominence eruptions near 24 cycle maximum

Failed prominence eruptions near 24 cycle maximum

Confined and eruptive catastrophes of solar magnetic flux ropes caused by mass loading and unloading

Mass of prominences experiencing failed eruptions

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