2019
DOI: 10.3847/1538-4357/ab037a
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Modeling the Effect of Mass-draining on Prominence Eruptions

Abstract: Quiescent solar prominences are observed to exist within the solar atmosphere for up to several solar rotations. Their eruption is commonly preceded by a slow increase in height that can last from hours to days. This increase in the prominence height is believed to be due to their host magnetic flux rope transitioning through a series of neighbouring quasi-equilibria before the main loss-of-equilibrium that drives the eruption. Recent work suggests that the removal of prominence mass from a stable, quiescent f… Show more

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Cited by 34 publications
(32 citation statements)
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“…We see that for the 3G case, the O-point of the flux rope initially oscillates as a result of the formation process before the condensation of the prominence interrupts this bulk oscillation, as indicated with the clear displacement of the O-point to lower heights (cf. Shafranov Shift, Blokland & Keppens 2011a;Jenkins et al 2019). Strikingly, the position of O-point and prominence material in time appear completely correlated between 2800 t 4500 s before the initiation of the internal reconnection that allows both the prominence material to continue falling and the O-point to return to a height of ≈ 15 Mm (an evolution that may prove related/comparable to eruptions that involve the ejection of a flux rope but leave the prominence behind e.g., Gilbert et al 2001;Jenkins et al 2018).…”
Section: Additional Features and Dynamicsmentioning
confidence: 91%
“…We see that for the 3G case, the O-point of the flux rope initially oscillates as a result of the formation process before the condensation of the prominence interrupts this bulk oscillation, as indicated with the clear displacement of the O-point to lower heights (cf. Shafranov Shift, Blokland & Keppens 2011a;Jenkins et al 2019). Strikingly, the position of O-point and prominence material in time appear completely correlated between 2800 t 4500 s before the initiation of the internal reconnection that allows both the prominence material to continue falling and the O-point to return to a height of ≈ 15 Mm (an evolution that may prove related/comparable to eruptions that involve the ejection of a flux rope but leave the prominence behind e.g., Gilbert et al 2001;Jenkins et al 2018).…”
Section: Additional Features and Dynamicsmentioning
confidence: 91%
“…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. ; Antiochos et al 1999;Moore et al 2001;Török & Kliem 2005;Kliem & Török 2006).…”
Section: Introductionmentioning
confidence: 99%
“…The heights place the ropes in the β < 1 region of the solar atmosphere (see Fig. 3 of Gary 2001), implying that plasma does not contribute to the stability of these HFT flux ropes in the same way that it would if their undersides were line-tied to dense photospheric or chromospheric plasma in a BPS configuration or if they contained dense filament plasma (Jenkins et al 2018(Jenkins et al , 2019. If perturbed, reconnection could occur at the HFT under these flux ropes, aiding the eruption of the structure.…”
Section: Discussionmentioning
confidence: 99%