A Micro Coronal Mass Ejection Associated Blowout Extreme-Ultraviolet Jet

Hong, Jiang; Jiang, Yong; Zheng, Ruisheng; Yang, Jiayan; Bi, Yi; Yang, Bo

doi:10.1088/2041-8205/738/2/l20

Cited by 114 publications

(119 citation statements)

References 22 publications

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“…These features are (a) the innermost part of the bubble, which is located at and around the center of the erupting field (marked by an asterisk), filled with dense plasma-we refer to this part as the "core" of the eruption, (b) the low-density area that immediately surrounds the "core"-we refer to this as the "cavity" and is the result of the cool adiabatic expansion of the rising magnetic field, and (c) the "front" of the erupting structure, which is a thin layer of dense material that envelops the "cavity" and demarcates the outskirts of the erupting field. To some extent, the shape of the eruptions in our simulations is reminiscent of the "three-part" structure of the observed small-scale prominence eruptions (mini or micro CMEs; e.g., Innes et al 2010;Raouafi et al 2010;Hong et al 2011) and/or CMEs (e.g., Reeves et al 2015). Because of this, we refer hereafter to the simulated eruptions as CME-like eruptions.…”

Section: Temperature Density Velocity and Currentmentioning

confidence: 87%

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

Syntelis

Archontis

Tsinganos

2017

ApJ

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We report on three-dimensional (3D) magnetohydrodynamic (MHD) simulations of recurrent eruptions in emerging flux regions. We find that reconnection of sheared field lines, along the polarity inversion line of an emerging bipolar region, leads to the formation of a new magnetic structure, which adopts the shape of a magnetic flux rope (FR) during its rising motion. Initially, the FR undergoes a slow-rise phase and, eventually, it experiences a fast-rise phase and ejective eruption toward the outer solar atmosphere. In total, four eruptions occur during the evolution of the system. For the first eruption, our analysis indicates that the torus instability initiates the eruption and that tether-cutting reconnection of the field lines, which envelop the FR, triggers the rapid acceleration of the eruptive field. For the following eruptions, we conjecture that it is the interplay between tether-cutting reconnection and torus instability that causes the onset of the various phases. We show the 3D shape of the erupting fields, focusing more on how magnetic field lines reconnect during the eruptions. We find that when the envelope field lines reconnect mainly with themselves, hot and dense plasma is transferred closer to the core of the erupting FR.The same area appears to be cooler and less dense when the envelope field lines reconnect with neighboring sheared field lines. The plasma density and temperature distribution, together with the rising speeds, energies, and size of the erupting fields, indicate that they may account for small-scale (mini) coronal mass ejections.

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Section: Temperature Density Velocity and Currentmentioning

confidence: 87%

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

Syntelis

Archontis

Tsinganos

2017

ApJ

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“…The filament in event 3 appears to be faint. A small filament of cool (T ∼0.01-0.10 MK) plasma has been often observed in blowout jets (Moore et al 2010;Hong et al 2011;Shen et al 2012;Filippov et al 2015). Figure 6 shows the evolution of the EUV jets in highcadence 171Å images.…”

Section: Event Sourcesmentioning

confidence: 99%

³He-rich Solar Energetic Particles in Helical Jets on the Sun

Bučík

Innes

Mason

et al. 2018

ApJ

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Particle acceleration in stellar flares is ubiquitous in the Universe, however, our Sun is the only astrophysical object where energetic particles and their source flares can both be observed. The acceleration mechanism in solar flares, tremendously enhancing (up to a factor of ten thousand) rare elements like 3 He and ultra-heavy nuclei, has been puzzling for almost 50 years. Here we present some of the most intense 3 He-and Fe-rich solar energetic particle events ever reported. The events were accompanied by non-relativistic electron events and type III radio bursts. The corresponding high-resolution, extreme-ultraviolet imaging observations have revealed for the first time a helical structure in the source flare with a jet-like shape. The helical jets originated in relatively small, compact active regions, located at the coronal hole boundary. A mini-filament at the base of the jet appears to trigger these events. The events were observed with the two Solar Terrestrial Relations Observatories STEREO on the backside of the Sun, during the period of increased solar activity in 2014. The helical jets may be a distinct feature of these intense events that is related to the production of high 3 He and Fe enrichments.

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“…They are observed in X-rays (e.g., Shimojo et al 1996;Cirtain et al 2007) and at a variety of extreme-ultraviolet (EUV) wavelengths (e.g., Nisticò et al 2009;Zhang et al 2016), reflecting the fact that some jets possess both hot and cool (relative to the ambient corona) components. Some jets are energetic enough to reach the heliosphere and become visible as jet-like coronal mass ejections (CMEs) in white-light coronagraphs (e.g., Wang et al 1998;Patsourakos et al 2008;Hong et al 2011;Moore et al 2015). From X-ray observations, Savcheva et al (2007) found that a sample of around 100 jets had typical lifetimes of around 10 minutes, lengths on the order of 50 Mm, widths of around 8 Mm, and bulk outflow velocities of around -200 km s 1 .…”

Section: Introductionmentioning

confidence: 99%

“…In jets where magnetogram data are available, it is often observed that little or no flux emergence occurs leading up to or during the jet (e.g., Chandrashekhar et al 2014;Hong et al 2016). More typically, flux is actually canceling at the base of the jet (e.g., Chae et al 1999;Hong et al 2011;Liu et al 2011;Adams et al 2014;Young & Muglach 2014aPanesar et al 2016). Therefore, while flux emergence is highly likely to account for the generation of some coronal jets, it seems improbable that it explains all such events.…”

Section: Introductionmentioning

confidence: 99%

“…These "mini-filaments" are observed along and above the polarity inversion lines (PILs) of preexisting strong bipoles (e.g., Chae et al 1999;Hong et al 2011Hong et al , 2014Hong et al , 2016Zheng et al 2012;Adams et al 2014;Panesar et al 2016;Zhang et al 2016). They contain cool, dense plasma (relative to the ambient corona) and resemble the large-scale filaments that erupt as CMEs, leaving behind arcades of bright flare loops.…”

Section: Introductionmentioning

confidence: 99%

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A Breakout Model for Solar Coronal Jets with Filaments

Wyper

DeVore²,

Antiochos³

2018

ApJ

137

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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A Micro Coronal Mass Ejection Associated Blowout Extreme-Ultraviolet Jet

Cited by 114 publications

References 22 publications

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

³He-rich Solar Energetic Particles in Helical Jets on the Sun

A Breakout Model for Solar Coronal Jets with Filaments

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A Micro Coronal Mass Ejection Associated Blowout Extreme-Ultraviolet Jet

Cited by 114 publications

References 22 publications

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

3He-rich Solar Energetic Particles in Helical Jets on the Sun

A Breakout Model for Solar Coronal Jets with Filaments

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Product

Resources

About

³He-rich Solar Energetic Particles in Helical Jets on the Sun