Blowout jets and impulsive eruptive flares in a bald-patch topology

Chandra, Ramesh; Mandrini, C. H.; Schmieder, B.; Joshi, Bhuwan; Cristiani, G.; Cremades, H.; Pariat, É.; Nuevo, F. A.; Srivastava, A. K.; Uddin, Wahab

doi:10.1051/0004-6361/201628984

Cited by 46 publications

(46 citation statements)

References 101 publications

(125 reference statements)

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“…Sterling et al (2015) mention that a likely trigger of the eruption is magnetic flux cancelation in the feet of the magnetic field in and around the minifilament flux rope, and Panesar et al (2016Panesar et al ( , 2018 have presented compelling evidence that in most coronal jets in quiet regions and coronal holes flux cancelation at the polarity inversion line under the pre--jet minifilament triggers the eruption. The results of Panesar et al (2016Panesar et al ( , 2018 are from 23 randomly selected jets, and are consistent with many recent studies of smaller samples of jets in which there is evidence for flux cancelation being the trigger (e.g., Young & Muglach 2014a, 2014bChen & Innes 2016;Chen et al 2017;Zhu et al 2017;Chandra et al 2017). The present paper is a direct follow--on to the Sterling et al (2015) paper.…”

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confidence: 90%

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Moore

Sterling

Panesar

2018

ApJ

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We follow up on the Sterling et al (2015) discovery that nearly all polar coronal X--ray jets are made by an explosive eruption of closed magnetic field carrying a miniature filament in its core. In the same X--ray and EUV movies used by Sterling et al (2015), we examine the onset and growth of the driving magnetic explosion in 15 of the 20 jets that they studied. We find evidence that: (1) in a large majority of polar X--ray jets, the runaway internal/tether--cutting reconnection under the erupting minifilament flux rope starts after both the minifilament's rise and the spire--producing external/breakout reconnection have started; and (2) in a large minority, (a) before the eruption starts there is a current sheet between the explosive closed field and the ambient open field, and (b) the eruption starts with breakout reconnection at that current sheet. The variety of event sequences in the eruptions supports the idea that the magnetic explosions that make polar X--ray jets work the same way as the much larger magnetic explosions that make a flare and coronal mass ejection (CME). That idea, and recent observations indicating that magnetic flux cancelation is the fundamental process that builds the field in and around the pre--jet mininfilament and triggers that field's jet--driving explosion, together suggest that flux cancelation inside the magnetic arcade that explodes in a flare/CME eruption is usually the fundamental process that builds the explosive field in the core of the arcade and triggers that field's explosion.

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confidence: 90%

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Moore

Sterling

Panesar

2018

ApJ

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“…Coronal jets typically show a brighten- navdeep.k.panesar@nasa.gov ing at an edge of their base (called the jet-base bright point, JBP) and a bright spire. Jets are typically observed at sites of emerging and canceling magnetic flux (Shen et al 2012;Panesar et al 2016a;Sterling et al 2016;Chandra et al 2017). The jet spire is produced by magnetic reconnection of closed field in the base with ambient open or far-reaching field; the spire plasma is driven out along the reconnected open/far-reaching field.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Flux Cancellation as the Origin of Solar Quiet-region Pre-jet Minifilaments

Panesar

Sterling

Moore

2017

ApJ

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We investigate the origin of ten solar quiet region pre-jet minifilaments, using EUV images from SDO/AIA and magnetograms from SDO/HMI. We recently found (Panesar et al. 2016b) that quiet region coronal jets are driven by minifilament eruptions, where those eruptions result from flux cancelation at the magnetic neutral line under the minifilament. Here, we study the longer-term origin of the pre-jet minifilaments themselves. We find that they result from flux cancelation between minority-polarity and majority-polarity flux patches. In each of ten pre-jet regions, we find that opposite-polarity patches of magnetic flux converge and cancel, with a flux reduction of 10-40% from before to after the minifilament appears. For our ten events, the minifilaments exist for periods ranging from 1.5 hr to two days before erupting to make a jet. Apparently, the flux cancelation builds highly sheared field that runs above and traces the neutral line, and the cool-transition-region-plasma minifilament forms in this field and is suspended in it. We infer that the convergence of the opposite-polarity patches results in reconnection in the low corona that builds a magnetic arcade enveloping the minifilament in its core, and that the continuing flux cancelation at the neutral line finally destabilizes the minifilament field so that it erupts and drives the production of a coronal jet. Thus our observations strongly support that quiet region magnetic flux cancelation results in both the formation of the pre-jet minifilament and its jet-driving eruption.

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“…The solar jets can be divided into two categories, that is, "standard" and "blowout" jets (Moore et al, 2013(Moore et al, , 2015Raouafi et al, 2016;Chandra et al, 2017). Initially this classification was based on their morphology.…”

Section: Introductionmentioning

confidence: 99%

Solar jet on 2014 April 16 modeled by Kelvin–Helmholtz instability

et al. 2018

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We study here the arising of Kelvin-Helmholtz Instability (KHI) in one fast jet of 2014 April 16 observed by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO) in different UV and EUV wavelengths. The evolution of jet indicates the blob like structure at its boundary which could be the observational evidence of the KHI. We model the jet as a moving cylindrical magnetic flux tube of radius a embedded in a magnetic field B i and surrounded by rest magnetized plasma with magnetic field B e . We explore the propagation of the kink MHD mode along the jet that can become unstable against the KHI if its speed exceeds a critical value.Concerning magnetic fields topology we consider three different configurations, notably of (i) spatially homogeneous magnetic fields (untwisted magnetic flux tube), (ii) internal (label 'i') twisted magnetic field and external homogeneous one (label 'e') (single-twisted flux tube), and (iii) both internal and external twisted magnetic fields (double-twisted magnetic flux tube). Plasma densities in the two media ρ i and ρ e are assumed to be homogeneous. The density contrast is defined in two ways: first as ρ e /ρ i and second as ρ e /(ρ i + ρ e ). Computations show that the KHI can occur at accessible flow velocities in all the cases of untwisted and single-twisted flux tubes. It turns out, however, that in the case of a double-twisted flux tube the KHI can merge at an accessible jet speed only when the density contrast is calculated from the ratio ρ e /(ρ i + ρ e ).Evaluated KHI developing times and kink mode wave phase velocities at wavelength of 4 Mm lie in the ranges of 1-6.2 min and 202-271 km s −1 , respectively-all being reasonable for the modeled jet.

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Blowout jets and impulsive eruptive flares in a bald-patch topology

Cited by 46 publications

References 101 publications

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Onset of the Magnetic Explosion in Solar Polar Coronal X-Ray Jets

Magnetic Flux Cancellation as the Origin of Solar Quiet-region Pre-jet Minifilaments

Solar jet on 2014 April 16 modeled by Kelvin–Helmholtz instability

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