Observations of solar X‐ray and EUV jets and their related phenomena

Innes, D. E.; Bučík, R.; Guo, Lucun; Nitta, N.

doi:10.1002/asna.201612428

Cited by 58 publications

(45 citation statements)

References 90 publications

(137 reference statements)

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“…Solar coronal jets are narrow, short-lived coronal features that occur frequently throughout the entire solar magnetic cycle (Shimojo et al 1998;Wang et al 1998;Savcheva et al 2007;Hong et al 2011;Raouafi et al 2016). These events have been observed in all regions of the solar surface: in active regions (Shibata et al 1992;Innes et al 2011;Panesar et al 2016;Sterling et al 2016Sterling et al , 2017, quiet regions (Hong et al 2011;Innes et al 2016), and coronal holes Nisticò et al 2009;Pucci et al 2013;Sterling et al 2015;Panesar et al 2018). In addition to being wide-spread across the solar surface, they also occur very frequently; Savcheva et al (2007) found that jets in polar coronal holes occur at an average rate of 60 jets per day.…”

Section: Introductionmentioning

confidence: 98%

Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets

McGlasson

Panesar

Sterling

et al. 2019

ApJ

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Coronal jets are transient narrow features in the solar corona that originate from all regions of the solar disk: active regions, quiet sun, and coronal holes. Recent studies indicate that at least some coronal jets in quiet regions and coronal holes are driven by the eruption of a minifilament (Sterling et al. 2015) following flux cancellation at a magnetic neutral line (Panesar et al. 2016). We have tested the veracity of that view by examining 60 random jets in quiet regions and coronal holes using multithermal (304Å, 171Å, 193Å, and 211Å) extreme ultraviolet (EUV) images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and line-of-sight magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). By examining the structure and changes in the magnetic field before, during, and after jet onset, we found that 85% of these jets resulted from a minifilament eruption triggered by flux cancellation at the neutral line. The 60 jets have a mean base diameter of 8800 ± 3100 km and a mean duration of 9 ± 3.6 minutes. These observations confirm that minifilament eruption is the driver and magnetic flux cancellation is the primary trigger mechanism for most coronal hole and quiet region coronal jets.

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Section: Introductionmentioning

confidence: 98%

Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets

McGlasson

Panesar

Sterling

et al. 2019

ApJ

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“…Coronal jets are collimated plasma ejections that occur repeatedly everywhere on the Sun and may contribute a significant amount of mass and energy to the corona and solar wind (Patsourakos et al 2008;Moore et al 2010;Raouafi et al 2010;Sterling et al 2015;Innes et al 2016;Raouafi et al 2016). Recurrent jets often are ejected from coronal bright points throughout their lifetimes of hours to days (Kumar et al 2019).…”

Section: Introductionmentioning

confidence: 99%

First Detection of Plasmoids from Breakout Reconnection on the Sun

Kumar

Karpen

Antiochos

et al. 2019

ApJ

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Transient collimated plasma ejections (jets) occur frequently throughout the solar corona, in active regions, quiet Sun, and coronal holes. Although magnetic reconnection is generally agreed to be the mechanism of energy release in jets, the factors that dictate the location and rate of reconnection remain unclear. Our previous studies demonstrated that the magnetic breakout model explains the triggering and evolution of most jets over a wide range of scales, through detailed comparisons between our numerical simulations and high-resolution observations. An alternative explanation, the resistive-kink model, invokes breakout reconnection without forming and explosively expelling a flux rope. Here we report direct observations of breakout reconnection and plasmoid formation during two jets in the fan-spine topology of an embedded bipole. For the first time, we observed the formation and evolution of multiple small plasmoids with bidirectional flows associated with fast reconnection in 3D breakout current sheets in the solar corona. The first narrow jet was launched by reconnection at the breakout current sheet originating at the deformed 3D null, without significant flare reconnection or a filament eruption. In contrast, the second jet and release of cool filament plasma were triggered by explosive breakout reconnection when the leading edge of the rising flux rope formed by flare reconnection beneath the filament encountered the preexisting breakout current sheet. These observations solidly support both reconnection-driven jet models: the resistive kink for the first jet, and the breakout model for the second explosive jet with a filament eruption.

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“…They occur in different solar environments over a broad range of temporal and spatial scales (Cirtain et al 2007;Moore et al 2010;Innes et al 2016). 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.…”

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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Observations of solar X‐ray and EUV jets and their related phenomena

Cited by 58 publications

References 90 publications

Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets

Magnetic Flux Cancellation as the Trigger Mechanism of Solar Coronal Jets

First Detection of Plasmoids from Breakout Reconnection on the Sun

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

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