Solar Coronal Jets: Observations, Theory, and Modeling

Raouafi, N. E.; Patsourakos, S.; Pariat, É.; Young, Peter R.; Sterling, Alphonse C.; Savcheva, Antonia; Shimojo, Masataka; Moreno‐Insertis, F.; DeVore, C. R.; Archontis, V.; Török, Tibor; Mason, H. E.; Curdt, W.; Meyer, Karen; Dalmasse, K.; Matsui, Yutaka

doi:10.1007/s11214-016-0260-5

Cited by 328 publications

(318 citation statements)

References 202 publications

Supporting

Mentioning

299

Contrasting

Unclassified

Order By: Relevance

“…Depending on their morphology, solar jets have been recently divided into two categories, standard and blowout (or erupting) jets (Raouafi et al 2016). With their peculiar untwisting motion, blowout jets are still not well understood.…”

Section: Introduction Particle Acceleration In Solar Flaresmentioning

confidence: 99%

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

Bučík

Innes

Mason

et al. 2018

ApJ

View full text Add to dashboard Cite

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.

show abstract

Section: Introduction Particle Acceleration In Solar Flaresmentioning

confidence: 99%

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

Bučík

Innes

Mason

et al. 2018

ApJ

View full text Add to dashboard Cite

show abstract

“…Coronal jets are transient collimated features (Raouafi et al 2016) typically observed in extreme ultraviolet (EUV) (Wang et al 1998) and X-ray (Shibata et al 1992;Canfield et al 1996;Alexander & Fletcher 1999) emission. 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).…”

Section: Introductionmentioning

confidence: 99%

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

Panesar

Sterling

Moore

2017

ApJ

View full text Add to dashboard Cite

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.

show abstract

“…They are most often detected as rapidly evolving linear features in which plasma appears to be accelerated and sometimes heated, with the bulk of the plasma flow often penetrating into the overlying and much hotter corona. There is a wide variety of chromospheric jets, including surges, penumbral microjets, anemone jets, macrospicules, and spicules (Raouafi et al 2016). To fully understand the impact of these different jets on the mass and energy balance of the low solar atmosphere, it is key to better understand the mechanisms that drive these jets.…”

Section: Introductionmentioning

confidence: 99%

What Causes the High Apparent Speeds in Chromospheric and Transition Region Spicules on the Sun?

Pontieu

Martínez-Sykora

Chintzoglou

2017

ApJL

View full text Add to dashboard Cite

Spicules are the most ubuiquitous type of jets in the solar atmosphere. The advent of high-resolution imaging and spectroscopy from the Interface Region Imaging Spectrograph (IRIS) and ground-based observatories has revealed the presence of very high apparent motions of order 100-300 km s −1 in spicules, as measured in the plane of the sky. However, line of sight measurements of such high speeds have been difficult to obtain, with values deduced from Doppler shifts in spectral lines typically of order 30-70 km s −1 . In this work, we resolve this long-standing discrepancy using recent 2.5D radiative MHD simulations. This simulation has revealed a novel driving mechanism for spicules in which ambipolar diffusion resulting from ion-neutral interactions plays a key role. In our simulation, we often see that the upward propagation of magnetic waves and electrical currents from the low chromosphere into already existing spicules can lead to rapid heating when the currents are rapidly dissipated by ambipolar diffusion. The combination of rapid heating and the propagation of these currents at Alfvénic speeds in excess of 100 km s −1 leads to the very rapid apparent motions, and often wholesale appearance, of spicules at chromospheric and transition region temperatures. In our simulation, the observed fast apparent motions in such jets are actually a signature of a heating front, and much higher than the mass flows, which are of order 30-70 km s −1 . Our results can explain the behavior of transition region "network jets" and the very high apparent speeds reported for some chromospheric spicules.

show abstract

Solar Coronal Jets: Observations, Theory, and Modeling

Cited by 328 publications

References 202 publications

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

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

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

What Causes the High Apparent Speeds in Chromospheric and Transition Region Spicules on the Sun?

Contact Info

Product

Resources

About

Solar Coronal Jets: Observations, Theory, and Modeling

Cited by 328 publications

References 202 publications

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

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

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

What Causes the High Apparent Speeds in Chromospheric and Transition Region Spicules on the Sun?

Contact Info

Product

Resources

About

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

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