H alpha Surges and X-Ray Jets in AR 7260

Canfield, R. C.; Reardon, K.; Leka, K. D.; Shibata, Kazunari; Yokoyama, T.; Shimojo, Masataka

doi:10.1086/177389

Cited by 277 publications

(305 citation statements)

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“…Rotation about the jet axis (spinning) and helical features were noticed long ago in spicules (Cook et al 1984;Pike & Mason 1998;Sterling et al 2010), surges (Xu et al 1984; Kurokawa et al 1987;Canfield et al 1996), and jets Patsourakos et al 2008; Liu et al…”

Section: Introductionmentioning

confidence: 98%

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Filippov

Srivastava

Dwivedi

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyze multi-wavelength and multi-viewpoint observations of a helically twisted plasma jet formed during a confined filament eruption on 10-11 April 2013. Given a rather large scale event with its high spatial and temporal resolution observations, it allows us to clearly understand some new physical details about the formation and triggering mechanism of twisting jet. We identify a pre-existing flux rope associated with a sinistral filament, which was observed several days before the event. The confined eruption of the filament within a null point topology, also known as an Eiffel tower (or inverted-Y) magnetic field configuration results in the formation of a twisted jet after the magnetic reconnection near a null point. The sign of helicity in the jet is found to be the same as that of the sign of helicity in the filament. Untwisting motion of the reconnected magnetic field lines gives rise to the accelerating plasma along the jet axis. The event clearly shows the twist injection from the pre-eruptive magnetic field to the jet.

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Section: Introductionmentioning

confidence: 98%

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Filippov

Srivastava

Dwivedi

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…The path followed by this enhancement seems to be coincident with the top part of the dark loop. [ Canfield et al, 1996] and also near X-ray bright points [Schmieder et al, 1996].…”

Section: Commentsmentioning

confidence: 99%

The eruptive events on September 30, 1998: 1. The jet

Bagalá¹,

Stenborg²,

Schwenn³

et al. 2001

J. Geophys. Res.

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“…Transient, impulsive, collimated flows of plasma are observed both as bright, emitting features at high (coronal) temperatures and as dark, absorbing features at low (chromospheric) temperatures; generally, these events are referred to as jets and surges, respectively (e.g., Canfield et al 1996). The wavelengths involved range from the optical, through the UV and EUV, to X-rays.…”

Section: Introductionmentioning

confidence: 99%

“…The advent of telescopes placed in space, above Earth's atmosphere, was a prerequisite for the detection of UV and EUV jets from Skylab (Schmahl 1981) and from sounding rockets (Brueckner & Bartoe 1983), and, later still, X-ray jets from Yohkoh (Shibata et al 1992(Shibata et al , 1994Shimojo et al 1996). Cool surges and hot jets are sometimes observed together, in close association in space and time (Canfield et al 1996). Subsequent improvements in the spatial resolutions and temporal cadences of space-borne instruments have enabled more detailed studies of jets and surges from the Solar and Heliospheric Observatory (SOHO; e.g., Wang et al 1998), the Transition Region and Coronal Explorer (e.g., Chae et al 1999), the Solar-Terrestrial Relations Observatory (e.g., Patsourakos et al 2008), Hinode (e.g., Cirtain et al 2007;Savcheva et al 2007;Nishizuka et al 2008;Török et al 2009;Moore et al 2010Moore et al , 2013Liu et al 2011), the Solar Dynamics Observatory (SDO; e.g., Shen et al 2011;Guo et al 2013;Lee et al 2013;Schmieder et al 2013;Zheng et al 2013), and the Interface Region Imaging Spectrograph (e.g., Tian et al 2014;Cheung et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Simulations of Solar Jets Confined by Coronal Loops

Wyper

DeVore

2016

ApJ

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Coronal jets are collimated, dynamic events that occur over a broad range of spatial scales in the solar corona. In the open magnetic field of coronal holes, jets form quasi-radial spires that can extend far out into the heliosphere, while in closed-field regions the jet outflows are confined to the corona. We explore the application of the embedded-bipole model to jets occurring in closed coronal loops. In this model, magnetic free energy is injected slowly by footpoint motions that introduce twist within the closed dome of the jet source region, and is released rapidly by the onset of an ideal kink-like instability. Two length scales characterize the system: the width (N) of the jet source region and the footpoint separation (L) of the coronal loop that envelops the jet source. We find that both the conditions for initiation and the subsequent dynamics are highly sensitive to the ratio L/N. The longest-lasting and most energetic jets occur along long coronal loops with large L/N ratios, and share many of the features of open-field jets, while smaller L/N ratios produce shorter-duration, less energetic jets that are affected by reflections from the far-loop footpoint. We quantify the transition between these behaviors and show that our model replicates key qualitative and quantitative aspects of both quiet Sun and active-region loop jets. We also find that the reconnection between the closed dome and surrounding coronal loop is very extensive: the cumulative reconnected flux at least matches the total flux beneath the dome for small L/N, and is more than double that value for large L/N.

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H alpha Surges and X-Ray Jets in AR 7260

Cited by 277 publications

References 0 publications

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Formation of a rotating jet during the filament eruption on 2013 April 10–11

The eruptive events on September 30, 1998: 1. The jet

Simulations of Solar Jets Confined by Coronal Loops

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