HOMOLOGOUS HELICAL JETS: OBSERVATIONS BYIRIS,SDO, ANDHINODEAND MAGNETIC MODELING WITH DATA-DRIVEN SIMULATIONS

Cheung, Mark C. M.; Pontieu, Bart De; Tarbell, T. D.; Fu, Yixing; Tian, Hui; Testa, Paola; Reeves, Katharine K.; Martínez-Sykora, Juan; Boerner, P.; Wülser, J. P.; Lemen, J. R.; Title, A. M.; Hurlburt, N. E.; Kleint, Lucia; Kankelborg, C. C.; Jaeggli, Sarah A.; Golub, L.; McKillop, S.; Saar, Steven H.; Carlsson, Mats; Hansteen, V. H.

doi:10.1088/0004-637x/801/2/83

Cited by 111 publications

(137 citation statements)

References 88 publications

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“…This is a generic feature of all closed-field jets, most evident when the coronal loop has significant curvature (e.g., Shibata et al 1992;Shimojo et al 1998;Török et al 2009;Yang et al 2012;Guo et al 2013;Lee et al 2013;Schmieder et al 2013;Zheng et al 2013;Cheung et al 2015). The curtain-like shape of our jets was shown to expand as it propagates toward the loop top (driven by the expansion of the ambient field as the background field strength declines with height) and contract again toward the far loop footpoint.…”

Section: Qualitative Featuresmentioning

confidence: 55%

“…As in open-field regions, closed-field jets sometimes are generated repeatedly from the same source region (e.g., Cheung et al 2015). The free energy that drives the jets in our model arose from boundary motions, applied on the photosphere, which were stopped once a single jet was produced.…”

Section: Qualitative Featuresmentioning

confidence: 99%

“…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%

“…It is well-established from observations that such anemone regions form as a result of flux emergence into coronal holes (e.g., Török et al 2009;Liu et al 2011). The photospheric magnetic field beneath the loops typically has a concentrated vertical field of one (minority) polarity embedded within a large-scale, generally weaker vertical field of the other (majority) polarity (e.g., Cheung et al 2015). Magnetic flux tubes that originate within the minority-polarity patch close back to the Sun's surface locally, on the far side of the polarity inversion line encircling the patch.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Qualitative Featuresmentioning

confidence: 55%

Section: Qualitative Featuresmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Simulations of Solar Jets Confined by Coronal Loops

Wyper

DeVore

2016

ApJ

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“…The speed of these jets lie between 86 and 267 km s −1 , and thhey are triggered in the direction of open field lines as shown by Potentialfield Source-surface (PFSS) extrapolations (Schatten et al 1969;Altschuler & Newkirk 1969;Wang & Sheeley 1992). Cheung et al (2015) have presented the evolution of four homologous helical recurrent jets triggered from NOAA AR 11793 in the transition region and corona on July 21, 2013 by using the AIA/SDO. These jets have also been observed by the Interface Region Imaging Spectrograph (IRIS; De Pontieu et al 2014) and the Doppler velocities in these jets have been estimated using the spectral data.…”

Section: Introductionmentioning

confidence: 99%

Kelvin–Helmholtz instability in an active region jet observed with Hinode

Zhelyazkov

Chandra

Srivastava

2016

Astrophys Space Sci

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Over past ten years a variety of jet-like phenomena were detected in the solar atmosphere, including plasma ejections over a range of coronal temperatures being observed as extreme ultraviolet (EUV) and X-ray jets. We study the possibility for the development of Kelvin-Helmholtz (KH) instability of transverse magnetohydrodynamic (MHD) waves traveling along an EUV jet situated on the west side of NOAA AR 10938 and observed by three instruments on board Hinode on 2007 January 15/16 (Chifor et al., Astron. Astrophys. 481, L57 (2008)). The jet was observed around Log T e = 6.2 with up-flow velocities exceeded 150 km s −1 . Using Fe XII λ186 and λ195 line ratios, the measured densities were found to be above Log N e = 11. We have modeled that EUV jet as a vertically moving magnetic flux tube (untwisted and weakly twisted) and have studied the propagation characteristics of the kink (m = 1) mode and the higher m modes with azimuthal mode numbers m = 2, 3, 4. It turns out that all these MHD waves can become unstable at flow velocities in the range of 112-114.8 km s −1 . The lowest critical jet velocity of 112 km s −1 is obtained when modeling the jet as compressible plasma contained in an untwisted magnetic flux tube. When the jet and its environments are treated as incompressible media, the critical jet velocity becomes higher, namely 114.8 km s −1 . A weak twist of the equilibrium magnetic field in the same approximation of incompressible plasmas slightly decreases the threshold Alfvén Mach number, M cr A , and consequently the corresponding critical velocities, notably to 114.4 km s −1 for the kink mode and to 112.4 km s −1 for the higher m modes. We have also compared two analytically found criteria for predicting the threshold Alfvén Mach number for the onset of KH instability and have concluded that one of them yields reliable values for M cr A . Our study of the nature of stable and unstable MHD modes propagating on the jet shows that in a stable regime all the modes are pure surface waves, while the unstable kink (m = 1) mode in untwisted compressible plasma flux tube becomes a leaky wave. In the limit of incompressible media (for the jet and its environment) all unstable modes are non-leaky surface waves.

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

et al. 2016

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Solar jets are fast‐moving, elongated brightenings related to ejections seen in both images and spectra on all scales from barely visible chromospheric jets to coronal jets extending up to a few solar radii. The largest, most powerful jets are the source of type III radio bursts, energetic electrons and ions with greatly enhanced 3He and heavy element abundances. The frequent coronal jets from polar and equatorial coronal holes may contribute to the solar wind. The primary acceleration mechanism for all jets is believed to be release of magnetic stress via reconnection; however the energy buildup depends on the jets' source environment. In this review, we discuss how certain features of X‐ray and EUV jets, such as their repetition rate and association with radio emission, depends on their underlying photospheric field configurations (active regions, polar and equatorial coronal holes, and quiet Sun). (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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HOMOLOGOUS HELICAL JETS: OBSERVATIONS BYIRIS,SDO, ANDHINODEAND MAGNETIC MODELING WITH DATA-DRIVEN SIMULATIONS

Cited by 111 publications

References 88 publications

Simulations of Solar Jets Confined by Coronal Loops

Simulations of Solar Jets Confined by Coronal Loops

Kelvin–Helmholtz instability in an active region jet observed with Hinode

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

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