Twisting solar coronal jet launched at the boundary of an active region

Schmieder, B.; Guo, Yang; Moreno‐Insertis, F.; Aulanier, G.; Chaouche, L. Yelles; Nishizuka, Naoto; Harra, L. K.; Thalmann, Julia K.; Domínguez, Santiago Vargas; Liu, Y.

doi:10.1051/0004-6361/201322181

Cited by 103 publications

(109 citation statements)

References 62 publications

(89 reference statements)

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“…Such flows might arise from the reconnection between small-scale emerging fields and larger-scale open field lines of ARs (Liu and Su 2014). Also SXR jets are sometimes observed at the boundaries of ARs (Shimizu et al 1994), often associated with parasitic polarities (Schmieder et al 2013). But despite such small-scale events, for most of the time, the magnetic field of an AR evolves slowly and can be considered to be in equilibrium.…”

Section: Temporal Evolution Of Active-region Magnetic Fieldsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

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Section: Temporal Evolution Of Active-region Magnetic Fieldsmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

182

125

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“…Inside the trailing negative polarity of the active region, new positive polarities continued to emerge. An emergence of mixed weak polarities (<500 G) led to several jets in November 2010 Schmieder et al 2013b). …”

Section: Overviewmentioning

confidence: 99%

Proper horizontal photospheric flows in a filament channel

Schmieder

Roudier

Mein

et al. 2014

A&A

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Context. An extended filament in the central part of the active region NOAA 11106 crossed the central meridian on Sept. 17, 2010 in the southern hemisphere. It has been observed in Hα with the THEMIS telescope in the Canary Islands and in 304 Å with the EUV imager (AIA) onboard the Solar Dynamic Observatory (SDO). Counterstreaming along the Hα threads and bright moving blobs (jets) along the 304 Å filament channel were observed during 10 h before the filament erupted at 17:03 UT. Aims. The aim of the paper is to understand the coupling between magnetic field and convection in filament channels and relate the horizontal photospheric motions to the activity of the filament.Methods. An analysis of the proper photospheric motions using SDO/HMI continuum images with the new version of the coherent structure tracking (CST) algorithm developed to track granules, as well as the large scale photospheric flows, was performed for three hours. Using corks, we derived the passive scalar points and produced a map of the cork distribution in the filament channel. Averaging the velocity vectors in the southern hemisphere in each latitude in steps of 3.5 arcsec, we defined a profile of the differential rotation. Results. Supergranules are clearly identified in the filament channel. Diverging flows inside the supergranules are similar in and out of the filament channel. Converging flows corresponding to the accumulation of corks are identified well around the Hα filament feet and at the edges of the EUV filament channel. At these convergence points, the horizontal photospheric velocity may reach 1 km s −1 , but with a mean velocity of 0.35 km s −1 . In some locations, horizontal flows crossing the channel are detected, indicating eventually large scale vorticity. Conclusions. The coupling between convection and magnetic field in the photosphere is relatively strong. The filament experienced the convection motions through its anchorage points with the photosphere, which are magnetized areas (ends, feet, lateral extensions of the EUV filament channel). From a large scale point-of-view, the differential rotation induced a shear of 0.1 km s −1 in the filament. From a small scale point-of-view, any convective motions favored the interaction of the parasitic polarities responsible for the anchorages of the filament to the photosphere with the surrounding network and may explain the activity of the filament.

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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%

“…These characteristics also have been observed, albeit for a much smaller event sample, in jets occurring in closed coronal loops (e.g., 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 magnetic structures hosting these jets range in size from long loops rooted in weak-field areas adjacent to coronal holes, to short loops rooted in strong-field areas within young active regions.…”

Section: Introductionmentioning

confidence: 77%

“…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%

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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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Twisting solar coronal jet launched at the boundary of an active region

Cited by 103 publications

References 62 publications

The magnetic field in the solar atmosphere

The magnetic field in the solar atmosphere

Proper horizontal photospheric flows in a filament channel

Simulations of Solar Jets Confined by Coronal Loops

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