Ubiquitous Rotating Network Magnetic Fields and Extreme-Ultraviolet Cyclones in the Quiet Sun

Zhang, Jun; Liu, Yang

doi:10.1088/2041-8205/741/1/l7

Cited by 60 publications

(56 citation statements)

References 41 publications

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“…This is a consequence of the high Alfvén speed in the photosphere, which reaches about 70 km s −1 at the upper boundary of the computational box: any twist of the vertical magnetic flux concentrations rapidly escapes upward in the form of torsional Alfvén waves. Such processes may drive swirling flows in the chromosphere (Wedemeyer-Böhm & Rouppe van der Voort 2009) and in the corona (Zhang & Liu 2011). Figure 10 shows height profiles of the temporarily and horizontally averaged temperature and dissipation rates (viscous and Ohmic).…”

Section: Dynamics Of the Upper Photospherementioning

confidence: 99%

Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field

Moll

Cameron

Schüßler

2012

A&A

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Aims. We study the differences between non-magnetic and magnetic regions in the flow and thermal structure of the upper solar photosphere. Methods. Radiative MHD simulations representing a quiet region and a plage region, respectively, which extend into the layers around the temperature minimum, are analyzed. Results. The flow structure in the upper photospheric layers of the two simulations is considerably different: the non-magnetic simulation is dominated by a pattern of moving shock fronts while the magnetic simulation shows vertically extended vortices associated with magnetic flux concentrations. Both kinds of structures induce substantial local heating. The resulting average temperature profiles are characterized by a steep rise above the temperature minimum due to shock heating in the non-magnetic case and by a flat photospheric temperature gradient mainly caused by Ohmic dissipation in the magnetic run. Conclusions. Shocks in the quiet Sun and vortices in the strongly magnetized regions represent the dominant flow structures in the layers around the temperature minimum. They are closely connected with dissipation processes providing localized heating.

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Section: Dynamics Of the Upper Photospherementioning

confidence: 99%

Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field

Moll

Cameron

Schüßler

2012

A&A

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“…Rotating magnetic structures driven by underlying photospheric vortex flows were observed by several authors (Zhang et al 2011;Wedemeyer-Böhm et al 2012;Yan et al 2013). Vršnak (1980) observed the detwisting motions with radial velocity of 100 km/s in prominences by using shapes and profiles of the Hα line.…”

mentioning

confidence: 94%

Kink Instability Evidenced by Analyzing the Leg Rotation of a Filament

Yan

Xue

Liu

et al. 2014

ApJ

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Kink instability is a possible mechanism for solar filament eruption. However, the twist of a solar filament is very difficult to directly measure from observation. In this paper, we carried out the measurement of the twist of a solar filament by analyzing its leg rotation. An inverse S-shaped filament in active region NOAA 11485 was observed by the Atmospheric Imaging Assembly (AIA) of Solar Dynamics Observatory (SDO) on 2012 May 22. During its eruption, the leg of the filament exhibited a significant rotation motion. The 304Å images were used to uncurl along the circles, whose centers are the axis of the filament's leg. The result shows that the leg of the filament rotated up to about 510 degrees (about 2.83π) around the axis of the filament within twenty-three minutes. The maximal rotation speed reached 100 degrees per minute (about 379.9 km/s at radius 18 ′′ ), which is the fastest rotation speed that has been reported. We also calculated the decay index along the polarity inversion line in this active region and found that the decline of the overlying field with height is not so fast enough to trigger the torus instability. According to the condition of kink instability, it is indicating that the kink instability is the trigger mechanism for the solar filament eruption.

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“…Those from the quiet Sun have smaller size and slower speed of 10-100 km s −1 and can be interpreted as slow-mode waves (Podladchikova et al 2010) or non-wave coronal reconfigurations. They are often associated with supergranular flows (Innes et al 2009) or coronal cyclones driven by rotating network magnetic fields (Zhang & Liu 2011;Yu et al 2015). So far, studies on small-scale EUV waves are still very scarce, questions such as their driving mechanism, physical nature, their relation to the variation of photosphere magnetic field, and their role played in the full spectrum of EUV waves are still unclear.…”

Section: Introductionmentioning

confidence: 99%

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

Shen

Liu

Tian

et al. 2017

ApJ

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We present observations of a small-scale Extreme-ultraviolet (EUV) wave that was associated with a mini-filament eruption and a GOES B1.9 micro-flare in the quiet Sun region. The initiation of the event was due to the photospheric magnetic emergence and cancellation in the eruption source region, which first caused the ejection of a small plasma ejecta, then the ejecta impacted on a nearby mini-filament and thereby led to the filament's eruption and the associated flare. During the filament eruption, an EUV wave at a speed of 182 -317 km s −1 was formed ahead of an expanding coronal loop, which propagated faster than the expanding loop and showed obvious deceleration and reflection during the propagation. In addition, the EUV wave further resulted in the transverse oscillation of a remote filament whose period and damping time are 15 and 60 minutes, respectively. Based on the observational results, we propose that the small-scale EUV wave should be a fast-mode magnetosonic wave that was driven by the the expanding coronal loop. Moreover, with the application of filament seismology, it is estimated that the radial magnetic field strength is about 7 Gauss. The observations also suggest that small-scale EUV waves associated with miniature solar eruptions share similar driving mechanism and observational characteristics with their large-scale counterparts.

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Ubiquitous Rotating Network Magnetic Fields and Extreme-Ultraviolet Cyclones in the Quiet Sun

Cited by 60 publications

References 41 publications

Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field

Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field

Kink Instability Evidenced by Analyzing the Leg Rotation of a Filament

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

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