The kinematics of an untwisting solar jet in a polar coronal hole observed by<i>SDO</i>/AIA

Chen, Huadong; Zhang, Jun; Ma, Suli

doi:10.1088/1674-4527/12/5/009

Cited by 70 publications

(72 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…the helical jet presented in PAD09 seems to fit the key observed properties of blowout jets very well (Moore et al 2010(Moore et al , 2013Liu et al 2011a;Shen et al 2011;Chen et al 2012;Pucci et al 2013): wide spires with multiple structures, intense emission at the footpoints, and strong rotation detected in cooler lines. More directly, the predicted density structure (line-of-sight integration of the square of the density) of our model matched the EUV observations of an example of a blowout jet very well (see Fig.…”

Section: Helical Jetsmentioning

confidence: 59%

“…In 2.5D, upflows are driven by a shear Alfvén wave (Karpen et al 1995(Karpen et al , 1998, while in 3D they are driven by torsional Alfvén waves (Patsourakos et al 2008;Pariat et al 2009Pariat et al , 2010Török et al 2009;Edmondson et al 2009;Rachmeler et al 2010;Dalmasse et al 2012;Lynch et al 2014). The untwisting model can explain the wave-like patterns and significant rotational motions observed in numerous coronal jets, in particular in cool emission lines (e.g., Canfield et al 1996;Harrison et al 2001;Patsourakos et al 2008;Liu et al 2009Liu et al , 2011bKamio et al 2010;Shen et al 2011;Chen et al 2012;Hong et al 2013). …”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Model for straight and helical solar jets

Pariat

Dalmasse

DeVore

et al. 2015

A&A

123

145

View full text Add to dashboard Cite

Context. Jets are dynamic, impulsive, well-collimated plasma events developing at many different scales and in different layers of the solar atmosphere. Aims. Jets are believed to be induced by magnetic reconnection, a process central to many astrophysical phenomena. Studying their dynamics can help us to better understand the processes acting in larger eruptive events (e.g., flares and coronal mass ejections) as well as mass, magnetic helicity, and energy transfer at all scales in the solar atmosphere. The relative simplicity of their magnetic geometry and topology, compared with larger solar active events, makes jets ideal candidates for studying the fundamental role of reconnection in energetic events. Methods. In this study, using our recently developed numerical solver ARMS, we present several parametric studies of a 3D numerical magneto-hydrodynamic model of solar-jet-like events. We studied the impact of the magnetic field inclination and photospheric field distribution on the generation and properties of two morphologically different types of solar jets, straight and helical, which can account for the observed so-called standard and blowout jets. Results. Our parametric studies validate our model of jets for different geometric properties of the magnetic configuration. We find that a helical jet is always triggered for the range of parameters we tested. This demonstrates that the 3D magnetic null-point configuration is a very robust structure for the energy storage and impulsive release characteristic of helical jets. In certain regimes determined by magnetic geometry, a straight jet precedes the onset of a helical jet. We show that the reconnection occurring during the straight-jet phase influences the triggering of the helical jet. Conclusions. Our results allow us to better understand the energization, triggering, and driving processes of straight and helical jets. Our model predicts the impulsiveness and energetics of jets in terms of the surrounding magnetic field configuration. Finally, we discuss the interpretation of the observationally defined standard and blowout jets in the context of our model, as well as the physical factors that determine which type of jet will occur.

show abstract

Section: Helical Jetsmentioning

confidence: 59%

Section: Introductionmentioning

confidence: 99%

Model for straight and helical solar jets

Pariat

Dalmasse

DeVore

et al. 2015

A&A

123

145

View full text Add to dashboard Cite

show abstract

“…The rotation was obviously the unwinding motion of the twisted magnetic field lines. The stored twist and magnetic helicity of the flux rope were possibly transported to the ambient open fields (Liu et al, 2009;Chen et al, 2012;Zhang et al, 2015). The average angular speed (15.7×10 −3 rad s −1 ) of the flux rope is comparable to that of the unwinding jet (11.1×10 −3 rad s −1 ) presented by Shen et al (2011).…”

Section: Summary and Discussionmentioning

confidence: 91%

“…Recently, the direct observations of flux ropes in the low corona have been reported (Li and Zhang, 2013a, 2013cChen et al, 2014aChen et al, , 2014bSong et al, 2014;Joshi et al, 2014b) by using the extreme ultraviolet (EUV) data from the Atmospheric Imaging Assembly (AIA; Lemen et al, 2012) onboard the Solar Dynamics Observatory (SDO; Pesnell et al, 2012). Kumar et al (2010) presented a successive activation of magnetic flux ropes in chromospheric and EUV lines and concluded that such activation plays an important role in triggering the flare.…”

Section: Introductionmentioning

confidence: 99%

High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

Zhang

2015

Sol Phys

Self Cite

View full text Add to dashboard Cite

We report the observations of a flux rope at transition region temperatures with the Interface Region Imaging Spectrograph (IRIS) on 30 August 2014. Initially, magnetic flux cancellation constantly took place and a filament was activated. Then the bright material from the filament moved southward and tracked out several fine structures. These fine structures were twisted and tangled with each other, and appeared as a small flux rope at 1330Å, with a total twist of about 4π. Afterwards, the flux rope underwent a counter-clockwise (viewed top-down) unwinding motion around its axis. Spectral observations of C ii 1335.71Å at the southern leg of the flux rope showed that Doppler redshifts of 6−24 km s −1 appeared at the western side of the axis, which is consistent with the counter-clockwise rotation motion. We suggest that the magnetic flux cancellation initiates reconnection and some activation of the flux rope. The stored twist and magnetic helicity of the flux rope are transported into the upper atmosphere by the unwinding motion in the late stage. The small-scale flux rope (width of 8.3′′ ) had a cylindrical shape with helical field lines, similar to the morphology of the large-scale CME core (width of 1.54 R ⊙ ) on 2 June 1998. This similarity shows the presence of flux ropes of different scales on the Sun.

show abstract

“…In addition, they found that the blowout eruption of the bipole field and the surrounding field often carrying a filament of cool plasma. Subsequently, more and more observations confirmed that many blowout jets are driven by minifilament eruptions (Hong et al 2011(Hong et al , 2016(Hong et al , 2017Chen et al 2012;Shen et al 2011Shen et al , 2012Shen et al , 2017Yang et al 2012;Moore et al 2013;Adams et al 2014;Sterling et al 2016;Li et al 2017). In particular, Sterling et al (2015) investigated 20 near-limb polar coronal hole jets and morphologically classified 14 as blowout, 5 as standard, and 1 as ambiguous.…”

Section: Introductionmentioning

confidence: 94%

Recurrent Two-sided Loop Jets Caused By Magnetic Reconnection between Erupting Minifilaments and a nearby Large Filament

Yang

et al. 2019

ApJ

View full text Add to dashboard Cite

Using high spatial and temporal data from the New Vacuum Solar Telescope (NVST) and the Solar Dynamics Observatory (SDO), we present unambiguous observations of recurrent two-sided loop jets caused by magnetic reconnection between erupting minifilaments and nearby large filament. The observations demonstrate that three twosided loop jets, which ejected along the large filament in opposite directions, had similar appearance and originated from the same region. We find that a minifilament erupted and drove the first jet. It reformed at the same neutral line later, and then underwent partial and total eruptions, drove the second and third jets, respectively. In the course of the jets, cool plasma was injected into the large filament. Furthermore, persistent magnetic flux cancelation occurred at the neutral line under the minifilament before its eruption and continued until the end of the observation. We infer that magnetic flux cancellation may account for building and then triggering the minifilament to erupt to produce the two-sided loop jets. This observation not only indicates that two-sided loop jets can be driven by minifilament eruptions, but also sheds new light on our understanding of the recurrent mechanism of two-sided loop jets.

show abstract

The kinematics of an untwisting solar jet in a polar coronal hole observed bySDO/AIA

Cited by 70 publications

References 72 publications

Model for straight and helical solar jets

Model for straight and helical solar jets

High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

Recurrent Two-sided Loop Jets Caused By Magnetic Reconnection between Erupting Minifilaments and a nearby Large Filament

Contact Info

Product

Resources

About