High latitude helical surge of May 22, 1989

Ökten, Adnan; Çakmak, Hikmet

doi:10.1007/bf00838472

Cited by 4 publications

(4 citation statements)

References 3 publications

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“…Jets or surges (hereafter, we will refer to both as "jets") with rotary motion have been reported in a lot of studies (e.g., Xu et al 1984;Ökten & Cakmak 1990;Canfield et al 1996;Pike & Mason 1998;Alexander & Fletcher 1999;Harrison et al 2001;Jibben & Canfield 2004;Patsourakos et al 2008;Liu et al 2009;Moore et al 2010). However, the exact physical causes remain unclear due to the limitation of our observations.…”

Section: Introductionmentioning

confidence: 80%

“…About 10 minutes later, it evolved into a collimated structure consisting of separate dense points (see the jointed white arrows in Figure 1(b) and (c)). According tö Okten & Cakmak (1990), these dense points represent the appearance of the rotary motion of the moving plasmas in a jet. The rising speed of the jet front is measured to be 68 km s −1 from the Hα images, and the maximum height traced is up to 5 ×10 4 km.…”

Section: Resultsmentioning

confidence: 99%

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KINEMATICS AND FINE STRUCTURE OF AN UNWINDING POLAR JET OBSERVED BY THE SOLAR DYNAMIC OBSERVATORY /ATMOSPHERIC IMAGING ASSEMBLY

Shen

Liu

et al. 2011

ApJ

117

126

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We present an observational study of the kinematics and fine structure of an unwinding polar jet, with high temporal and spatial observations taken by the Atmospheric Imaging Assembly on board the Solar Dynamic Observatory and the Solar Magnetic Activity Research Telescope. During the rising period, the shape of the jet resembled a cylinder with helical structures on the surface, while the mass of the jet was mainly distributed on the cylinder's shell. In the radial direction, the jet expanded successively at its western side and underwent three distinct phases: the gradually expanding phase, the fast expanding phase, and the steady phase. Each phase lasted for about 12 minutes. The angular speed of the unwinding motion of the jet and the twist transferred into the outer corona during the eruption are estimated to be 11.1 × 10 −3 rad s −1 (period = 564 s) and 1.17-2.55 turns (or 2.34-5.1π), respectively. On the other hand, by calculating the azimuthal component of the magnetic field in the jet and comparing the free energy stored in the non-potential magnetic field with the jet's total energy, we find that the non-potential magnetic field in the jet is enough to supply the energy for the ejection. These new observational results strongly support the scenario that the jets are driven by the magnetic twist, which is stored in the twisted closed field of a small bipole, and released through magnetic reconnection between the bipole and its ambient open field.

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Section: Introductionmentioning

confidence: 80%

Section: Resultsmentioning

confidence: 99%

KINEMATICS AND FINE STRUCTURE OF AN UNWINDING POLAR JET OBSERVED BY THE SOLAR DYNAMIC OBSERVATORY /ATMOSPHERIC IMAGING ASSEMBLY

Shen

Liu

et al. 2011

ApJ

117

126

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“…Xu et al [177] detected the rotating motion in a surge using the Hα spectral observations. With the improvements in the quality of imaging and spectral observations, rotating motion was widely observed in Hα surges [90,178,179], EUV jets [2,88,115,117,180,181] and macrospicules [182,183]. Some observations suggested that the eruptions of twisted filaments sometimes show as rotating jets [84,174,184], and this can be explained as a result of the reconnection between twisted filaments and their surrounding open fields [185].…”

Section: (Ii) Rotating Motionmentioning

confidence: 99%

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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The solar atmosphere is full of complicated transients manifesting the reconfiguration of the solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for our understanding of solar activities at different scales, the magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high-spatio-temporal-resolution, wide-temperature coverage and spectroscopic and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.

show abstract

“…Xu et al [177] detected the rotating motion in a surge using the Hα spectral observations. With the improvement of the quality of imaging and spectral observations, rotating motion was widely observed in Hα surges [90,178,179], EUV jets [2,88,115,117,180,181], and macrospicules [182,183]. Some observations suggested that the eruption of twisted filaments sometime show as rotating jets [84,174,184], and it can be explained as a result of the reconnection between twisted filaments and their surrounding open fields [185].…”

Section: (Ii) Rotating Motionmentioning

confidence: 99%

Observation and Modeling of Solar Jets

Shen

2021

Preprint

View full text Add to dashboard Cite

The solar atmosphere is full of complicated transients manifesting the reconfiguration of solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for the understanding of solar activities at different scales, magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high spatiotemporal resolution, wide-temperature coverage, spectroscopic, and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.

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High latitude helical surge of May 22, 1989

Cited by 4 publications

References 3 publications

KINEMATICS AND FINE STRUCTURE OF AN UNWINDING POLAR JET OBSERVED BY THE SOLAR DYNAMIC OBSERVATORY /ATMOSPHERIC IMAGING ASSEMBLY

KINEMATICS AND FINE STRUCTURE OF AN UNWINDING POLAR JET OBSERVED BY THE SOLAR DYNAMIC OBSERVATORY /ATMOSPHERIC IMAGING ASSEMBLY

Observation and modelling of solar jets

Observation and Modeling of Solar Jets

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