Transverse Oscillations in a Coronal Loop Triggered by a Jet

Sarkar, Shilpa; Pant, Vaibhav; Srivastava, A. K.; Banerjee, D.

doi:10.1007/s11207-016-1019-6

Cited by 17 publications

(16 citation statements)

References 52 publications

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“…Using the magneto-seismology technique, the measured oscillation parameters could be used to derive the magnetic field strength of the loops/filaments. For example, Sarkar et al [225] reported a case of jet-driven transverse oscillation of a coronal loop whose magnetic field strength was estimated to be about 2.68-4.5 Gauss. Luna et al [214] estimated the minimum magnetic field strength of an oscillating filament to be about 14 Gauss.…”

Section: (C) Magnetohydrodynamic Wavesmentioning

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.

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Section: (C) Magnetohydrodynamic Wavesmentioning

confidence: 99%

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

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“…Besides the ordinary collimated motions, jets often exhibit helical structure and untwisting motions (Shen et al, 2011;Shen et al, 2012). In addition to helical and untwisting motions, jet displays the swaying motions (transverse oscillations) (Sarkar et al, 2016). Jets may also be formed by shock waves (e.g., De Pontieu et al, 2004).…”

Section: Introductionmentioning

confidence: 99%

Blobs in a Solar EUV Jet

Chen

Erdélyi

et al. 2022

Front. Astron. Space Sci.

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An Extreme Ultraviolet (EUV) jet that occurred around 22:30 on July 2, 2012 was observed by the Atmospheric Imaging Assembly (AIA) on-board the Solar Dynamics Observatory (SDO). There were two phases of the jet. In Phase 1, two blobs were observed. In Phase 2, the intensity of the jet was almost coherent initially. One minute later, three blobs were formed at the same time in the jet, and the width of the jet changed after the formation of these blobs. The formation and evolution processes of the blobs in these two phases are analyzed in this paper. The physical parameters of the blobs are determined. The measured width of the blobs is 0.8 − 2.3 Mm, and the apparent velocities of the blobs are from 59 km s−1 to 185 km s−1. The formation mechanism of the blobs is likely to be tear-mode instability.

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“…Catalogs of observations have been produced by Zimovets and Nakariakov (2015) and . Kink oscillations attract a lot of attention due to their potential for seismological studies of the coronal plasma (e.g., reviews by De Moortel and Stepanov et al, 2012;Pascoe, 2014;De Moortel et al, 2016), in particular to estimate the strength of the coronal magnetic field (e.g., Nakariakov et al, 1999;Nakariakov and Ofman, 2001;Van Doorsselaere et al, 2007;White and Verwichte, 2012;Pascoe et al, 2016;Sarkar et al, 2016).…”

Section: Introductionmentioning

confidence: 99%

Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table

Pascoe

Hood

Doorsselaere

2019

Front. Astron. Space Sci.

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The transverse structure of coronal loops plays a key role in the physics but the small transverse scales can be difficult to observe directly. For wider loops the density profile may be estimated by forward modeling of the transverse intensity profile. The transverse density profile may also be estimated seismologically using kink oscillations in coronal loops. The strong damping of kink oscillations is attributed to resonant absorption and the damping profile contains information about the transverse structure of the loop. However, the analytical descriptions for damping by resonant absorption presently only describe the behavior for thin inhomogeneous layers. Previous numerical studies have demonstrated that this thin boundary approximation produces poor estimates of the damping behavior in loops with wider inhomogeneous layers. Both the seismological and forward modeling approaches suggest loops have a range of layer widths and so there is a need for a description of the damping behavior that accurately describes such loops. We perform a parametric study of the damping of standing kink oscillations by resonant absorption for a wide range of inhomogeneous layer widths and density contrast ratios, with a focus on the values most relevant to observational cases. We describe the damping profile produced by our numerical simulations without prior assumption of its shape and compile our results into a lookup table which may be used to produce accurate seismological estimates for kink oscillation observations.

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Transverse Oscillations in a Coronal Loop Triggered by a Jet

Cited by 17 publications

References 52 publications

Observation and modelling of solar jets

Observation and modelling of solar jets

Blobs in a Solar EUV Jet

Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table

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