Impulsive origin of solar spicule-like jets

Srivastava, A. K.; Singh, Balveer; Murawski, K.; Chen, Y.; Sharma, Kanika; Yuan, Ding; Tiwari, Sanjiv K.; Mathioudakis, M.

doi:10.1140/epjp/s13360-023-03833-5

Cited by 2 publications

(6 citation statements)

References 104 publications

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“…In addition, we include the effect of thermal conduction for both ions and neutrals in the model solar atmosphere, which may generically result in some energy transport towards the solar chromosphere, thus causing energy re-distribution during the propagation of these cool jets. However, this causes some background plasma upflows in the model solar atmosphere that enables more increased kinetic motions of the transition region counterpart of the spicular jets [7]. In the present model, thermal conduction may also create the damping of magnetoacoustic shocks/waves [7].…”

Section: Resultsmentioning

confidence: 99%

“…However, this causes some background plasma upflows in the model solar atmosphere that enables more increased kinetic motions of the transition region counterpart of the spicular jets [7]. In the present model, thermal conduction may also create the damping of magnetoacoustic shocks/waves [7]. Therefore, the ion–neutral collisions and thermal conduction may have a substantial impact on the formation, triggering/evolution of chromospheric cool jets by influencing their generation, propagation, dissipation, and thermal properties.…”

Section: Resultsmentioning

confidence: 99%

“…The complex magnetic field structuring and highly dynamic nature of the Sun's chromosphere permit the genesis of numerous high speed jet-like plasma ejecta at different time and spatial scales [1][2][3][4][5][6][7][8]. These cool spicule-like jets are significant dynamical plasma processes that may be accompanied by various types of waves, oscillations, instabilities etc.…”

Section: Introductionmentioning

confidence: 99%

“…These jets may also have impulsive origin, and they could exhibit quasi-periodic upward and downward plasma motions along their spine in the localized solar atmosphere. There are several observational and theoretical results available, which frequently describe their origin, evolution, physical properties and associated plasma processes [6][7][8]14,22]. However, their exact triggering mechanisms are still unclear, thereby detailed investigation is always an essential requirement using observations with high resolution observations as well as extensive numerical modelling.…”

Section: Introductionmentioning

confidence: 99%

“…The process generally proposed as the agents causing the formation of cool spicular jets and other chromospheric cool plasma ejecta (e.g. cool jets, network jets, macrospicules, spicules, swirls etc) is the shock-generated model [1,4,6,7,14,27,44,47,49]. Hansteen et al [14] reported the formation of cool jet-like plasma ejections (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Alfvén pulse driven spicule-like jets in the presence of thermal conduction and ion-neutral collision in two-fluid regime

Srivastava,

Singh,

Singh

et al. 2024

Phil. Trans. R. Soc. A.

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We present the formation of quasi-periodic cool spicule-like jets in the solar atmosphere using 2.5-D numerical simulation in two-fluid regime (ions+neutrals) under the presence of thermal conduction and ion-neutral collision. The nonlinear, impulsive Alfvénic perturbations at the top of the photosphere trigger field aligned magnetoacoustic perturbations due to ponderomotive force. The transport of energy from Alfvén pulse to such vertical velocity perturbations due to ponderomotive force is considered as an initial trigger mechanism. Thereafter, these velocity perturbations steepen into the shocks followed by quasi-periodic rise and fall of the cool jets transporting mass in the overlying corona. This article is part of the theme issue ‘Partially ionized plasma of the solar atmosphere: recent advances and future pathways’.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Alfvén pulse driven spicule-like jets in the presence of thermal conduction and ion-neutral collision in two-fluid regime

Srivastava,

Singh,

Singh

et al. 2024

Phil. Trans. R. Soc. A.

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Numerical Simulations of the Decaying Transverse Oscillations in the Cool Jet

Srivastava

Singh

2023

Physics

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In the present paper, we describe a 2.5D (two-and-a-half-dimensional) magnetohydrodynamic (MHD) simulation that provides a detailed picture of the evolution of cool jets triggered by initial vertical velocity perturbations in the solar chromosphere. We implement random multiple velocity, Vy, pulses of amplitude 20–50 km s−1 between 1 Mm and 1.5 Mm in the Sun’s atmosphere below its transition region (TR). These pulses also consist of different switch-off periods between 50 s and 300 s. The applied vertical velocity pulses create a series of magnetoacoustic shocks steepening above the TR. These shocks interact with each other in the inner corona, leading to complex localized velocity fields. The upward propagation of such perturbations creates low-pressure regions behind them, which propel a variety of cool jets and plasma flows in the localized corona. The localized complex velocity fields generate transverse oscillations in some of these jets during their evolution. We study the transverse oscillations of a representative cool jet J1, which moves up to the height of 6.2 Mm above the TR from its origin point. During its evolution, the plasma flows make the spine of jet J1 radially inhomogeneous, which is visible in the density and Alfvén speed smoothly varying across the jet. The highly dense J1, which is triggered along the significantly curved magnetic field lines, supports the propagating transverse wave of period of approximately 195 s with a phase speed of about 125 km s−1. In the distance–time map of density, it is manifested as a transverse kink wave. However, the careful investigation of the distance–time maps of the x- and z-components of velocity reveals that these transverse waves are actually of mixed Alfvénic modes. The transverse wave shows evidence of damping in the jet. We conclude that the cross-field structuring of the density and characteristic Alfvén speed within J1 causes the onset of the resonant conversion and leakage of the wave energy outward to dissipate these transverse oscillations via resonant absorption. The wave energy flux is estimated as approximately of 1.0 × 106 ergs cm−2 s−1. This energy, if it dissipates through the resonant absorption into the corona where the jet is propagated, is sufficient energy for the localized coronal heating.

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Impulsive origin of solar spicule-like jets

Cited by 2 publications

References 104 publications

Alfvén pulse driven spicule-like jets in the presence of thermal conduction and ion-neutral collision in two-fluid regime

Alfvén pulse driven spicule-like jets in the presence of thermal conduction and ion-neutral collision in two-fluid regime

Numerical Simulations of the Decaying Transverse Oscillations in the Cool Jet

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