Magnetohydrodynamic Simulations of Spicular Jet Propagation Applied to Lower Solar Atmosphere Model

Dover, Fionnlagh Mackenzie; Sharma, Rahul; Erdélyi, R.

doi:10.3847/1538-4357/abefd1

Cited by 11 publications

(7 citation statements)

References 64 publications

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“…Initially, we apply 30 randomly generated vertical velocity pulses in the chromosphere between 1 and 1.5 Mm height, which is accountable for the triggering of cool jets moving up in the model solar atmosphere along the magnetic field lines. These vertical velocity perturbations are applied for a fixed time ranging from 50 to 300 s (e.g., [16]). The applied perturbation is represented by the following equation (e.g., [16]):…”

Section: Perturbationmentioning

confidence: 99%

“…These vertical velocity perturbations are applied for a fixed time ranging from 50 to 300 s (e.g., [16]). The applied perturbation is represented by the following equation (e.g., [16]):…”

Section: Perturbationmentioning

confidence: 99%

“…These plasma ejecta may contribute to the transport of mass and substantial energy into the overlying layers of the Sun's atmosphere, i.e., the transition region (TR) and corona. The transport of mass and energy from the lower atmosphere to the outer corona may elucidate various physical mechanisms contributing to the localized heating, which is still an outstanding problem in solar physics (e.g., [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19] and references therein). These chromospheric plasma ejecta are mostly collimated beam-like plasma structures.…”

Section: Introductionmentioning

confidence: 99%

“…Extensive studies reveal that such structures are ubiquitous and quasi-periodic on the limbs and disks of the solar atmosphere. These jet-like structures are also categorized based on their physical and morphological properties (e.g., [3,[5][6][7]10,12,16,18,20,21] and references therein).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Perturbationmentioning

confidence: 99%

“…These vertical velocity perturbations are applied for a fixed time ranging from 50 to 300 s (e.g., [16]). The applied perturbation is represented by the following equation (e.g., [16]):…”

Section: Perturbationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Numerical Simulations of the Decaying Transverse Oscillations in the Cool Jet

Srivastava

Singh

2023

Physics

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“…These jets show quasi-periodic rise and fall in the model solar atmosphere and describe the physical manifestation of spicules. There are several single fluid MHD models in ideal and non-ideal regime, that clearly depict the generation of cool spicular jets [52,53].…”

Section: Introductionmentioning

confidence: 99%

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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Interaction of convective plasma and small-scale magnetic fields in the lower solar atmosphere

Domínguez

Utz

2022

Rev. Mod. Plasma Phys.

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In the following short review we will outline some of the possible interaction processes of lower solar atmospheric plasma with the embedded small-scale solar magnetic fields. After introducing the topic, important types of small-scale solar magnetic field elements are outlined to then focus on their creation and evolution, and finally end up describing foremost processes these magnetic fields are involved in, such as the reconnection of magnetic field lines and the creation of magneto-hydrodynamic waves. The occurrence and global coverage in the solar atmosphere of such small-scale phenomena surpass on average those of the more explosive and intense events, mainly related to solar active regions and, therefore, their key role as building blocks of solar activity even during the weaker phases of the 11-year solar cycle. In particular, understanding the finest ingredients of solar activity from the lower to the upper solar atmosphere could be determinant to fully understand the heating of the solar corona, which stands out as one of the most intriguing problems in astrophysics nowadays.

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Magnetohydrodynamic Simulations of Spicular Jet Propagation Applied to Lower Solar Atmosphere Model

Cited by 11 publications

References 64 publications

Numerical Simulations of the Decaying Transverse Oscillations in the Cool Jet

Numerical Simulations of the Decaying Transverse Oscillations in the Cool Jet

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

Interaction of convective plasma and small-scale magnetic fields in the lower solar atmosphere

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