3D numerical simulations of propagating two-fluid, torsional Alfvén waves and heating of a partially ionized solar chromosphere

Kuźma, Błażej; Murawski, K.; Poedts, Stefaan

doi:10.1093/mnras/stab1780

Cited by 11 publications

(17 citation statements)

References 60 publications

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“…1 of Alharbi et al (2021). These conditions are still reasonable as it is shown in the two-fluid simulations of jets and waves in the solar atmosphere (see, e.g., Kuźma et al 2021;Murawski et al 2020;Wójcik et al 2019;Srivastava et al 2018).…”

Section: Model Of the Solar Atmospheresupporting

confidence: 66%

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

González-Avilés,

Murawski,

Zaqarashvili

2022

Preprint

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We study the formation and evolution of jets in the solar atmosphere using numerical simulations of partially ionized plasma. The two-fluid magnetohydrodynamic equations with ion+electron and neutral hydrogen components are used in two-dimensional (2D) Cartesian geometry. Numerical simulations show that a localized nonlinear Gaussian pulse of ion and neutral pressures initially launched from the magnetic null point of a potential arcade located below the transition region quickly develops into a shock due to the decrease of density with height. The shock propagates upwards into the solar corona and lifts the cold and dense chromospheric plasma behind in the form of a collimated jet with an inverted-Y shape. The inverted-Y shape of jets is connected with the topology of a magnetic null point. The pulse also excites a nonlinear wake in the chromosphere, which leads to quasi-periodic secondary shocks. The secondary shocks lift the chromospheric plasma upwards and create quasi-periodic jets in the lower corona. Ion and neutral fluids show generally similar behavior, but their relative velocity is higher near the upper part of jets, which leads to enhanced temperature or heating due to ion-neutral collisions. Simulations of jets with inverted-Y shape and their heating may explain the properties of some jets observed in the solar atmosphere.

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Section: Model Of the Solar Atmospheresupporting

confidence: 66%

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

González-Avilés,

Murawski,

Zaqarashvili

2022

Preprint

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“…We also take into account the thermal conduction which contributes to the formation/dynamics of the cool jets. The governing equations of two-fluid systems in the solar magnetized plasma are given as follows [56,58,61,[63][64][65][66][67][68][69][70]:…”

Section: Model and Initial Configuration (A) The Two-fluid Modelmentioning

confidence: 99%

“…The E i and E n are expressed as total energy densities. The coefficient α c denotes the ion-neutral collisions expressed as follows [56,71,72]:…”

Section: Model and Initial Configuration (A) The Two-fluid Modelmentioning

confidence: 99%

“…The partially ionized solar chromosphere contains ions, electrons and neutrals. Many models of the solar chromosphere, therefore, include non-ideal factors like conduction, radiative cooling, and dissipation predominantly caused by the ion-neutral collisions, providing crucial information regarding the heating and plasma dynamics in the chromosphere [54][55][56]. James et al [57] have described the generation of spicules caused by the dissipation of high-frequency Alfvén waves/pulse invoking the physics of ion-neutral collision damping in axisymmetric and initially untwisted flux tubes by performing 1.5-dimensional simulation.…”

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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“…The vertical profiles of the equilibrium gas pressures and mass densities at the magnetohydrostatic equilibrium state are given by (e.g., Kuźma et al 2021b)…”

Section: Magnetohydrostatic Equilibriummentioning

confidence: 99%

Generation of solar chromosphere heating and coronal outflows by two-fluid waves

Pelekhata

Murawski

Poedts

2023

A&A

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Context. It is known that Alfvén and magnetoacoustic waves both contribute to the heating of the solar chromosphere and drive plasma outflows. In both cases, the thermalization of the wave energy occurs due to ion-neutral collisions, but the obtained rates of plasma heating cannot explain the observational data. The same is true for the magnitudes of the outflows. Aims. The aim of the present paper is to reexamine two-fluid modeling of Alfvén and magnetoacoustic waves in the partially ionized solar chromosphere. We attempt to detect variations in the ion temperature and vertical plasma flows for different wave combinations. Methods. We performed numerical simulations of the generation and evolution of coupled Alfvén and magnetoacoustic waves using the JOANNA code, which solves the two-fluid equations for ions (protons)+electrons and neutrals (hydrogen atoms), coupled by collision terms. Results. We confirm that the damping of impulsively generated small-amplitude waves negligibly affects the chromosphere temperature and generates only slow plasma flows. In contrast, waves generated by large-amplitude pulses significantly increase the chromospheric temperature and result in faster plasma outflows. The maximum heating occurs when the pulse is launched from the center of the photosphere, and the magnitude of the related plasma flows increases with the amplitude of the pulse. Conclusions. Large-amplitude coupled two-fluid Alfvén and magnetoacoustic waves can significantly contribute to the heating of the solar chromosphere and to the generation of plasma outflows.

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3D numerical simulations of propagating two-fluid, torsional Alfvén waves and heating of a partially ionized solar chromosphere

Cited by 11 publications

References 60 publications

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

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

Generation of solar chromosphere heating and coronal outflows by two-fluid waves

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