Solar chromosphere heating and generation of plasma outflows by impulsively generated two-fluid Alfvén waves

Pelekhata, M.; Murawski, K.; Poedts, Stefaan

doi:10.1051/0004-6361/202141262

Cited by 10 publications

(17 citation statements)

References 47 publications

(57 reference statements)

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“…The authors concluded that ambipolar diffusion has the potential to efficiently heat the chromosphere. Additionally, Kuźma et al (2019), Niedziela et al (2021), andPelekhata et al (2021) showed that in the regime of two-fluid, respectively monochromatic acoustic, impulsively generated magneto-acoustic and Alfvén waves are likely to effectively heat the chromosphere. Moreover, Srivastava et al (2018) proposed that the smallscale, two-fluid penumbral jets that are omnipresent in active regions, possess sufficient energy to heat the solar corona.…”

Section: Introductionmentioning

confidence: 99%

Two-fluid numerical model of chromospheric heating and plasma outflows in a quiet-Sun

Murawski

Musielak

Poedts

et al. 2022

Astrophys Space Sci

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Purpose: This paper addresses long-standing solar physics problems, namely, the heating of the solar chromosphere and the origin of the solar wind. Our aim is to reveal the related mechanisms behind chromospheric heating and plasma outflows in a quiet-Sun. Methods: The approach is based on a two-fluid numerical model that accounts for thermal non-equilibrium (ionization/recombination), non-adiabatic and non-ideal dynamics of protons+electrons and hydrogen atoms. The model is applied to numerically simulate the propagation and dissipation of granulation-generated waves in the chromosphere and plasma flows inside a quiet region. Results: The obtained results demonstrate

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Section: Introductionmentioning

confidence: 99%

Two-fluid numerical model of chromospheric heating and plasma outflows in a quiet-Sun

Murawski

Musielak

Poedts

et al. 2022

Astrophys Space Sci

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“…Along with low-frequency Alfvén waves, a range of MHD waves are generated in the photosphere and travel out along the coronal magnetic field lines (see review of Srivastava et al 2021), including acoustic-gravity waves (Vigeesh et al 2017;Fleck et al 2021), magnetosonic waves (Yadav et al 2021), kink waves (Tiwari et al 2019;Morton et al 2021), and Alfvén waves (Jess et al 2009;Wang & Yokoyama 2020;Pelekhata et al 2021). The propagation, and characteristics, of these waves are likely modified by the configuration of the overlying magnetic field (Bogdan et al 2003;Snow et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Stirring the base of the solar wind: On heat transfer and vortex formation

Finley

Brun

Carlsson

et al. 2022

A&A

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Context. Current models of the solar wind must approximate (or ignore) the small-scale dynamics within the solar atmosphere, however these are likely important in shaping the emerging wave-turbulence spectrum and ultimately heating/accelerating the coronal plasma.Aims. This study strives to make connections between small-scale vortex motions at the base of the solar wind and the resulting heating/acceleration of coronal plasma. Methods. The Bifrost code produces realistic simulations of the solar atmosphere that facilitate the analysis of spatial and temporal scales which are currently at, or beyond, the limit of modern solar telescopes. For this study, the Bifrost simulation is configured to represent the solar atmosphere in a coronal hole region, from which the fast solar wind emerges. The simulation extends from the upper-convection zone (2.5 Mm below the photosphere) to the low-corona (14.5 Mm above the photosphere), with a horizontal extent of 24 Mm x 24 Mm. The network of magnetic funnels in the computational domain influence the movement of plasma, and the propagation of magnetohydrodynamic waves, into the low-corona.Results. The twisting of the coronal magnetic field by photospheric flows, efficiently injects energy into the low-corona. Poynting fluxes of up to 2 − 4 kWm −2 are commonly observed inside twisted magnetic structures with diameters in the low-corona of 1-5 Mm. Torsional Alfvén waves are favourably transmitted along these structures, and will subsequently escape into the solar wind. However, reflections of these waves from the upper boundary condition make it difficult to unambiguously quantify the emerging Alfvén wave-energy flux. Conclusions. This study represents a first step in quantifying the conditions at the base of the solar wind using Bifrost simulations. It is shown that the coronal magnetic field is readily braided and twisted by photospheric flows. Temperature and density contrasts form between regions with active stirring motions and those without. Stronger whirlpool-like flows in the convection, concurrent with magnetic concentrations, launch torsional Alfvén waves up through the magnetic funnel network, which are expected to enhance the turbulent generation of magnetic switchbacks in the solar wind.

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“…Recently, a potential contribution of two-fluid Alfvén waves to the heating of the solar chromosphere and the generation of plasma outflows was investigated by Pelekhata et al (2021). It was found that a significant temperature increase was only observed for large amplitudes of the initial pulse and that these waves can drive plasma outflows that, higher up, may originate the solar wind.…”

Section: Introductionmentioning

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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Solar chromosphere heating and generation of plasma outflows by impulsively generated two-fluid Alfvén waves

Cited by 10 publications

References 47 publications

Two-fluid numerical model of chromospheric heating and plasma outflows in a quiet-Sun

Two-fluid numerical model of chromospheric heating and plasma outflows in a quiet-Sun

Stirring the base of the solar wind: On heat transfer and vortex formation

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

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