Influence of ambipolar and Hall effects on vorticity in three-dimensional simulations of magneto-convection

Khomenko, E.; Collados, M.; Vitas, N.; González-Morales, P. A.

doi:10.1098/rsta.2020.0176

Cited by 10 publications

(10 citation statements)

References 56 publications

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“…The action of Khodachenko & Zaitsev (2002) mechanism in our simulations needs to be investigated further. In a subsequent paper, Khomenko et al (2020) traced an individual long-living feature in the ambihall simulation. The results show that there is an enhancement of the η H coefficient right around the feature coincident with local intensification of the magnetic field.…”

Section: Discussionmentioning

confidence: 99%

Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun

González-Morales

Khomenko

Vitas

et al. 2020

A&A

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The partial ionization of the solar plasma causes several nonideal effects such as the ambipolar diffusion, the Hall effect, and the Biermann battery effect. Here we report on the first three-dimensional realistic simulations of solar local dynamo where all three effects were taken into account. The simulations started with a snapshot of already saturated battery-seeded dynamo, where two new series were developed: one with solely ambipolar diffusion and another one also taking into account the Hall term in the generalized Ohm’s law. The simulations were then run for about 4 h of solar time to reach the stationary regime and improve the statistics. In parallel, a purely MHD dynamo simulation was also run for the same amount of time. The simulations are compared in a statistical way. We consider the average properties of simulation dynamics, the generation and dissipation of compressible and incompressible waves, and the magnetic Poynting flux. The results show that, with the inclusion of the ambipolar diffusion, the amplitudes of the incompressible perturbations related to Alfvén waves are reduced, and the Poynting flux is absorbed, with a frequency dependence. The Hall effect causes the opposite action: significant excess of incompressible perturbations is generated and an excess of the Poynting flux is observed in the chromospheric layers. The model with ambipolar diffusion shows, on average, sharper current sheets and slightly more abundant fast magneto-acoustic shocks in the chromosphere. The model with the Hall effect has higher temperatures at the lower chromosphere and stronger and more vertical magnetic field concentrations all over the chromosphere. The study of high-frequency waves reveals that significant power of incompressible perturbations is associated with areas with intense and more vertical magnetic fields and larger temperatures. This behavior explains the large Poynting fluxes in the simulations with the Hall effect and provides confirmation as to the role of Alfvén waves in chromospheric heating in internetwork regions, under the action of both Hall and ambipolar effects. We find a positive correlation between the magnitude of the ambipolar heating and the temperature increase at the same location after a characteristic time of 102 s.

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Section: Discussionmentioning

confidence: 99%

Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun

González-Morales

Khomenko

Vitas

et al. 2020

A&A

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“…Furthermore, the heating through ion-neutral collisions will affect the reconnection rate and may give more homogenous heating in the emergence regions (Leake & Arber, 2006). Finally, the inclusion of ambipolar diffusion and the Hall effect will further help the production of Poynting flux in the form of Alfvén waves (Khomenko et al, 2021).…”

Section: Computationally Expensive Physicsmentioning

confidence: 99%

Modeling of Chromospheric Features and Dynamics in Solar Plage

Danilović¹

2022

Preprint

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The chromosphere is a dynamic and complex layer where all the relevant physical processes happen on very small spatio-temporal scales. A few spectral lines that can be used as chromospheric diagnostics give us convoluted information that is hard to interpret without realistic theoretical models. What are the key ingredients that these models need to contain? The magnetic field has a paramount effect on chromospheric structuring. This is obvious from the ubiquitous presence of chromospheric dynamic fibrilar structures visible on the solar disk and at the limb. The numerical experiments presented in this manuscript illustrate the present state of modeling. They showcase to what extent our models reproduce various chromospheric features and their dynamics. The publication describes the effect different ingredients have on chromospheric models and provides a recipe for building one-to-one models. Combining these models with observations will provide insight into the physical processes that take place in the solar atmosphere.

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“…As waves continue to propagate into the upper solar photosphere and chromosphere, the associated plasma motions encounter the increasing influences of ambipolar and Hall effects. Khomenko et al [26] examine how the ambipolar and Hall terms affect the vorticities seen in three-dimensional simulations of magneto-convection. The authors find that ambipolar diffusion results in a reduction of vorticity in the upper chromosphere, with vortical perturbations being dissipated and converted into thermal energy.…”

Section: Publications In the Special Issuementioning

confidence: 99%

High-resolution wave dynamics in the lower solar atmosphere

Jess

Keys

Stangalini

et al. 2020

Phil. Trans. R. Soc. A.

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The magnetic and convective nature of the Sun’s photosphere provides a unique platform from which generated waves can be modelled, observed and interpreted across a wide breadth of spatial and temporal scales. As oscillations are generated in-situ or emerge through the photospheric layers, the interplay between the rapidly evolving densities, temperatures and magnetic field strengths provides dynamic evolution of the embedded wave modes as they propagate into the tenuous solar chromosphere. A focused science team was assembled to discuss the current challenges faced in wave studies in the lower solar atmosphere, including those related to spectropolarimetry and radiative transfer in the optically thick regions. Following the Theo Murphy international scientific meeting held at Chicheley Hall during February 2020, the scientific team worked collaboratively to produce 15 independent publications for the current Special Issue, which are introduced here. Implications from the current research efforts are discussed in terms of upcoming next-generation observing and high-performance computing facilities. This article is part of the Theo Murphy meeting issue ‘High-resolution wave dynamics in the lower solar atmosphere’.

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Influence of ambipolar and Hall effects on vorticity in three-dimensional simulations of magneto-convection

Cited by 10 publications

References 56 publications

Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun

Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun

Modeling of Chromospheric Features and Dynamics in Solar Plage

High-resolution wave dynamics in the lower solar atmosphere

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