Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

Wójcik, Dariusz; Kuźma, Błażej; Murawski, K.; Srivastava, A. K.

doi:10.3847/1538-4357/ab26b1

Cited by 21 publications

(20 citation statements)

References 56 publications

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“…To solve the two-fluid equations numerically, we use the JOANNA code (Wójcik et al 2018;Wójcik et al 2019). For the considered problem, we set the Courant-Friedrichs-Lewy number equal to 0.3 and choose the TVDLF approximate Riemann solver (Toro 2009).…”

Section: Numerical Box and Perturbationsmentioning

confidence: 99%

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

Kuźma

Murawski

Poedts

2021

Monthly Notices of the Royal Astronomical Society

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We present a new insight into the propagation, attenuation, and dissipation of two-fluid, torsional Alfvén waves in the context of heating of the lower solar atmosphere. By means of numerical simulations of the partially ionized plasma, we solve the set of two-fluid equations for ion plus electron and neutral fluids in 3D Cartesian geometry. We implement initially a current-free magnetic field configuration, corresponding to a magnetic flux-tube that is rooted in the solar photosphere and expands into the chromosphere and corona. We put the lower boundary of our simulation region in the low chromosphere, where ions and neutrals begin to decouple, and implement there a monochromatic driver that directly generates Alfvén waves with a wave period of 30 s. As the ion-neutral drift increases with height, the two-fluid effects become more significant and the energy carried by both Alfvén and magneto-acoustic waves can be thermalized in the process of ion–neutral collisions there. In fact, we observe a significant increase in plasma temperature along the magnetic flux-tube. In conclusion, the two-fluid torsional Alfvén waves can potentially play a role in the heating of the solar chromosphere.

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Section: Numerical Box and Perturbationsmentioning

confidence: 99%

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

Kuźma

Murawski

Poedts

2021

Monthly Notices of the Royal Astronomical Society

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“…For instance, Tu et al (2005) found these outflows in coronal funnels at altitudes between 5 and 20 Mm above the photosphere. Later, the problem was reconsidered by Wójcik et al (2019) who proposed that jets and associated plasma outflows, generated by the solar granulation, may higher up result in the formation of the solar wind. Moving upwardly, the plasma requires a source of momentum which can be provided by MHD waves (Ofman 2005;Marsch 2006;De Pontieu et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Chromospheric heating and generation of plasma outflows by impulsively generated two-fluid magnetoacoustic waves

Niedziela

Murawski

Poedts

2021

A&A

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Context. The origin of the heating of the solar atmosphere is still an unsolved problem. As the photosphere and chromosphere radiate more energy than the solar corona it is challenging but important to reveal all the mechanisms that contribute to plasma heating there. Ion-neutral collisions could play an important role. Aims. Impulsively generated two-fluid magnetoacoustic waves are investigated in the partially ionized solar chromosphere and the associated heating and plasma outflows are studied, which higher up may result in nascent solar wind. Methods. To describe the plasma dynamics, a two-fluid model is applied in which ions+electrons and neutrals are treated as separate fluids. The two-fluid equations are solved numerically using the JOANNA code. Results. We show that magnetoacoustic waves, triggered in the photosphere by localised velocity pulses, can steepen into shocks which heat the chromosphere through ion-neutral collisions. Larger amplitude and wider pulses more effectively heat plasma and generate larger plasma outflows. Rising the altitude at which the pulse is launched, results in opposite effects, mainly in local cooling of the chromosphere, and slower plasma outflows. Conclusions. Even a solitary pulse results in a train of waves. These waves can transform to shock waves and release thermal energy, heating the chromosphere significantly. A pulse can drive vertical flows which higher up can result in the origin of the solar wind.

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“…How do these contribute to the fast component of the solar wind at higher altitudes? Despite significant observational and theoretical developments over two decades on magnetic waves, shocks, instabilities, and formation of the jets/flows, their respective roles or inter-relationships in a variety of chromospheric magnetic structures are not yet fully understood (e.g., Kudoh and Shibata 1999;De Pontieu et al 2004;Shibata et al 2007;Nishizuka et al 2011;Iijima and Yokoyama 2015;Zhelyazkov et al 2015;Brady and Arber 2016;Kuźma et al 2017;Kayshap et al 2018b;Mishra and Srivastava 2019;Wójcik et al 2019;Wang and Yokoyama 2020;Zaqarashvili et al 2020).…”

Section: Mhd Instabilities In the Chromospheric Plasmamentioning

confidence: 99%

Chromospheric Heating by Magnetohydrodynamic Waves and Instabilities

et al. 2021

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The importance of the chromosphere in the mass and energy transport within the solar atmosphere is now widely recognised. This review discusses the physics of magnetohydrodynamic (MHD) waves and instabilities in large-scale chromospheric structures as well as in magnetic flux tubes. We highlight a number of key observational aspects that have helped our understanding of the role of the solar chromosphere in various dynamic processes and wave phenomena, and the heating scenario of the solar chromosphere is also discussed. The review focuses on the physics of waves and invokes the basics of plasma instabilities in the context of this important layer of the solar atmosphere. Potential implications, future trends and outstanding questions are also delineated.

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Two-fluid Numerical Simulations of the Origin of the Fast Solar Wind

Cited by 21 publications

References 56 publications

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

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

Chromospheric heating and generation of plasma outflows by impulsively generated two-fluid magnetoacoustic waves

Chromospheric Heating by Magnetohydrodynamic Waves and Instabilities

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