Acoustic waves in two-fluid solar atmosphere model: cut-off periods, chromospheric cavity, and wave tunnelling

Wójcik, Dariusz; Murawski, K.; Musielak, Z. E.

doi:10.1093/mnras/sty2306

Cited by 27 publications

(31 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

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

Self Cite

View full text Add to dashboard Cite

show abstract

“…The Courant-Friedrichs-Lewy (CFL) number is set to 0.1, a small number in order to obtain a small time step to solve the elliptic term introduced by the thermal conduction, and an adaptive time step. We use the HLLE Riemann solver (Harten et al 1983), the van Leer slope limiter (van Leer 1977), and a third order total variation diminishing Runge-Kutta (Abramowitz & Stegun 1972). The Flux Constrained Transport method (Evans & Hawley 1988;Balsara 2004) is adapted to avoid the growth in time of ∇ • ì .…”

Section: Simulation Box and Boundary Conditionsmentioning

confidence: 99%

“…It is believed that the origin of high temperatures in the corona is of magnetic nature and that the energy source lies in the solar surface plasma motions (Arregui 2015). Several mechanisms have been considered to contribute to the heating like the dissipation of magnetic energy by magnetic reconnection (van Ballegooĳen 1986), current cascades (Parker 1963), viscous turbulence (van Ballegooĳen 1986), magnetic braiding (Peter et al 2004), the dissipation of wave energy (Alfvén 1947;Ionson 1978;Heyvaerts & Priest 1983;Goossens 1991;Hood et al 1997), and the mass flow cycle between the chromosphere and corona (McIntosh et al 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Due to the high energy transported by it, this interesting new phenomenon could make an important contribution to the coronal heating problem. These 2D simulations were performed using the ★ E-mail:ana.navarro1@correo.uis.edu.co JOANNA code (Wójcik et al 2018), solving two fluid equations (for ions + electrons and neutrals) under ideal conditions, that is, without considering non-adiabatic terms. However, in these specific conditions the thermal conduction should be considered because of the steep gradient temperatures in the transition region, and due to the shape of the magnetic field that conducts very efficiently the heat flux along its field lines (Spitzer 1956).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Thermal conduction effects on formation of chromospheric solar tadpole-like jets

Navarro

Lora-Clavijo

Murawski

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We measure the effects of non-isotropic thermal conduction on generation of solar chromospheric jets through numerical simulations carried out with the use of one fluid MHD code MAGNUS. Following the work of Srivastava et al. (2018), we consider the atmospheric state with a realistic temperature model and generate the ejection of plasma through a gas pressure driver operating in the top chromosphere. We consider the magnetic field mimicking a flux tube and perform parametric studies by varying the magnetic field strength and the amplitude of the driver. We find that in the case of thermal conduction the triggered jets exhibit a considerably larger energy and mass fluxes and their shapes are more collimated and penetrate more the solar corona than for the ideal MHD equations. Low magnetic fields allow these jets to be more energetic, and larger magnetic fields decrease the enhancement of mass and energy due to the inclusion of the thermal conductivity.

show abstract

“…Soler et al (2013) studied Alfvén-wave propagation in partially ionized plasma while taking a generalized approach with free parameters with the lower solar atmosphere case as an example. Maneva et al (2017) and Wójcik, Murawski, and Musielak (2018) studied acoustic-wave propagation using a collisional two-fluid approach as well. Three-fluid simulations, with electrons being the third fluid, were carried out to study reconnection events in the chromosphere (Leake, Lukin, and Linton, 2013).…”

Section: Introductionmentioning

confidence: 99%

Time-Dependent Two-Fluid Magnetohydrodynamic Model and Simulation of the Chromosphere

et al. 2019

View full text Add to dashboard Cite

The Sun's chromosphere is a highly dynamic, partially ionized region where spicules (hot jets of plasma) form. Here we present a two-fluid MHD model to study the chromosphere, which includes ion-neutral interaction and frictionalheating. Our simulation recovers a magnetic-canopy shape that forms quickly, but it is also quickly disrupted by the formation of a jet. Our simulation produces a shock self-consistently, where the jet is driven by the frictional-heating, which is much greater than the ohmic-heating. Thus, our simulation demonstrates that the jet could be driven purely by thermal effects due to ion-neutral collisions and not by magnetic reconnection. We plan to improve the model to include photo-chemical effects and radiation.

show abstract

Acoustic waves in two-fluid solar atmosphere model: cut-off periods, chromospheric cavity, and wave tunnelling

Cited by 27 publications

References 26 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

Thermal conduction effects on formation of chromospheric solar tadpole-like jets

Time-Dependent Two-Fluid Magnetohydrodynamic Model and Simulation of the Chromosphere

Contact Info

Product

Resources

About