3D numerical simulations of propagating two-fluid, torsional Alfvén waves and heating of a partially-ionized solar chromosphere
arXiv:2106.10537 · doi:10.1093/mnras/stab1780
Abstract
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 three-dimensional (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.
arXiv comment10 pages, 7 figures
References in corpus (26)
- On the Generation, Propagation, and Reflection of Alfven Waves from the Solar Photosphere to the Distant Heliosphere
- Alfven Waves in the Lower Solar Atmosphere
- Dynamic Fibrils are driven by Magnetoacoustic Shocks
- On-disk counterparts of type II spicules in the Ca II 854.2 nm and Halpha lines
- Partially Ionized Plasmas in Astrophysics
- MHD Waves and Coronal Heating: Unifying Empirical and MHD Turbulence Models
- Alfven Waves in the Solar Atmosphere
- Magnetohydrodynamic waves in solar partially ionized plasmas: two-fluid approach
- On the prevalence of small-scale twist in the solar chromosphere and transition region
- Fluid description of multi-component solar partially ionized plasma
- Collisional dissipation of Alfvén waves in a partially ionised solar chromosphere
- Collisions, magnetization, and transport coefficients in the lower solar atmosphere
- Three-dimensional simulations of solar magneto-convection including effects of partial ionization
- Heating of the partially ionized solar chromosphere by waves in magnetic structures
- The Dynamics of Rapid Redshifted and Blueshifted Excursions in the Solar Halpha line
- Alfvén Wave Heating of the Solar Chromosphere: 1.5D models
- Two-fluid simulations of waves in the solar chromosphere I: numerical code verification
- Magnetoacoustic waves in a partially ionized two-fluid plasma
- Transverse Oscillations in Slender Ca II H Fibrils Observed with Sunrise/SuFI
- Energy transport and heating by torsional Alfvén waves propagating from the photosphere to the corona in the quiet Sun
- Torsional Alfvén waves in solar partially ionized plasma: effects of neutral helium and stratification
- Conditions for Photospherically Driven Alfvenic Oscillations to Heat the Solar Chromosphere by Pedersen Current Dissipation
- Multi-fluid approach to high-frequency waves in plasmas. III. Nonlinear regime and plasma heating
- Two-fluid Modeling of Acoustic Wave Propagation in Gravitationally Stratified Isothermal Media
- Heating of a Quiet Region of the Solar Chromosphere by Ion and Neutral Acoustic Waves
- Two-fluid numerical simulations of the origin of the fast solar wind