The Role of Partial Ionization Effects in the Chromosphere
arXiv:1503.02723 · doi:10.1098/rsta.2014.0268
Abstract
The energy for the coronal heating must be provided from the convection zone. The amount and the method by which this energy is transferred into the corona depends on the properties of the lower atmosphere and the corona itself. We review: 1) how the energy could be built in the lower solar atmosphere; 2) how this energy is transferred through the solar atmosphere; and 3) how the energy is finally dissipated in the chromosphere and/or corona. Any mechanism of energy transport has to deal with the various physical processes in the lower atmosphere. We will focus on a physical process that seems to be highly important in the chromosphere and not deeply studied until recently: the ion-neutral interaction effects (INIE) in the chromosphere. We review the relevance and the role of the partial ionization in the chromosphere and show that this process actually impacts considerably the outer solar atmosphere. We include analysis of our 2.5D radiative MHD simulations with the Bifrost code (Gudiksen et al. 2011) including the partial ionization effects on the chromosphere and corona and thermal conduction along magnetic field lines. The photosphere, chromosphere and transition region are partially ionized and the interaction between ionized particles and neutral particles has important consequences on the magneto-thermodynamics of these layers. The INIE are treated using generalized Ohm's law, i.e., we consider the Hall term and the ambipolar diffusion in the induction equation. The interaction between the different species affects the modeled atmosphere as follows: 1) the ambipolar diffusion dissipates magnetic energy and increases the minimum temperature in the chromosphere; 2) the upper chromosphere may get heated and expanded over a greater range of heights. These processes reveal appreciable differences between the modeled atmospheres of simulations with and without INIE.
25 pages, 3 figures, accepted to be published in Royal Society
References in corpus (31)
- The Solar Optical Telescope for the Hinode Mission: An Overview
- Alfven Waves in the Lower Solar Atmosphere
- Observing the Roots of Solar Coronal Heating - in the Chromosphere
- Dynamic Fibrils are driven by Magnetoacoustic Shocks
- High Resolution Observations and Modeling of Dynamic Fibrils
- Emergence of Small-Scale Magnetic Loops in the Quiet Sun Internetwork
- Evidence of Non-Thermal Particles in Coronal Loops Heated Impulsively by Nanoflares
- Hall magnetohydrodynamics of partially ionized plasmas
- Non-equilibrium hydrogen ionization in 2D simulations of the solar atmosphere
- Emergence of small-scale magnetic loops through the quiet solar atmosphere
- On the prevalence of small-scale twist in the solar chromosphere and transition region
- Twisted flux tube emergence from the convection zone to the corona
- Two components of the coronal emission revealed by EUV spectroscopic observations
- Solar Magnetic Tracking. I. Software Comparison and Recommended Practices
- The Unresolved Fine Structure Resolved - IRIS observations of the Solar Transition Region
- The Solar Internetwork. I. Contribution to the Network Magnetic Flux
- Transient horizontal magnetic fields in solar plage regions
- Dynamics of the Solar Magnetic Network. II. Heating the Magnetized Chromosphere
- Rayleigh-Taylor instability in prominences from numerical simulations including partial ionization effects
- Detailed and simplified non-equilibrium helium ionization in the solar atmosphere
- Twisted flux tube emergence from the convection zone to the corona II: Later states
- Conditions for Photospherically Driven Alfvenic Oscillations to Heat the Solar Chromosphere by Pedersen Current Dissipation
- Rayleigh-Taylor instability in partially ionized compressible plasmas: one fluid approach
- Are Chromospheric Nanoflares a Primary Source of Coronal Plasma?
- Radiating Current Sheets in the Solar Chromosphere
- Study of single-lobed circular polarization profiles in the quiet Sun
- Pervasive Linear Polarization Signals in the Quiet Sun
- Chromospheric magnetic reconnection: Two-fluid simulations of coalescing current loops
- Pair separation of magnetic elements in the quiet Sun
- Detection of supersonic horizontal flows in the solar granulation
- On the Alfven wave cut-off in partly ionized collisional plasmas
Cited by in corpus (22)
- Partially Ionized Plasmas in Astrophysics
- Recent advances in coronal heating
- Three-dimensional Magnetohydrodynamic Simulation of the Formation of Solar Chromospheric Jets with Twisted Magnetic Field Lines
- Two-dimensional Radiative Magnetohydrodynamic Simulations of Partial Ionization in the Chromosphere. II. Dynamics and Energetics of the Low Solar Atmosphere
- The cool surge following flux emergence in a radiation-MHD experiment
- Ion-neutral interactions and non-equilibrium ionization in the solar chromosphere
- Multifluid modeling of magnetosonic wave propagation in the solar chromosphere -- effects of impact ionization and radiative recombination
- Emergence of granular-sized magnetic bubbles through the solar atmosphere. II. Non-LTE chromospheric diagnostics and inversions
- On chromospheric heating during flux emergence in the solar atmosphere
- Nonequilibrium ionization and ambipolar diffusion in solar magnetic flux emergence processes
- On the effects of ion-neutral interactions in solar plasmas
- Chromospheric Heating by MHD Waves and Instabilities
- Ambipolar diffusion in the Bifrost code
- Time Dependent Non-Equilibrium Ionization of Transition Region Lines Observed with IRIS
- Two-fluid simulations of Rayleigh-Taylor instability in a magnetized solar prominence thread II. Effects of collisionality
- Can Hall effect trigger Kelvin-Helmholtz instability in sub-Alfvenic flows?
- Structure of sunspot light bridges in the chromosphere and transition region
- Coronal Properties of Low-mass Population III Stars and the Radiative Feedback in the Early Universe
- The Effect of the Chromospheric Temperature on Coronal Heating
- Multi-fluid Simulation of Solar Chromospheric Turbulence and Heating Due to the Thermal Farley-Buneman Instability
- Future Prospects for Partially Ionised Solar Plasmas: the Prominence Case
- Solar Interior