Partially Ionized Plasmas in Astrophysics

Ballester, J. L.; Alexeev, I. I.; Collados, M.; Downes, T. P.; Pfaff, R. F.; Gilbert, H. R.; Khodachenko, M. L.; Khomenko, E.; Шайхисламов, И. Ф.; Soler, Roberto; Vázquez‐Semadeni, Enrique; Zaqarashvili, T. V.

doi:10.1007/s11214-018-0485-6

Cited by 134 publications

(121 citation statements)

References 471 publications

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“…That property gives the Boltzmann equation an excellent advantage and various modern applications rather than the Navier-Stokes equations [12,13]. Many papers were dealing with Boltzmann kinetic equation and its applications in many critical physical situations such as heat transfer between two parallel plates [14,15], shock waves [16], irreversible thermodynamics [17], sound propagation in a rarefied gases [18], oscillatory flow [19,20], thermal radiation [21][22][23], plasma [24], and other various amazing applications [25][26][27].…”

Section: Figmentioning

confidence: 99%

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Thermodynamic and kinetic investigation of the influence of external centrifugal field and the heat transfer on a confined neutral gas

Wahid

Elmalky

2020

SN Appl. Sci.

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In the present paper, we offer a new model studying the influence of an external centrifugal field and the heat transfer on a neutral gas confined between two parallel horizontal rigid stationary plane plates. The system of nonlinear differential equations is solved analytically. The temperature and concentration are calculated with a broad range of Knudsen numbers, centrifugal Mach number, and temperatures ratio parameter. We utilized the moment method with suitable boundary conditions. Thermodynamic predictions and internal energy change are examined. Results are applied for laboratory argon gas. Three-dimensional, two-dimensional, and contour plots graphics are drawn, and their manner is discussed.

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Section: Figmentioning

confidence: 99%

“…The constants values for 1 , 2 , and 3 can be calculated using the boundary conditions that have the nondimensional forms: Solving the algebraic system of Eqs. (24)(25)(26)(27), we acquire Substituting Eq. (28) into Eq.…”

Section: Basic Equations and Analytical Solution Proceduresmentioning

confidence: 99%

Thermodynamic and kinetic investigation of the influence of external centrifugal field and the heat transfer on a confined neutral gas

Wahid

Elmalky

2020

SN Appl. Sci.

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“…In this regime, there is a drift in the velocity between ions and neutrals because of the different forces the different species feel 8,9 . These physical processes are found to be important in a wide range of astrophysical plasmas 10 .…”

Section: Introductionmentioning

confidence: 99%

Ion-neutral decoupling in the nonlinear Kelvin–Helmholtz instability: Case of field-aligned flow

Hillier

2019

Physics of Plasmas

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The nonlinear magnetic Kelvin-Helmholtz instability (KHi), and the turbulence it creates, appears in many astrophysical systems. This includes those systems where the local plasma conditions are such that the plasma is not fully ionised, for example in the lower solar atmosphere and molecular clouds. In a partially ionised system, the fluids couple via collisions which occur at characteristic frequencies, therefore neutral and plasma species become decoupled for sufficiently high-frequency dynamics. Here we present high-resolution 2D two-fluid simulations of the nonlinear KHi for a system that traverses the dynamic scales between decoupled fluids and coupled dynamics. We discover some interesting phenomena, including the presence of a density coupling that is independent of the velocity coupling. Using these simulations we analyse the heating rate, and two regimes appear. The first is a regime where the neutral flow is decoupled from the magnetic field that is characterised with a constant heating rate, then at larger scales the strong coupling approximation holds and the heating rate. At large scales with the KHi layer width to the −2 power. There is an energy cascade in the simulation, but the nature of the frictional heating means the heating rate is determined by the largest scale of the turbulent motions, a fact that has consequences for understanding turbulent dissipation in multi-fluid systems.

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“…A gravity vector is g = [0, −g, 0] with its magnitude g = 274.78 m s −2 , α c is the coefficient of collisions between ion and neutral particles (e.g. Oliver et al 2016;Ballester et al 2018, and references cited therein), Q i R radiative losses term which is implemented here in the framework of Abbett & Fisher (2012) in the low atmospheric regions and of thin radiation (Moore & Fung 1972) in the top atmospheric layers, q i,n are thermal conduction terms (Spitzer 1962), µ i = 0.29 and µ n = 1.21 are the mean masses of respectively ions and neutrals, which are taken from the OPAL solar abundance model (e.g. Vögler et al 2004), m H is the hydrogen mass, k B is the Boltzmann constant, γ = 1.4 is the specific heats ratio, and µ is magnetic permeability of the medium.…”

Section: Two-fluid Model Of a Partially-ionized Coronal Holementioning

confidence: 99%

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

Wójcik

Kuźma

Murawski

et al. 2019

ApJ

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With the use of our JOANNA code, which solves radiative equations for ion + electron and neutral fluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solar granulation. These outflows exhibit physical quantities consistent to the order of magnitude with the observational findings for mass and energy losses in the upper chromosphere, transition region and inner corona, and they may originate the fast solar wind.

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Partially Ionized Plasmas in Astrophysics

Cited by 134 publications

References 471 publications

Thermodynamic and kinetic investigation of the influence of external centrifugal field and the heat transfer on a confined neutral gas

Thermodynamic and kinetic investigation of the influence of external centrifugal field and the heat transfer on a confined neutral gas

Ion-neutral decoupling in the nonlinear Kelvin–Helmholtz instability: Case of field-aligned flow

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

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