Rayleigh-Taylor instability of a finitely conducting partially ionized Hall plasma

Khan, Aiyub; Bhatia, P. K.

doi:10.1088/0031-8949/48/5/017

Cited by 4 publications

(4 citation statements)

References 8 publications

(4 reference statements)

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“…While they are predicted to occur within h0 of the surface, we do not observe them in these simulations. Resistive ballooning (Velli & Hood, 1986) and resistive Rayleigh-Taylor modes (Khan & Bhatia, 1993) are not considered by virtue of our restriction to ideal MHD, but they are known to be common in distorted axisymmetric equilibria similar to those in Figure 1(a). These instabilities can allow plasma slippage faster than Ohmic diffusion, but slower than the Alfven time.…”

Section: Instabilities In Three Dimensionsmentioning

confidence: 99%

Burial of the polar magnetic field of an accreting neutron star – II. Hydromagnetic stability of axisymmetric equilibria

Payne

Melatos

2007

Monthly Notices of the Royal Astronomical Society

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The theory of polar magnetic burial in accreting neutron stars predicts that a mountain of accreted material accumulates at the magnetic poles of the star, and that, as the mountain spreads equatorward, it is confined by, and compresses, the equatorial magnetic field. Here, we extend previous, axisymmetric, Grad-Shafranov calculations of the hydromagnetic structure of a magnetic mountain up to accreted masses as high as M a = 6 × 10 −4 M , by importing the output from previous calculations (which were limited by numerical problems and the formation of closed bubbles to M a < 10 −4 M ) into the time-dependent, ideal-magnetohydrodynamic code ZEUS-3D and loading additional mass on to the star dynamically. The rise of buoyant magnetic bubbles through the accreted layer is observed in these experiments. We also investigate the stability of the resulting hydromagnetic equilibria by perturbing them in ZEUS-3D. Surprisingly, it is observed that the equilibria are marginally stable for all M a 6 × 10 −4 M ; the mountain oscillates persistently when perturbed, in a combination of Alfvén and acoustic modes, without appreciable damping or growth, and is therefore not disrupted (apart from a transient Parker instability initially, which expels <1 per cent of the mass and magnetic flux).

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Section: Instabilities In Three Dimensionsmentioning

confidence: 99%

Burial of the polar magnetic field of an accreting neutron star – II. Hydromagnetic stability of axisymmetric equilibria

Payne

Melatos

2007

Monthly Notices of the Royal Astronomical Society

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“…More recently Ali and Bhatia [17] have studied the effects of Hall currents, finite conductivity in partially ionized plasma in an oblique magnetic field. Khan and Bhatia [18] considered the effects of finite resistivity and collisions with neutrals on the Rayleigh-Taylor instability of stratified plasma.…”

Section: Introductionmentioning

confidence: 99%

Gravitational instability of partially-ionized plasma in an oblique magnetic field

Bhatia

Hazarika

1995

Phys. Scr.

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cloud where the plasma are frequently not fully-ionized but may instead be partially-ionized so that the interactionThe gravitational instability of an infinitely extending homogenous partially-ionized plasma permeated by an oblique magnetic field has been between the ionized fluid and the neutral gas becomes investigated here in the presence of the effects of Hall currents, magnetic important. The importance of such collisions between resistivity and ion viscosity. The dispersion relation has been obtained and numerical calculations have been performed to obtain the dependence of the growth rate of the gravitationally unstable mode on the various physical effects. It is found that Jeans' criterion remains unchanged. The Hall currents and finite conductivity and collisions with neutrals are all found to have a destabilizing influence on the unstable mode of wave propagation of a gravitational instability of partially-ionized plasma. Ion viscosity is, however, found to have a stabilizing effect.

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“…The effects of horizontal magnetic field, Hall currents and viscosity have been studied on the RTI of an incompressible infinitely conducting stratified plasma by Ahsan and Bhatia [14]. The effect of horizontal magnetic field of Hall currents have been investigated on the RTI of a finitely conducting stratified partially ionized plasma by Aiyub and Bhatia [15]. The instability of stratified plasmas in the presence of horizontal magnetic field of incompressible plasmas with the effect of a transverse velocity shear was studied by Wu et al [16].…”

Section: Introductionmentioning

confidence: 99%

Rayleigh-Taylor Instability in Magnetized Plasma

Hoshoudy¹

2014

WJM

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The Rayleigh-Taylor instability in stratified plasma has been investigated in the presence of combined effect of horizontal and vertical magnetic field. The linear growth rate has been derived for the case where plasma with exponential density distribution is confined between two rigid planes by solving the linear MHD equations into normal mode. Some special cases have been particularized to explain the roles the variables of the problem play; numerical solutions have been made and some stability diagrams are plotted and discussed. The results show that, the growth rate depends on the horizontal and vertical components of magnetic field and also depends on the parameter λ λ

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Rayleigh-Taylor instability of a finitely conducting partially ionized Hall plasma

Cited by 4 publications

References 8 publications

Burial of the polar magnetic field of an accreting neutron star – II. Hydromagnetic stability of axisymmetric equilibria

Burial of the polar magnetic field of an accreting neutron star – II. Hydromagnetic stability of axisymmetric equilibria

Gravitational instability of partially-ionized plasma in an oblique magnetic field

Rayleigh-Taylor Instability in Magnetized Plasma

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