Gravitational instability in partially ionized plasmas: A two-fluid approach

Abstract

We propose a new two-fluid model for a partially ionized magnetoplasma under gravity, where electrons and neutrals are treated as a single fluid, and singly charged positive ions are a separate fluid. We observe that the classical result of gravitational instability (also known as Rayleigh-Taylor instability) in fully ionized plasmas is significantly modified by the influence of ion-neutral collisions (with frequency $ν_{\rm{in}}$) and transverse wave numbers ($k_x$ and $k_y$). The instability growth rate can be enhanced or decreased depending on the values of the ratios $κ\equiv k_x/k_y$ and $f\equivν_{\rm{in}}/Ω_{\rm{ci}}$, where $Ω_{\rm{ci}}$ is the ion-cyclotron frequency. We also estimate the growth rates relevant to the ionospheric E-region and solar atmosphere, noting that such growth rates can be maximized for $κ,~f\ll1$, or for $κ>1$ and $f\sim0.64$, and minimized for $f\gg1$ irrespective of the value of $κ$. Furthermore, the timescale of instability ranges from $1$ minute to $2$ minutes in the solar atmosphere, while in the E region, it ranges from $1$ minute to $80$ minutes. The latter can be a satisfactory result for the reported lifetime of solar prominence threads.

Figures (1)

• Figure 1: The normalized growth rate of instability ($\gamma/\omega_g$) is shown against the frequency ratio $f\equiv\nu_{\rm{in}}/\Omega_{\rm{ci}}$ for different values of the wave-number ratio, $\kappa\equiv k_x/k_y$ as in the legends.