The evolutionary instability dynamics, which is naturally excitable in an astrophysical complex gyrogravitating partially ionised molecular cloud in a magnetic field, is herein semianalytically investigated. It is rooted in a non-ideal classical non-relativistic magnetohydrodynamic (MHD) mean-fluidic model fabric. The effects of fluid kinematic viscosity, cosmic rays and tidal force field are concurrently included. Application of a standard normal mode analysis reduces the astrocloud into a unique generalised linear quartic dispersion relation having atypical variable coefficients. A numerical illustrative analysis shows that the instability is noticeably damped (grown) in the viscous (inviscid) domains. The magnetic field and rotation have stabilising influences against thenon-local self-gravity. In contrast, the cosmic ray pressure and tidal interaction destabilise the cloud along its self-gravity. We see that the ambipolar diffusion is the only non-ideal MHD factor with significant stimulus on themagneto-acoustic waves. The non-trivial results explored herematch with the prior predictions both as special cases and stimulating corollaries relevant in the bounded astrostructure creation dynamics.
Volume 96, 2022
Continuous Article Publishing mode
Click here for Editorial Note on CAP Mode