A non-ideal MHD formalism for stability analysis of gyro-gravitating complex astroclouds

In the present work the linear instability excitation dynamics (low-frequency) in a complex, low density, partially ionized gyro-gravitating dust molecular cloud (DMC) is theoretically studied in a non-ideal magnetohydrodynamic (MHD) fluid framework. The planar model consists of electrons, ions, negatively charged dust grains and neutral atoms in an initially local magnetohydrostatic homogeneous equilibrium. The key dynamical realistic factors, such as the Coriolis rotation, viscosity and magnetic field diffusion (ambipolar) are concurrently included. We use a standard technique of plane-wave analysis over the basic governing equations describing the DMC in a coupled integrated form. It reduces the perturbed model into a unique mathematical construct of quartic dispersion relation. The numerical analysis constructed here shows mainly that the compressive tidal force acts as a destabilizing agency both in the viscid and inviscid regimes by enhancing the instability growth. The magnetic field coupled together with the DMC rotation have stabilizing influence. The results investigated here could be useful for seeing the initiation of the formation dynamics of different bounded structures in varied space and astrophysical environments. (author)