Abstract
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 the non-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 the magneto-acoustic waves. The non-trivial results explored here match with the prior predictions both as special cases and stimulating corollaries relevant in the bounded astrostructure creation dynamics.
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The authors are extremely thankful to their learned colleagues for extending valuable comments and insightful suggestions. The financial support received through the SERB Project (Grant-EMR/2017/003222) is duly recognised.
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Dutta, P., Karmakar, P.K. Instability dynamics in gyrogravitating astroclouds with cosmic ray moderation in non-ideal MHD fabric. Pramana - J Phys 95, 169 (2021). https://doi.org/10.1007/s12043-021-02199-6
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DOI: https://doi.org/10.1007/s12043-021-02199-6