Rayleigh-Taylor instability in magnetized and rotating radiative viscoelastic quantum fluids

¹ Department of Mathematics, Siksha Bhavana, Visva-Bharati University - Santiniketan-731 235, West Bengal, India
² School of Physical Sciences, Jawaharlal Nehru University - New Delhi-110 067, India

Received: 12 February 2025
Accepted: 13 August 2025

Abstract

The linear Rayleigh-Taylor (R-T) instability and the propagation of the internal waves are analytically studied in ultra-relativistic degenerate viscoelastic quantum fluids. A generalized hydrodynamic fluid model is considered composed of strongly coupled non-degenerate ions and weakly coupled ultra-relativistic degenerate electrons with their radiation effects in the presence of a uniform magnetic field and vertically downward gravity. The impact of quantum corrections and the fluid rotation is included in the momentum transport equation in terms of the Bohm potential and the Coriolis force. A generalized dispersion relation is derived using the normal mode method and discussed for two different cases of interest, namely hydrodynamic and kinetic regimes. The numerical investigation reveals that the thermal radiation of the ultra-relativistic degenerate electrons, quantum correction, and compressible viscoelastic speed significantly suppress the onset of R-T instability in the medium. In contrast, the high-strength magnetic field strongly supports the excitation of R-T instability in the configuration. The rotation of the fluid remarkably reduces the instability growth rate without modifying the instability criterion. The outcomes are useful for understanding the R-T instability excitation and internal wave propagation in different dense astrophysical plasma environments, such as the core of white dwarfs.