Models of Vortices and Spirals in White Dwarf's Accretion Binaries

TL;DR

This paper models the formation and evolution of vortices and spiral structures in accretion disks of white dwarf binary systems using hydrodynamic simulations, highlighting the effects of tidal interactions.

Contribution

It introduces new hydrodynamic models and numerical simulations to explain vortex and spiral structure formation in white dwarf accretion binaries.

Findings

Spiral structures form due to tidal interactions in close binaries.

Vortical configurations develop in the accretion disk zones.

Structure longevity depends on rotation period, density, and velocity.

Abstract

The main aim in the current survey is to suggest models of the development of structures, such as vortices and spirals, in accretion white dwarf's binaries. Numerical methods and simulations are applied on the bases of hydrodynamic analytical considerations. It is suggested in the theoretical model the perturbation's parameters of the accretion flow, which are caused by the influences of the tidal wave over the flux of accretion matter around the secondary star. The results of numerical code application on the disturbed flow reveal an appearing of structure with spiral shape due to the tidal interaction in the close binaries. Our further simulations give the solution, which expresses the formation of vortical configurations in the accretion disc's zone. The evolution of vortices in areas of the flow's interaction is explored using single vortex and composite vortex models. Gas in the disc matter is considered to be compressible and non-ideal. The longevity of all these structures is different and each depends on the time period of the rotation, density and velocity of the accretion matter.