Hydrodynamical and radiative modeling of temporal H{\alpha} emission V/R variations caused by a discontinuous mass transfer in binaries

TL;DR

This study models the Hα emission V/R variations in interacting binaries caused by discontinuous mass transfer, using 3D hydrodynamical simulations and radiative transfer calculations to understand the formation and evolution of gaseous disks.

Contribution

First qualitative modeling of Hα V/R variations due to discontinuous mass transfer in binaries using combined hydrodynamical and radiative transfer simulations.

Findings

Formation of elongated gaseous disks with prograde revolution.

Hα profiles show double emission with V/R and radial velocity variations.

Variations are likely temporary, fading with disk circularization.

Abstract

H{\alpha} emission V/R variations caused by a discontinous mass transfer in interacting binaries with a rapidly rotating accreting star are modelled qualititatively for the first time. The program ZEUS-MP was used for a non-linear 3-D hydrodynamical modeling of a development of a blob of gaseous material injected into an orbit around a star. It resulted in the formation of an elongated disk with a slow prograde revolution. The LTE radiative transfer program SHELLSPEC was used to calculate the H{\alpha} profiles originating in the disk for several phases of its revolution. The profiles have the form of a double emission and exhibit V/R and radial velocity variations. However, these variations should be a temporal phenomenon since imposing a viscosity in given model would lead to a circularization of the disk and fading-out of given variations.