Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008pasj...60..259l&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.60, No.2, pp.259--266
Astronomy and Astrophysics
Astronomy
7
Accretion, Accretion Discs, Hydrodynamics, Methods: Numerical, Stars: Binaries: Close, Dwarf Novae, Cataclysmic Variables
Scientific paper
In this work, the roles of both the inflow kinematic conditions at the inner Lagrangian point L1 as an initial boundary condition and the gas compressibility, physical turbulent viscosity on an accretion disc's dynamics and structure were investigated via simulations of 3D SPH stationary accretion-disc models. Physical viscosity supports accretion-disc development inside the primary gravitational potential well in a close binary system, even for low-compressibility modelling. Currently, an assigned typical turbulent Shakura-Sunyaev parameter, α ≃ 0.1, is widely adopted for these structures. Such an investigation was carried out here with the aim of evaluating, in a compressibility-viscosity graph, the most suitable domains where the physical conditions allow a well-bound disc development as a function of the mass-transfer kinematic conditions. Physical, turbulent viscosity is represented by a viscous force contribution, expressed by the divergence of the symmetric viscous stress tensor in the Navier-Stokes equation, while the viscous energy contribution is given by a symmetric combination of the symmetric shear tensor multiplied by the particle velocity. The same binary system parameters-stellar masses and their separation- were adopted throughout, whilst the adopted polytropic index, γ, is chosen to be in the range between 1-(5/3). The results show that in such domains, the lower is the gas compressibility (the higher the polytropic index γ), the higher is the physical viscosity (α) requested. Conclusions, as far as dwarf nova outbursts are concerned, induced by mass-transfer rate variations are also reported.
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