Simulation of the boundary layer in accretion disks with the SPH method

Details Simulation of the boundary layer in accretion disks with the SPH method Simulation of the boundary layer in accretion disks with the SPH method

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296..537m&link_type=abstract

In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 1: X Ray Binaries p 537-540 (SEE N90-25711 19-89)

Statistics

Computation

Accretion Disks, Computerized Simulation, Stellar Mass Accretion, Three Dimensional Boundary Layer, Turbulent Boundary Layer, Computational Fluid Dynamics, Hydrodynamics, Star Formation, Stellar Envelopes, Stellar Models, X Ray Astronomy

Scientific paper

The boundary layer between the accretion disk formed by gas falling onto a compact star is considered. The description of the structure of the region of transition from highly supersonic to subsonic motion is investigated. Numerical solutions to understand the physical processes operating in this region are presented. The Smoothed Particle Hydrodynamics (SPH) method is used to integrate the equations of the gas and radiation. Radiation is treated in the flux limited diffusion approximation. Simulations of the 3-D motion of the gas are presented.

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