Numerical simulation of accretion discs in close binary systems and discovery of spiral shocks

Abstract

The history of hydrodynamic numerical simulations for accretion disks in close binary systems is reviewed, in which emphasis is placed, in particular, on the facts that spiral shock waves were numerically found in 1986 by researchers including one of the present authors and that spiral structure was discovered in IP Pegasi in 1997 by Steeghs et al. The results of our two and three-dimensional numerical simulations in recent years are then summarized, with comparison being made with observations.

16 pages, LaTeX with 14 eps figures using kluwer.cls. Submitted to Astrophysics and Space Science

References in corpus (4)

• 3D numerical simulation of gaseous flows structure in semidetached binaries
• Three-dimensional Modeling of the Matter Flow Structure in Semidetached Binary Systems
• Spiral Structure in IP Peg: Confronting Theory and Observations
• 3D Finite Volume Simulation of Accretion Discs with Spiral Shocks

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• Variable Star Network: World Center for Transient Object Astronomy and Variable Stars
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• Optical spectroscopy of the dwarf nova U Geminorum
• Formation of the Asymmetric Accretion Disk from Stellar Wind Accretion in an S-type Symbiotic Star
• Numerical simulation of the surface flow of a companion star in a close binary system
• Numerical Simulation of Interaction between an L1 Stream and an Accretion Disk in a Close Binary System
• Numerical Simulation of the Surface Flow on the Companion Star in a Close Binary System II. Construction of Doppler maps and application to Galactic supersoft X-ray sources