The structure of cool accretion disc in semidetached binaries

Abstract

We present the results of qualitative consideration of possible changes occurring during the transition from the hot accretion disc to the cool one. We argue the possible existence of one more type of spiral density waves in the inner part of the disc where gasdynamical perturbations are negligible. The mechanism of formation of such a wave as well as its parameters are considered. We also present the results of 3D gasdynamical simulation of cool accretion discs. These results confirm the hypothesis of possible formation of the spiral wave of a new, "precessional" type in the inner regions of the disc. Possible observational manifestations of this wave are discussed.

arXiv commentLaTeX, 16 pages, 8 figures, to be published in Astron. Zh

References in corpus (1)

• 3D numerical simulation of gaseous flows structure in semidetached binaries

Cited by in corpus (8)

• Spiral patterns in planetesimal circumbinary disks
• Earth, Moon, Sun, and CV Accretion Disks
• Numerical Simulations of Naturally Tilted, Retrogradely Precessing, Nodal Superhumping Accretion Disks
• Full 3-D MHD calculations of accretion flow Structure in magnetic cataclysmic variable stars with strong and complex magnetic fields
• On the possible turbulence mechanism in accretion disks in non-magnetic binary stars
• Investigating lack of accretion disk eccentricity growth in a global 3D MHD simulation of a superhump system
• Point-wise Self-similar Solution for Spiral Shocks in Accretion Disk with Mass Outflow in Binary
• Accretion Discs with an Inner Spiral Density Wave