Non-axisymmetric Structure of Accretion Disks in Be/X-ray Binaries

Kimitake Hayasaki (1 , 2) , Atsuo T. Okazaki (3) ((1) Department of Applied Physics , Graduate School of Engineering , Hokkaido University , Sapporo 060-8628 , Japan (2) Centre for Astrophysics , Supercomputing

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Swinburne University of Technology Hawthorn Victoria 3122 Australia (3)Faculty of Engineering Hokkai-Gakuen University Sapporo 062-8625 Japan)

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classification 🌌 astro-ph

keywords accretiondiskaroundspiralstructurebinariesdisksexcited

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The non-axisymmetric structure of accretion disks around the neutron star in Be/X-ray binaries is studied by analyzing the results from three dimensional (3D) Smoothed Particle Hydrodynamics (SPH) simulations. It is found that ram pressure due to the phase-dependent mass transfer from the Be-star disk excites a one-armed, trailing spiral structure in the accretion disk around the neutron star. The spiral wave has a transient nature; it is excited around the periastron, when the material is transferred from the Be disk, and is gradually damped afterwards. It is also found that the orbital phase-dependence of the mass-accretion rate is mainly caused by the inward propagation of the spiral wave excited in the accretion disk.

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Non-axisymmetric Structure of Accretion Disks in Be/X-ray Binaries

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