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SPH Simulations of Accretion Disks and Narrow Rings

Published online by Cambridge University Press:  25 April 2016

Sarah T. Maddison ,
James R. Murray  and
Joe J. Monaghan
Sarah T. Maddison
Affiliation:
Mathematics Department, Monash University, Clayton, Vic. 3168, Australia. maddison@hypatia.maths.monash.edu.au
James R. Murray
Affiliation:
CITA, University of Toronto, Ontario, M5S 1A7, Canada
Joe J. Monaghan
Affiliation:
Mathematics Department, Monash University, Clayton, Vic. 3168, Australia. maddison@hypatia.maths.monash.edu.au
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Abstract

We model a massless viscous disk using smoothed particle hydrodynamics (SPH) and note that it evolves according to the Lynden-Bell & Pringle (1974) theory until a non-axisymmetric instability develops at the inner edge of the disk. This instability may have the same origin as the instability of initially axisymmetric viscous disks discussed by Lyubarskij, Postnov & Prokhorov (1994). To clarify the evolution we evolved single and double rings of particles. It is actually inconsistent with the SPH scheme to set up a single ring as an initial condition because SPH assumes a smoothed initial state. As would be expected from an SPH simulation, the ring rapidly breaks up into a band. We analyse the stability of the ring and show that the predictions are confirmed by the simulation.

Keywords

methods: numericalhydrodynamicsinstabilitiesaccretion: accretion disks
Type
Magnetic Fields, Disks and Jets: A Workshop organised by the ANU Astrophysical Theory Centre The ANU Astrophysical Theory Centre
Information
Publications of the Astronomical Society of Australia , Volume 13 , Issue 1 , January 1996 , pp. 66 - 70
Copyright
Copyright © Astronomical Society of Australia 1996

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References

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