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On the nature of superoutbursts in dwarf novae

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posted on 2009-12-08, 16:24 authored by M. R. Truss, J. R. Murray, Graham A. Wynn
We present the first detailed hydrodynamic simulation of a superoutburst to incorporate the full tidal potential of a binary system. A two-dimensional smoothed particle hydrodynamics code is used to simulate a superoutburst in a binary with the parameters of the SU UMa system Z Chamaeleontis. The simulated light curves shows all the features observed in such systems. Analysis of the mass flux through the disc and the growth rate of the superhumps and disc eccentricity show that the superoutburst–superhump phenomenon is a direct result of tidal instability. No enhanced mass transfer from the secondary is required to initiate or sustain these phenomena. Comparisons of superoutbursts with normal outbursts are made and we show that the model can be reconciled with the behaviour of U Geminorum-type dwarf novae, which show no superoutbursts.

History

Citation

Monthly Notices of the Royal Astronomical Society, 2001, 324 (1), pp. 1-5

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP) on behalf of Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Copyright date

2001

Available date

2009-12-08

Publisher version

http://mnras.oxfordjournals.org/content/324/1/L1

Notes

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2001 Royal Astronomical Society Published by Oxford University Press [on behalf of Royal Astronomical Society]. All rights reserved.

Language

en

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