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Shaping of Nova Shells by Binary Motion

Published online by Cambridge University Press:  12 April 2016

H. M. Lloyd ,
T. J. O’Brien  and
M. F. Bode
H. M. Lloyd
Affiliation:
Astrophysics Group, Liverpool John Moores University, Byrom Street, Liverpool L3 3AF, UK
T. J. O’Brien
Affiliation:
Astrophysics Group, Liverpool John Moores University, Byrom Street, Liverpool L3 3AF, UK
M. F. Bode
Affiliation:
Astrophysics Group, Liverpool John Moores University, Byrom Street, Liverpool L3 3AF, UK

Abstract

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Several years after outburst, extended optical emission can be seen around many classical novae. Common features include shells, polar ‘blobs’, equatorial rings and, at least in the case of DQ Her (1934), tropical rings above and below the ‘equator’. We present hydrodynamic calculations of the dynamical effects of the underlying binary system on the material ejected during outburst, and show that many of the features observed in the optical remnants of novae can be reproduced. Polar blobs, banded shells and spherical shells can all be obtained in the model, depending on the speed class of the nova.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 313 - 314
Copyright
Copyright © Kluwer 1996

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