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The Ejecta of Classical Novae

Published online by Cambridge University Press:  13 May 2016

T.J. O'Brien ,
R.J. Davis ,
M.F. Bode ,
S. P. S. Eyres  and
J.M. Porter
T.J. O'Brien
Affiliation:
Jodrell Bank Observatory, The University of Manchester, Macclesfield, SK11 9DL, UK
R.J. Davis
Affiliation:
Jodrell Bank Observatory, The University of Manchester, Macclesfield, SK11 9DL, UK
M.F. Bode
Affiliation:
Astrophysics Research Institute, Liverpool JMU, Birkenhead, CH41 1LD, UK
S. P. S. Eyres
Affiliation:
Astrophysics Research Institute, Liverpool JMU, Birkenhead, CH41 1LD, UK
J.M. Porter
Affiliation:
Astrophysics Research Institute, Liverpool JMU, Birkenhead, CH41 1LD, UK

Abstract

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Classical novae are interacting binary stars in which a thermonuclear runaway in material accreted onto a white dwarf from a companion red dwarf results in the ejection of around 10−4M⊙ at hundreds to thousands of kilometres per second. Recent Hubble Space Telescope and MERLIN imaging of the expanding ejecta from several classical novae are presented. In general the ejecta are clumpy but often display coherent structures, most notably equatorial rings of enhanced emission encircling prolate ellipsoidal shells. Physical mechanisms (including the common envelope phase and anisotropic irradiation of the shell) which may result in the generation of these structures are discussed.

Type
Star Formation Regions and Outflow Processes in our Galaxy
Information
Symposium - International Astronomical Union , Volume 205: Galaxies and their Constituents at the Highest Angular Resolutions , 2001 , pp. 260 - 263
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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