The ejecta of classical novae

Details The ejecta of classical novae The ejecta of classical novae

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..260o&link_type=abstract

Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at

Physics

Scientific paper

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 up to 10-4 Modot at hundreds to thousands of kilometres per second. The expanding shell can typically be resolved a few months after outburst using high-resolution imaging at radio or optical wavelengths. Old nova shells remain visible years after outburst as they are bathed in the photoionizing radiation field of the central system containing the hot white dwarf with its re-established accretion disc. Recent Hubble Space Telescope and MERLIN imaging of the expanding ejecta from several classical novae will be 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 will be discussed.

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