The Nebular Remnant and Quiescent Spectrum of Nova Gk-Persei

Details The Nebular Remnant and Quiescent Spectrum of Nova Gk-Persei The Nebular Remnant and Quiescent Spectrum of Nova Gk-Persei

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.263..335a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 263, NO.2/JUL15, P. 335, 1993

Astronomy and Astrophysics

Astronomy

11

Accretion, Accretion Discs - Circumstellar Matter - Stars: Individual: Gk Per - Novae, Cataclysmic Variables - White Dwarfs

Scientific paper

CCD images of the nebular shell of the old nova GK Per in [N II] and [O III] emission lines, and also the quiescent spectrum in the optical region, are presented. Proper motion measurements of the knots in [N III] over the baseline 1984-90 give a mean expansion rate of 0.31±0.07 arcsec yr-1. This value agrees with models of the expansion of the ejecta into the ambient circumstellar medium. A correction for projection effects indicates that the ratio of the mass of the shell to the density of the circumstellar medium is a factor of 2-3 higher than estimated previously. The optical spectrum is decomposed into those of the secondary and the accretion disc. The estimate of Mv= +4.9 for the accretion disc implies a mass transfer rate of 3.5 × 10-9 Msun yr-1 in the steady state. The H and He emission-line fluxes are used to infer that (i) the line-emitting region has a high density, (ii) the He/H abundance is near-solar, and (iii) the ionizing source has a Zanstra temperature of 1.3 × 105 K and an effective radius of 0.01 Rsun, which are consistent with its being a white dwarf.

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