The nebular remnant and quiescent spectrum of Nova GK Persei

Anupama, G. C. ; Prabhu, T. P. (1993) The nebular remnant and quiescent spectrum of Nova GK Persei Monthly Notices of the Royal Astronomical Society, 263 (2). pp. 335-342. ISSN 0035-8711

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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 II] 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 M☉ 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 R☉, which are consistent with its being a white dwarf.

Item Type:Article
Source:Copyright of this article belongs to Oxford University Press.
Keywords:Accretion, Accretion Discs; Circumstellar Matter; Stars: Individual: GK Per; Novae, Cataclysmic Variables; White Dwarfs
ID Code:100448
Deposited On:10 Dec 2016 13:01
Last Modified:10 Dec 2016 13:01

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