Spectroscopy of the recurrent nova V3890 Sagittarii 18 d after the 1990 outburst

Anupama, G. C. ; Sethi, S. (1994) Spectroscopy of the recurrent nova V3890 Sagittarii 18 d after the 1990 outburst Monthly Notices of the Royal Astronomical Society, 269 (1). pp. 105-109. ISSN 0035-8711

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Official URL: http://mnras.oxfordjournals.org/content/269/1/105....

Related URL: http://dx.doi.org/10.1093/mnras/269.1.105

Abstract

The spectrum of the recurrent nova V3890 Sgr, obtained from the Vainu Bappu Observatory 18 d after the 1990 outburst maximum, is presented. The nova was in the coronal line phase. The spectrum is similar to that of the recurrent nova RS Oph. An extinction E(B – V) = 1.1 is derived from the B – V colours, and from Balmer and He I line ratios. From the maximum magnitude-rate-of-decline relations for a nova, M v= – 8.6 mag is estimated, which places the nova at a distance of about 5 kpc. Balmer line fluxes are used to derive the density, ∼ 10 9 cm -3, and the mass of the ejected ionized shell, ∼10 -7 M☉. The temperature and radius estimates for the ionizing source are 3 × 10 5 K and 0.06 R☉. A helium abundance of 0.23 is estimated.

Item Type:Article
Source:Copyright of this article belongs to Oxford University Press.
Keywords:Stars: Fundamental Parameters; Stars: Individual: V3890 Sgr; Stars: Mass-loss; Novae, Cataclysmic Variables
ID Code:100452
Deposited On:10 Dec 2016 13:01
Last Modified:10 Dec 2016 13:01

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