Spectroscopy of the Recurrent Nova V3890-SAGITTARII 18-DAYS after the 1990 Outburst

Details Spectroscopy of the Recurrent Nova V3890-SAGITTARII 18-DAYS after the 1990 Outburst Spectroscopy of the Recurrent Nova V3890-SAGITTARII 18-DAYS after the 1990 Outburst

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.269..105a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 269, NO. 1/JUL1, P. 105, 1994

Astronomy and Astrophysics

Astronomy

10

Stars: Fundamental Parameters - Stars: Individual: V3890 Sgr - Stars: Mass-Loss - Novae, Cataclysmic Variables

Scientific paper

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, MV = -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, ˜109 cm-3, and the mass of the ejected ionized shell, ˜10-7 Msun. The temperature and radius estimates for the ionizing source are 3 × 105 K and 0.06 Rsun. A helium abundance of 0.23 is estimated.

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