SPECTROSCOPY OF THE RECURRENT NOVA-V3890 SAGITTARII-18D AFTER THE 1990 OUTBURST

被引：13

作者：

ANUPAMA, GC ^{[1
]}

SETHI, S ^{[1
]}

机构：

[1] BENARAS HINDU UNIV,INST TECHNOL,VARANASI,INDIA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 1994年 / 269卷 / 01期

关键词：

STARS; FUNDAMENTAL PARAMETERS; INDIVIDUAL; V3890; SGR; MASS-LOSS; NOVAE; CATACLYSMIC VARIABLES;

D O I：

10.1093/mnras/269.1.105

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 fine fluxes are used to derive the density, approximately 10(9) cm-3, and the mass of the ejected ionized shell, approximately 10(-7) M.. The temperature and radius estimates for the ionizing source are 3 X 10(5) K and 0.06 R.. A helium abundance of 0.23 is estimated.

引用

页码：105 / 109

页数：5