Abstract
Nova Cygni 1978 was observed from October 11 to December 23, 1978 at the Beijing Observatory with the grating spectrograph attached to the Naismith focus of the 60 90- cm Schmidt telescope. This paper gives postmaximum photographic magnitudes, identification of the spectral features, emission line structures, intensity ratios of some emission lines and the temperature of the underlying star. The main spectral lines in wavelength range λλ 3400–6700 A ̊ from October 11 to 30 are those of the following atoms or ions: H, FeII, NII, TiII, [0I], NIII. From November 10, lines of [0III], HeI and Hell become visible one after the other. The emission line H α shows three components of which the most redshifted is the strongest. In turn, each component is split into a number of secondary peaks. Temperature of the underlying star increases with decline of the nova brightness. The upper limit of temperature may be ∼120000 K.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
