【摘要】 本文给出新星极大后的照相星等m_og光谱成份、发射带结构、发射带相对强度比和核星温度。由10月11日至30日在3500—6700波长范围内它的主要光谱成份为H,FeII,NIITiII,[OI],[NII],NIII。从11月10日开始,陆续出现[OIII],HeI和HeII等谱线。H_a发射带由3个子峰构成,红移最大的子峰强度最大,每个子峰又各分成几个小子峰。核星温度随新星亮度的下降而升高,其温度上限可能为120000K左右。更多还原

【Abstract】 Nova Cygni 1978 was observed from October 11 to December 23, 1978 at the Beijing Observatory with the grating spectrograph attached to the Naysmith 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 temperatures of the underlying star. The main spectral lines in wavelength range λλ3400—6700 from October 11 to 30 are those of the following atoms or ions: H, FeⅡ, NⅡ, TiⅡ, [0Ⅰ], [NⅡ], NⅢ. From November 10, lines of [OⅢ], HeⅠ and HeⅡ become visible one after another. The emission line H_α shows three components, of which the most redshifted is the strongest. In turn, each component consists of a number of weak emission peaks. Temperature of the underlying star increases with decline of the nova brightness. The upper limit of temperature may be～120000K.更多还原