LOCATIONS OF ORIGIN OF SPECTRAL FEATURES OF NOVAE
LOCATIONS OF ORIGIN OF SPECTRAL FEATURES OF NOVAE
复制标题
新星光谱特征的起源位置
DOI：
10.1086/125957
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发表时间：
1947
影响因子：
3.5
通讯作者：
D. B. Mclaughlin
中科院分区：
文献类型：
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作者：
D. B. Mclaughlin
关于新星周围吸收云和发射云的排列的一般方案以前已经概述过了。[1]本说明的目的是审查所提出的结构所依据的主要证据点，这些证据点必须由任何替代模型来满足。在几乎所有经过彻底研究的新星的光谱中，可以识别出四个吸收系统，每个吸收系统都与一组发射“带”相关联，实际上是在其正常位置附近加宽的明亮线条。这些系统是：（1）前极大，（2）主要，（3）“扩散增强”，（4）猎户座。最后是Ho附近的强N吸收线和宽的朦胧的“4640”发射。列表的顺序是按时间顺序排列的，但也是吸收速度或发射宽度增加的顺序，以及激发增加的顺序。表I总结了这些系统与新星光变曲线的关系。最后一列给出了1918年天鹰座新星中每组吸收线最大发展时的近似速度。
A general scheme of the arrangement of absorbing and emitting clouds about a nova has been previously outlined.1 The purpose of this note is to review the main points of evidence on which the proposed structure is based and which must be satisfied by any alternative model. In the spectra of practically all the thoroughly studied novae it is possible to recognize four absorption systems with each of which is associated a set of emission "bands" actually bright lines widened about their normal positions. These systems are : (1) pre-maximum, (2) principal, (3) "diffuse-enhanced," (4) Orion. The last includes the strong N in absorption lines near Ho and the broad hazy "4640" emission. The order of listing is chronological, but it is also that of increasing absorption velocity or emission width, as well as of increasing excitation. Table I summarizes the relationships of these systems to the light-curve of the nova. In the last column are given approximate velocities of the absorption lines of each set at its maximum development in Nova Aquilae 1918.