The nova-like variable star HV 11976
The nova-like variable star HV 11976
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类新星变星 HV 11976
DOI：
10.1086/105935
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发表时间：
1946
期刊：
影响因子：
--
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
在1944年夏天，在哈佛天文台检查银河系179号场的光谱板时，伊迪丝·詹森小姐发现了一个光谱，在1929年4月2日出现了明亮的线条，而在1928年7月13日则没有。该天体起初被认为是一颗新星，但对几个板块的检查显示，一颗星星比最大亮度暗了不到两个星等，并且在爆发前后的位置都是相同的。还有一种可能性是，这颗星星是一颗真正的新星，它有一颗明亮的尚未解决的伴星。在这个阶段，詹森小姐离开了哈佛天文台，在沙普利博士的建议下，作者继续进行研究。表I给出了1875年的位置以及比较星和变星的星等。的幅度确定的板采取的10英寸梅特卡夫望远镜相比，附近的Carte du Ciel序列在i6 hom，-40？5.这些位置是用24英寸的布鲁斯望远镜在底片上测量的。图1是标记了比较星的字段的图表。在大约500个板块上估计了这个变量的大小。图2是除1905年至1912年和1918年至1923年这两个时间段之外的所有观测结果的曲线图。在第一个时间间隔内，观测结果的分布相当好，表明星星在最小值13.2等时相当不活跃。在第二个时间间隔内，观测结果很少，但都一致表明星星处于或接近最小值。似乎没有必要将所有意见全部列成表格。在表II中，
During the summer of 1944, while examining spectrum plates of Milky Way Field 179, at the Harvard Observatory, Miss Edith Janssen found a spectrum with bright lines present on 1929 April ii and lacking on 1928 July 13. The object was at first believed to be a nova, but examination of several plates showed a star less than two magnitudes fainter than the maximum, and in the same position, both before and after the outburst. There remained the possibility that the star was a true nova with a bright unresolved companion. At this stage Miss Janssen left the Harvard Observatory, and at the suggestion of Dr. Shapley, the writer continued the study. Positions for 1875 and magnitudes of the comparison stars and the variable are given in Table I. The magnitudes were determined on plates taken with the 10-inch Metcalf telescope by comparison with a nearby Carte du Ciel sequence at i6hom,—40? 5. The positions were measured on a plate taken with the 24-inch Bruce telescope. Figure 1 is a chart of the field on which the comparison stars are marked. The magnitude of the variable has been estimated on about 500 plates. Figure 2 is a plot of all the observations, except for the intervals 1905 to 1912 and 1918 to 1923. In the first of these intervals, a fairly good distribution of observations shows the star quite inactive at minimum, 13.2 mag. In the second interval there are very few observations, but all agree in showing the star at or near minimum. A complete tabulation of all the observations does not appear to be necessary. In Table II the