探索 M31 中新星的最大亮度与衰减率的关系

J. Grace Clark, Kamil Hornoch, Allen W. Shafter, Hana Kučáková, Jan Vraštil, Peter Kušnirák, Marek Wolf
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摘要

本文介绍了对 M31 中的新星进行的长达二十年的 R 波段测光调查的结果。根据这些数据,确定了 180 个新星的 R 波段光变曲线,其数据足以估算峰值亮度和随后的衰减率。数据显示峰值亮度与衰减率之间存在微弱的相关性,这与众所周知的最大亮度与衰减率(MMRD)关系是一致的。正如银河系新星的普遍情况一样,MMRD 关系中的巨大散差使其无法用于确定单个新星的距离。新星最大亮度的标准偏差 σ = 0.89 等,围绕平均 R 波段绝对星等的分布为〈M R 〉 = -7.57 ± 0.07。M31的整体光度分布与银河系新星的光度分布非常吻合,这表明M31和银河系的新星群非常相似。我们还探讨了所有新星都可以用最大光后 15 天的标准光度(M 15)来表征的概念。出乎意料的是,M 15 值的分布特点是标准偏差仅比最大光时的新星标准偏差略小,因此对于精确的河外距离测定没有什么希望。根据它们在MMRD图和M 15分布图中的位置,我们确定了十几颗暗新星和快新星,它们很可能是以前未发现的周期新星。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Exploring the Maximum Magnitude versus Rate of Decline Relation for Novae in M31
The results of a two-decade-long R-band photometric survey of novae in M31 are presented. From these data, R-band light curves have been determined for 180 novae with data sufficient for estimating the peak brightness and subsequent rate of decline. The data show a weak correlation of peak brightness with fade rate consistent with the well-known maximum magnitude versus rate of decline (MMRD) relation. As generally appreciated for Galactic novae, the large scatter in the MMRD relation precludes its use in determining distances to individual novae. The novae at maximum light are distributed with standard deviation σ = 0.89 mag about a mean R-band absolute magnitude given by 〈M R 〉 = −7.57 ± 0.07. The overall M31 luminosity distribution is in excellent agreement with that found for Galactic novae suggesting that the nova populations in M31 and the Galaxy are quite similar. The notion that all novae can be characterized by a standard luminosity 15 days after maximum light (M 15) is also explored. Surprisingly, the distribution of M 15 values is characterized by a standard deviation only slightly smaller than that for novae at maximum light and thus offers little promise for precise extragalactic distance determinations. A dozen faint and fast novae that are likely to be previously unidentified recurrent novae have been identified from their position in the MMRD plot and in the M 15 distribution.
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