Novae：I.最大震级与衰减时间（MMRD）和距离的关系
Novae: I. The maximum magnitude relation with decline time (MMRD) and distance
摘要：
新星最大绝对星等与下降时间的关系（MMRD）的起源和校准，首先由Zwicky（1936）推导，并由McLaughlin（1940）进行经验验证，广泛用于估计到经典新星的距离和新星绝对星等的近似恒定性，在光学极大值之后15天，Buscombe和de Vaucouleurs（1955）提出的一种新的线性化方法，并证明是有效的。本文的主要结果是：（1）基于能量瞬时注入到新星系统的MMRD的物理推导。(2)一个明显更好的约束MMRD：M_{V,0} = 2.16（+-0.16）log_{10} t_2 - 10.804（+-0.117），使用两步校准程序。(3)它表明，MMRD是最好的距离估计新星提供给我们的距离和精度主要是有限的低估的峰值视亮度。(4)结果表明，同样的MMRD校准适用于所有速度级的新星和银河系和河外新星。(5)结果表明：2.4 < t_2 <86 $d的新星在光学极大值后第12天的绝对星等离散度（M_{V,12} = -6.616 +-0.043）比第15天的小。我们重申，需要在光学波段的经典和复发新星爆发，有效地利用MMRD和M_{V,12}在确定其光度和距离的潜力的均匀高保真分光光度数据。
英文摘要：
The origin and calibration of the maximum absolute magnitude relation with decline time (MMRD) for novae, first derived by Zwicky (1936) empirically validated by McLaughlin (1940) and widely used to estimate distances to classical novae and the near-constancy of the absolute magnitude of novae, 15 days after optical maximum, suggested by Buscombe and de Vaucouleurs (1955) are revisited in this paper and found to be valid. The main results presented in the paper are: (1) A physical derivation of the MMRD based on instantaneous injection of energy to the nova system. (2) A significantly better-constrained MMRD: M_{V,0} = 2.16(+-0.16)log_{10}t_2 - 10.804(+-0.117) using a two step calibration procedure. (3) It is shown that the MMRD is one of the best distance estimators to novae available to us and that accuracy of the distances is predominantly limited by an underestimated peak apparent brightness. (4) It is shown that the same MMRD calibration is applicable to novae of all speed class and to both Galactic and extragalactic novae. (5) It is shown that the absolute magnitudes of novae with 2.4 < t_2 < 86$days have a smaller scatter on day 12 (M_{V,12} = -6.616 +-0.043) compared to day 15 following optical maximum. We reiterate the need for homogenised high fidelity spectrophotometric data in optical bands on classical and recurrent novae in outburst to effectively utilise the potential of the MMRD and M_{V,12} in determining their luminosities and distances.
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