Abstract

We consider the effect of a change in the rate of flux decline in the \(U\) band for type II-P supernovae (SNe IIP) as a function of metallicity \(Z\). Based on this effect, we propose a new method to determine the photometric redshift from the SN IIP light curve in the \(U\) band. Using the STELLA code, we have constructed model light curves in different bands for different redshifts \(z=0.0\), 0.1, and 0.3 as the metallicity in the models decreases from \(Z\sim 10^{-3}\) to \({\sim}10^{-6}\). The flux in the \(U\) band is shown to reach a plateau at the lowest metallicities. We consider the influence of other parameters as well: the presupernova mass and the mass of radioactive nickel-56.

中文翻译：

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II型超新星高原形状对金属性的依赖性研究

摘要

我们认为II-P型超新星（SNe IIP）的\（U \）波段通量下降速率的变化的影响是金属性\（Z \）的函数。基于此效果，我们提出了一种从\（U \）波段的SN IIP光曲线确定光度红移的新方法。使用STELLA代码，随着模型中的金属性从\（Z \ sim 10 ^ {-3} \减小，我们针对不同的红移\（z = 0.0 \），0.1和0.3构造了不同波段的模型光曲线。到\（{\ sim} 10 ^ {-6} \）。\（U \）中的通量所示的金属带在最低金属含量时达到平稳状态。我们还考虑了其​​他参数的影响：超新星前质量和放射性镍56的质量。