We examine the sensitivity of neutrino emissions to stellar evolution models for a 15$M_\odot$ progenitor, paying particular attention to a phase prior to the collapse. We demonstrate that the number luminosities in both electron-type neutrinos ($\nu_e$) and their anti-partners ($\bar{\nu}_e$) differ by more than an order of magnitude by changing spatial resolutions and nuclear network sizes on stellar evolution models. We also develop a phenomenological model to capture the essential trend of the diversity, in which neutrino luminosities are expressed as a function of central density, temperature and electron fraction. In the analysis, we show that neutrino luminosity can be well characterized by these central quantities. This analysis also reveals that the most influential quantity to the time evolution of $\nu_e$ luminosity is matter density, while it is temperature for $\bar{\nu}_e$. These qualitative trends will be useful and applicable to constrain the physical state of progenitors at the final stages of stellar evolution from future neutrino observations, although more detailed systematic studies including various mass progenitors are required to assess the applicability.

中文翻译：

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超新星前中微子对恒星演化模型的敏感性

我们研究了中微子排放对 15$M_\odot$ 前身恒星演化模型的敏感性，特别关注坍缩前的一个阶段。我们证明了通过改变空间分辨率和核网络大小，电子型中微子 ($\nu_e$) 和它们的反中微子 ($\bar{\nu}_e$) 的数量光度差异超过一个数量级关于恒星演化模型。我们还开发了一个现象学模型来捕捉多样性的基本趋势，其中中微子光度表示为中心密度、温度和电子分数的函数。在分析中，我们表明这些中心量可以很好地表征中微子光度。该分析还表明，对 $\nu_e$ 光度的时间演化影响最大的量是物质密度，而它是 $\bar{\nu}_e$ 的温度。这些定性趋势将是有用的，适用于从未来的中微子观测中限制恒星演化最后阶段的祖细胞的物理状态，尽管需要包括各种质量祖细胞在内的更详细的系统研究来评估适用性。