标题： 对I型超新星单简并模型中对流过冲的影响 显示英文标题

标题： Impact of convective overshooting on the single-degenerate model of Type Ia supernovae

摘要： 单简并（SD）模型是Ia型超新星（SNe Ia）前身星的主要模型之一。 然而，它面临一些挑战，主要问题是无法解释观测到的SNe Ia诞生率。 许多研究通过扩展可能导致SNe Ia的参数空间（由初始供体恒星质量和轨道周期定义）以及改进双星种群合成来解决这一问题。 尽管这些努力取得了显著进展，但恒星物理中仍存在许多不确定性，这影响了此类研究的结果。 对流越界可以显著影响恒星的内部结构及其在双星系统中的演化，是恒星物理中最主要的不确定性来源之一。 我们研究了对流越界在SD模型中对SNe Ia参数空间和诞生率的影响。 我们采用了共同包层风（CEW）模型，即SD模型的新版本，作为我们的前身星模型。 使用MESA，我们获得了三种不同对流越界参数导致SNe Ia的参数空间，并计算了相应的SNe Ia诞生率。 对流越界扩大了大质量白矮星（WDs；>= 0.75Msun）系统的参数空间的上边界（对应于更大的初始供体质量）和右边界（对应于更长的初始轨道周期）。 然而，白矮星的最小质量以及低质量WDs的参数空间——以及因此计算出的SNe Ia诞生率——随着对流越界参数呈非单调变化。 CEW模型可能解释与周围介质（CSM）相互作用的SNe Ia，即SNe Ia-CSM。 我们发现，随着对流越界参数的增加，SNe Ia-CSM的参数空间及其诞生率都会增加。 显示英文摘要

摘要： The single-degenerate (SD) model is one of the principal models for the progenitors of Type Ia supernovae (SNe Ia). However, it faces some challenges, the primary being its inability to account for the observed SN Ia birth rate. Many studies have attempted to address this issue by expanding the parameter space, defined by the initial donor star mass and orbital period, that can lead to SNe Ia, as well as by improving binary population synthesis. While these efforts have led to significant progress, many uncertainties in stellar physics persist, which influences the outcomes of such studies. Convective overshooting, which can significantly affect the internal structure of a star and subsequently its evolution within a binary system, is one of the most significant sources of uncertainty in stellar physics. We investigate the effect of convective overshooting on the parameter space and birth rate of SNe Ia within the SD model. We employed the common-envelope wind (CEW) model, a new version of the SD model, as our progenitor model. Using MESA, we obtained the parameter space that leads to SNe Ia for three different convective overshooting parameters and calculated the corresponding SN Ia birth rate. Convective overshooting expands the upper boundaries (corresponding to a larger initial donor mass) and right boundaries (corresponding to a longer initial orbital period) of the parameter space for systems with massive white dwarfs (WDs; >= 0.75Msun). However, the minimum WD mass and the parameter space for low-mass WDs - and, consequently, the calculated SN Ia birth rate - vary non-monotonically with convective overshooting parameters. The CEW model may explain the SNe Ia that interact with the circumstellar medium (CSM), i.e., SNe Ia-CSM. We find that the parameter space for SNe Ia-CSM increases with convective overshooting parameters, as does their birth rate.