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arXiv 2409.03540astro-ph.HE
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II型超新星富氢包层质量的多样性（II）：SN 2023ixf作为部分剥离中等质量恒星的爆炸

Diversity in hydrogen-rich envelope mass of type II supernovae (II): SN 2023ixf as explosion of partially-stripped intermediate massive star

Qiliang Fang, Takashi J. Moriya, Lucía Ferrari, Keiichi Maeda, Gaston Folatelli, Keila Y. Ertini, Hanindyo Kuncarayakti, Jennifer E. Andrews, Tatsuya Matsumoto

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12 pages, 4 figures. Submitted
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AI总结：

本文通过光变曲线建模和晚相光谱分析，确定SN 2023ixf是一颗ZAMS质量为15-16倍太阳质量、氢包层被部分剥离至4-5倍太阳质量的中等质量恒星的非球对称爆炸。

摘要：

SN 2023ixf是近几十年来观测最为充分的核坍缩超新星之一，然而对其前身星的零龄主序（ZAMS）质量$M_{\rm ZAMS}$的推断存在不一致。对超新星爆发前红超巨星（RSG）的直接观测估计$M_{\rm ZAMS}$的范围很广，从11到18 $M_{\rm \odot}$不等。额外的约束条件，包括宿主环境和其前身红超巨星的脉动，表明存在一个$M_{\rm ZAMS}$ > 17 $M_{\rm \odot}$的大质量前身星。然而，对超新星性质的分析，从光变曲线建模到晚相光谱，都倾向于相对低质量的情形（$M_{\rm ZAMS}$ < 15 $M_{\rm \odot}$）。在这项工作中，我们对SN 2023ixf进行了系统分析，从红超巨星前身星、平台期光变曲线到晚相光谱。利用MESA+STELLA模拟红超巨星前身星及其爆炸，我们发现，尽管红超巨星模型的ZAMS质量在12.0到17.5 $M_{\rm \odot}$之间变化，但如果允许包层质量和爆炸能量变化，它们可以产生与SN 2023ixf很好匹配的光变曲线。利用晚相光谱作为独立测量手段，氧发射线[O I]表明ZAMS为中等质量（约16.0 $M_{\rm \odot}$），而相对较弱的H$α$发射线表明氢包层在爆炸前已被部分移除。通过将光变曲线建模导出的速度结构纳入轴对称模型，我们成功生成了与SN 2023ixf晚相光谱中观测到的[O I]线一致的[O I]线轮廓。综合这些分析，我们得出结论：SN 2023ixf是一颗中等质量恒星（$M_{\rm ZAMS}$ = 15-16 $M_{\rm \odot}$）的非球对称爆炸，其氢包层在爆炸前被部分剥离至4-5 $M_{\rm \odot}$。

英文摘要：

SN 2023ixf is one of the most well-observed core-collapse supernova in recent decades, yet there is inconsistency in the inferred zero-age-main-sequence (ZAMS) mass $M_{\rm ZAMS}$ of its progenitor. Direct observations of the pre-SN red supergiant (RSG) estimate $M_{\rm ZAMS}$ spanning widely from 11 to 18 $M_{\rm \odot}$. Additional constraints, including host environment and the pulsation of its progenitor RSG, suggest a massive progenitor with $M_{\rm ZAMS}$ > 17 $M_{\rm \odot}$. However, the analysis of the properties of supernova, from light curve modeling to late phase spectroscopy, favor a relatively low mass scenario ($M_{\rm ZAMS}$ < 15 $M_{\rm \odot}$). In this work, we conduct systematic analysis of SN 2023ixf, from the RSG progenitor, plateau phase light curve to late phase spectroscopy. Using MESA+STELLA to simulate the RSG progenitor and their explosions, we find that, despite the ZAMS mass of the RSG models being varied from 12.0 to 17.5 $M_{\rm \odot}$, they can produce light curves that well match with SN 2023ixf if the envelope mass and the explosion energy are allowed to vary. Using late phase spectroscopy as independent measurement, the oxygen emission line [O I] suggests the ZAMS is intermediate massive (~16.0 $M_{\rm \odot}$), and the relatively weak H$α$ emission line indicates the hydrogen envelope has been partially removed before the explosion. By incorporating the velocity structure derived from the light curve modeling into an axisymmetric model, we successfully generated [O I] line profiles that are consistent with the [O I] line observed in late phase spectroscopy of SN 2023ixf. Bringing these analyses together, we conclude that SN 2023ixf is the aspherical explosion of an intermediate massive star ($M_{\rm ZAMS}$ = 15-16 $M_{\rm \odot}$) with the hydrogen envelope being partially stripped to 4-5 $M_{\rm \odot}$ prior to its explosion.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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