Synthetic light curves and spectra from a self-consistent 2D simulation of an ultra-strippped supernova
Synthetic light curves and spectra from a self-consistent 2D simulation of an ultra-strippped supernova
复制标题
来自超剥离超新星自洽二维模拟的合成光变曲线和光谱
DOI：
10.1093/mnras/stad3284
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发表时间：
2024
影响因子：
4.8
通讯作者：
Maunder T
中科院分区：
文献类型：
--
作者：
Maunder T
光谱学是一个重要的工具，提供洞察结构的核心坍缩超新星爆炸。我们使用Monte Carlo辐射传输代码artisto计算合成光谱和光变曲线的超剥离超新星的二维爆炸模型的基础上。这些计算的目的是确定可观察到的指纹的超剥离超新星和作为一个原则的证明，使用合成光谱学，以限制更广泛的剥离信封超新星的性质。我们预测我们的超剥离爆炸模型的特征光谱和光度特征，并发现这些不匹配观察到的超剥离超新星候选人，如SN 2005 ek。该模型的峰值热光度为、R波段的峰值量级，且Δm15，R= 3.50，比SN 2005 ek更暗，发展速度更快，是光度特性中最接近的可能模拟物。预测的光谱是非常不寻常的。最突出的特征是在2 {，}800\，{\mathring{\rm A}}$和4 {，}500\，{\mathring{\rm A}}$处的Mgilines和在晚期的红外Ca三重态。Mg线对模型的多维结构敏感，并且与视角相关。他们消失，由于线覆盖铁族元素在球平均模型与额外的微观混合。在未来的研究中，多维辐射传输计算需要应用到更广泛的模型，以阐明观察到的Ib/c型超新星的性质。
Spectroscopy is an important tool for providing insights into the structure of core-collapse supernova explosions. We use the Monte Carlo radiative transfer codeartisto compute synthetic spectra and light curves based on a two-dimensional explosion model of an ultra-stripped supernova. These calculations are designed both to identify observable fingerprints of ultra-stripped supernovae and as a proof of principle for using synthetic spectroscopy to constrain the nature of stripped-envelope supernovae more broadly. We predict characteristic spectral and photometric features for our ultra-stripped explosion model, and find that these do not match observed ultra-stripped supernova candidates like SN 2005ek. With a peak bolometric luminosity of, a peak magnitude ofinRband, and Δm15,R= 3.50, the model is even fainter and evolves even faster than SN 2005ek as the closest possible analogue in photometric properties. The predicted spectra are extremely unusual. The most prominent features are Mgiilines at $2 {,}800\, {\mathring{\rm A}}$ and $4 {,}500\, {\mathring{\rm A}}$ and the infrared Ca triplet at late times. The Mg lines are sensitive to the multidimensional structure of the model and are viewing-angle dependent. They disappear due to line blanketing by iron group elements in a spherically averaged model with additional microscopic mixing. In future studies, multi-D radiative transfer calculations need to be applied to a broader range of models to elucidate the nature of observed Type Ib/c supernovae.