论文标题
早期相互作用超新星的祖细胞
Progenitors of early-time interacting supernovae
论文作者
论文摘要
我们使用辐射传输代码CMFGEN计算了一组超新星的早期光谱。我们的模型适用于爆炸后1到几天观察到的事件。使用这些模型，我们限制了17个观察到的相互作用超新星的样本的祖细胞和爆炸特性。由于巨大的恒星具有强大的质量损失，因此这些光谱提供了有关超新星祖细胞的有价值信息，例如质量损失率，风速和表面丰度。 We show that these events span a wide range of explosion and progenitor properties, exhibiting supernova luminosities in the 1e8 to 1e12 Lsun range, temperatures from 10000 to 60000 K, progenitor mass-loss rates from a few 1e-4 up to 1 Msun/yr, wind velocities from 100 to 800 km/s, and surface abundances from solar-like to H-depleted.我们的结果表明，与大型恒星在其余的一生中相比，许多超新星与星际材料相互作用的祖细胞在爆炸前的质量损失显着增加。我们还推断出表面丰度和质量损失率之间的相关性不足。这可能表明，探索前质量损失机制独立于恒星质量。我们发现，这些事件中的大多数具有CNO处理的表面丰度。在单星情景中，这表明偏爱高质量的RSG作为相互作用的SNE的祖细胞，而二元进化可能会影响这一结论。我们的模型公开可用，并且很容易适用，可用于分析正在进行的大规模调查（例如Zwicky Transient Factory）的结果。
We compute an extensive set of early-time spectra of supernovae interacting with circumstellar material using the radiative transfer code CMFGEN. Our models are applicable to events observed from 1 to a few days after explosion. Using these models, we constrain the progenitor and explosion properties of a sample of 17 observed interacting supernovae at early-times. Because massive stars have strong mass loss, these spectra provide valuable information about supernova progenitors, such as mass-loss rates, wind velocities, and surface abundances. We show that these events span a wide range of explosion and progenitor properties, exhibiting supernova luminosities in the 1e8 to 1e12 Lsun range, temperatures from 10000 to 60000 K, progenitor mass-loss rates from a few 1e-4 up to 1 Msun/yr, wind velocities from 100 to 800 km/s, and surface abundances from solar-like to H-depleted. Our results suggest that many progenitors of supernovae interacting with circumstellar material have significantly increased mass-loss before explosion compared to what massive stars show during the rest of their lifetimes. We also infer a lack of correlation between surface abundances and mass-loss rates. This may point to the pre-explosion mass-loss mechanism being independent of stellar mass. We find that the majority of these events have CNO-processed surface abundances. In the single star scenario this points to a preference towards high-mass RSGs as progenitors of interacting SNe, while binary evolution could impact this conclusion. Our models are publicly available and readily applicable to analyze results from ongoing and future large scale surveys such as the Zwicky Transient Factory.
