论文标题
sub-chandrasekhar-mas爆炸与观察到的$ t_0-m_ \ text {ni56} $ IA类型IA超新星的关系紧张
Sub-Chandrasekhar-mass detonations are in tension with the observed $t_0-M_\text{Ni56}$ relation of type Ia supernovae
论文作者
论文摘要
IA型超新星（SNE IA）可能是碳氧气（CO）白色谷歌（WD）恒星的热核爆炸，但其祖细胞系统仍然难以捉摸。最近的研究表明，围绕亚chandrasekhar质量核心的薄氦壳内的传播爆炸可以随后触发核心内的爆炸（双二键模型，DDM）。这次爆炸的结果类似于亚chandrasekhar质量Co WD（SCD）的中心点火。尽管SCD与SNE IA的某些观察性特性是一致的，但一些计算挑战禁止与观测值进行良好的比较。我们专注于观察到的$ t_0-m_ \ text {ni56} $关系，其中$ t_0 $（$γ$ -rays从弹射器中的逃生时间）与$ m_ \ text {ni56} $（合成的$^{56} $ ni ass）呈正相关。我们应用了我们最近开发的数值方案来计算SCD，并表明计算出的$ T_0-M_ \ text {ni56} $关系，该关系不需要辐射传输计算，而是将其收敛至几个百分之几的精度。我们在计算和观察到的$ T_0-m_ \ text {ni56} $关系之间找到明确的张力。 SCD预测$ t_0 $和$ m_ \ text {ni56} $之间的反相关，并带有$ t_0 \ oft30 \，\ textrm {day} $用于发光（$ m_ \ text {ni56} \ gtrsim0.5 \ gtrsim0.5 \ \，m _ _ { $ 35-45 \，\ textrm {day} $。我们表明，这种张力大于结果的不确定性，并且它存在于对问题的所有先前研究中。我们的结果暗示，需要更复杂的模型，但我们认为DDM不太可能通过观测来解决张力。
Type Ia supernovae (SNe Ia) are likely the thermonuclear explosions of carbon-oxygen (CO) white-dwarf (WD) stars, but their progenitor systems remain elusive. Recent studies have suggested that a propagating detonation within a thin helium shell surrounding a sub-Chandrasekhar mass CO core can subsequently trigger a detonation within the core (the double-detonation model, DDM). The outcome of this explosion is similar to a central ignition of a sub-Chandrasekhar mass CO WD (SCD). While SCD is consistent with some observational properties of SNe Ia, several computational challenges prohibit a robust comparison to the observations. We focus on the observed $t_0-M_\text{Ni56}$ relation, where $t_0$ (the $γ$-rays' escape time from the ejecta) is positively correlated with $M_\text{Ni56}$ (the synthesized $^{56}$Ni mass). We apply our recently developed numerical scheme to calculate SCD and show that the calculated $t_0-M_\text{Ni56}$ relation, which does not require radiation transfer calculations, converges to an accuracy of a few percent. We find a clear tension between our calculations and the observed $t_0-M_\text{Ni56}$ relation. SCD predicts an anti-correlation between $t_0$ and $M_\text{Ni56}$, with $t_0\approx30\,\textrm{day}$ for luminous ($M_\text{Ni56}\gtrsim0.5\,M_{\odot}$) SNe Ia, while the observed $t_0$ is in the range of $35-45\,\textrm{day}$. We show that this tension is larger than the uncertainty of the results, and that it exists in all previous studies of the problem. Our results hint that more complicated models are required, but we argue that DDM is unlikely to resolve the tension with the observations.
