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Ia型超新星的$^{56}$ Ni产额分布及其对祖先的意义

Distribution of $^{56}$Ni Yields of Type Ia Supernovae and its Implication for Progenitors

Bo Wang, Xiangcun Meng, Xiaofeng Wang, Zhanwen Han

备注：
11 pages, 7 figures
发表信息：
Chin.J.Astron.Astrophys.8:71-80,2008
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摘要：

Ia型超新星爆发产生的$^{56}$ Ni的量可能是Ia型超新星光度与其光变曲线相关性的最重要的物理参数。基于$^{56}$ Ni质量与光变曲线参数$\triangle m_{15}$之间的经验关系，我们获得了附近超新星Ia大样本的$^{56}$ Ni质量的粗略估计，目的是探索超新星Ia的多样性。我们发现，不同SNe Ia的推导出的$^{56}$ Ni质量可以变化十倍（例如，$M_{\rm Ni}=0.1 - 1.3$ $M_{\odot}$），这不能用标准的拉塞卡质量模型（$^{56}$ Ni的质量产量为0.4 - 0.8 $M_{\odot}$）来解释。对于不同的Ia超新星，特别是对于那些极贫镍和富镍的生产者，显然需要不同的爆炸和/或祖先模型。富镍（含$M_{\rm Ni}$ $>$ 0.8 $M_{\odot}$）SNe Ia非常明亮，并且可能具有大量的超过克拉塞卡质量极限的原始体，因为需要额外的原始体燃料来产生更多的$^{56}$ Ni，从而为光变曲线提供动力。这也与本质上明亮的Ia超新星更喜欢出现在年轻和大质量恒星的恒星环境中的发现相一致。例如，75%的Ia超新星在螺旋星系中具有$Δm_{15} < 1.2$，而在E/S 0星系中这一比例仅为18%。另一方面，贫镍的Ia型超新星（$M_{\rm Ni}$ $<$ 0.2 $M_{\odot}$）可能符合亚克拉塞卡模型，因为它们大多数都是在由较老和低质量的恒星星族占主导地位的早期型E/S 0星系中发现的。这表明螺旋星系和E/S 0星系中的SNe Ia具有不同性质的祖先。

英文摘要：

The amount of $^{56}$Ni produced in type Ia supernova (SN Ia) explosion is probably the most important physical parameter underlying the observed correlation of SN Ia luminosities with their light curves. Based on an empirical relation between the $^{56}$Ni mass and the light curve parameter $\triangle m_{15}$, we obtained rough estimates of the $^{56}$Ni mass for a large sample of nearby SNe Ia with the aim of exploring the diversity in SN Ia. We found that the derived $^{56}$Ni masses for different SNe Ia could vary by a factor of ten (e.g., $M_{\rm Ni}=0.1 - 1.3$ $M_{\odot}$), which cannot be explained in terms of the standard Chandrasekhar-mass model (with a $^{56}$Ni mass production of 0.4 -- 0.8 $M_{\odot}$). Different explosion and/or progenitor models are clearly required for various SNe Ia, in particular, for those extremely nickel-poor and nickel-rich producers. The nickel-rich (with $M_{\rm Ni}$ $>$ 0.8 $M_{\odot}$) SNe Ia are very luminous and may have massive progenitors exceeding the Chandrasekhar-mass limit since extra progenitor fuel is required to produce more $^{56}$Ni to power the light curve. This is also consistent with the finding that the intrinsically bright SNe Ia prefer to occur in stellar environments of young and massive stars. For example, 75% SNe Ia in spirals have $Δm_{15} < 1.2$ while this ratio is only 18% in E/S0 galaxies. On the other hand, the nickel-poor SNe Ia (with $M_{\rm Ni}$ $<$ 0.2 $M_{\odot}$) may invoke the sub-Chandrasekhar model, as most of them were found in early-type E/S0 galaxies dominated by the older and low-mass stellar populations. This indicates that SNe Ia in spiral and E/S0 galaxies have progenitors of different properties.

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