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arXiv 1601.04874astro-ph.SRastro-ph.HE
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一种估算Ia型超新星$^{56}$ Ni质量的无红化方法

A reddening-free method to estimate the $^{56}$Ni mass of Type Ia supernovae

S. Dhawan, B. Leibundgut, J. Spyromilio, S. Blondin

备注：
9 pages, 3 figures, Accepted to A&A
发表信息：
A&A 588, A84 (2016)
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摘要：

Ia型超新星（SNe\，Ia）数量的增加表明，该种群的多样性比过去所假设的要大。这种多样性的原因（例如亲本种群、爆炸机制）在很大程度上仍然未知。我们研究了SNe\，Ia近红外线曲线的一个样本，并将第二个极大值的相位与测热峰值亮度关联起来。峰值辐射热光度与第二个最大值的时间（相对于{ \it B}光曲线最大值）的关系如下：$L_{max}(10^{43} erg s^{-1}) = (0.039 \pm 0.004) \times t_2(J)(days) + (0.013 \pm 0.106)$。$^{56}$ Ni的质量可以根据阿内特规则从峰值光度导出，该规则规定最大光度等于镍衰变产生的瞬时能量。我们将这一假设与最近的质量延迟爆轰模型的辐射传递计算进行了比较，发现这一假设在最近的质量延迟爆轰模型的辐射传递计算中的有效性在10%以内。将$L_{max}$与$t_2$的关系应用于40个具有显著红化（$E(B-V) >$ 0.1 mag）的额外SNe ~ 1，Ia的样品，并建立了SNe~Ia的无红化的辐射热光度函数。通过直接观测SN 2014 J中大量吸收的$γ-$射线的$^{56}$ Ni质量测量，对该方法进行了测试，发现结果完全一致。超巨星系塞卡质量爆炸，特别是SN 1，2007 if，不遵循峰值光度与第二红外极大值之间的关系。这可能指向一个额外的能量源在最大光贡献。构造了SNe\，Ia的光度函数，结果表明它是不对称的，有一个低光度天体的尾部和一个相当尖锐的高光度截止，尽管它可能受到选择效应的影响.

英文摘要：

The increase in the number of Type Ia supernovae (SNe\,Ia) has demonstrated that the population shows larger diversity than has been assumed in the past. The reasons (e.g. parent population, explosion mechanism) for this diversity remain largely unknown. We have investigated a sample of SNe\,Ia near-infrared light curves and have correlated the phase of the second maximum with the bolometric peak luminosity. The peak bolometric luminosity is related to the time of the second maximum (relative to the {\it B} light curve maximum) as follows : $L_{max}(10^{43} erg s^{-1}) = (0.039 \pm 0.004) \times t_2(J)(days) + (0.013 \pm 0.106)$. $^{56}$Ni masses can be derived from the peak luminosity based on Arnett's rule, which states that the luminosity at maximum is equal to instantaneous energy generated by the nickel decay. We check this assumption against recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models and find this assumption is valid to within 10\% in recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models. The $L_{max}$ vs. $t_2$ relation is applied to a sample of 40 additional SNe\,Ia with significant reddening ($E(B-V) >$ 0.1 mag) and a reddening-free bolometric luminosity function of SNe~Ia is established. The method is tested with the $^{56}$Ni mass measurement from the direct observation of $γ-$rays in the heavily absorbed SN 2014J and found to be fully consistent. Super-Chandrasekhar-mass explosions, in particular SN\,2007if, do not follow the relations between peak luminosity and second IR maximum. This may point to an additional energy source contributing at maximum light. The luminosity function of SNe\,Ia is constructed and is shown to be asymmetric with a tail of low-luminosity objects and a rather sharp high-luminosity cutoff, although it might be influenced by selection effects.

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