OGLE14-073 – a promising pair-instability supernova candidate
OGLE14-073 – a promising pair-instability supernova candidate
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OGLE14-073——一个有前途的不稳定对超新星候选者
DOI：
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发表时间：
2018
期刊：
影响因子：
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通讯作者：
R. Hirschi
中科院分区：
文献类型：
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作者：
A. Kozyreva;M. Kromer;U. M. Noebauer;R. Hirschi
最近发现的明亮的II型超新星OGLE 14 -073演化非常缓慢。光变曲线在发现后的90天内上升到最大值，然后以与56 Co的放射性衰变相容的速度下降。在这项研究中，我们表明，对不稳定超新星是一个合理的机制，这一事件。我们用辐射流体力学程序STELLA计算了两个M（ZAMS）= 150太阳质量，Z=0.001的原恒星的爆炸模型和光变曲线。通过在模型中心添加额外的56 Ni并将氢混合到喷出物的内层中，使其径向质量坐标为10个太阳质量，我们获得了与OGLE 14 -073宽带光变曲线的满意拟合。额外的56镍需要点到一个稍微大一点的祖星星。氢气的混合可能是由于爆炸过程中的大规模混合。我们还提出了我们的模型模拟的Monte Carlo辐射传输代码ARTIS的合成光谱。合成光谱再现了OGLE 14 -073观测光谱的主要特征。我们的结论是OGLE 14 -073是一个对不稳定爆炸的最有希望的候选人之一。
The recently discovered bright type II supernova OGLE14-073 evolved very slowly. The light curve rose to maximum for 90 days from discovery and then declined at a rate compatible with the radioactive decay of 56Co. In this study, we show that a pair-instability supernova is a plausible mechanism for this event. We calculate explosion models and light curves with the radiation hydrodynamics code STELLA starting from two M(ZAMS) = 150 solar masses, Z=0.001 progenitors. We obtain satisfactory fits to OGLE14-073 broadband light curves by including additional 56Ni in the centre of the models and mixing hydrogen down into the inner layers of the ejecta to a radial mass coordinate of 10 solar masses. The extra 56Ni required points to a slightly more massive progenitor star. The mixing of hydrogen could be due to large scale mixing during the explosion. We also present synthetic spectra for our models simulated with the Monte Carlo radiative transfer code ARTIS. The synthetic spectra reproduce the main features of the observed spectra of OGLE14-073. We conclude that OGLE14-073 is one of the most promising candidates for a pair-instability explosion.
DOI：
10.1017/s1743921314004657
发表时间：
2012-08
期刊：
Proceedings of the International Astronomical Union
影响因子：
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作者：
J. Vink
通讯作者：
J. Vink