Fast evolving pair-instability supernova models: evolution, explosion, light curves
Fast evolving pair-instability supernova models: evolution, explosion, light curves
复制标题
快速演化的对不稳定超新星模型：演化、爆炸、光变曲线
DOI：
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
E. Sorokina
中科院分区：
文献类型：
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作者：
A. Kozyreva;Matthew S. Gilmer;R. Hirschi;C. Frohlich;S. Blinnikov;R. Wollaeger;U. M. Noebauer;D. V. Rossum;A. Heger;W. Even;R. Waldman;A. Tolstov;E. Chatzopoulos;E. Sorokina
随着越来越多的超亮超新星（SLSNe）被发现，它们的起源问题仍然悬而未决，并在超新星界引起了激烈的争论。目前，SLSNe有三种被提出的机制：(1)对不稳定超新星（PISN），(2)磁驱动超新星，以及(3)超新星喷发物与爆炸前喷出的星周物质相互作用的模型。根据目前对SLSNe的观测，PISN的起源由于许多原因而不受欢迎。由于大量的喷射物和大量的镍，许多PISN模型提供了过于宽泛的光曲线和过于泛红的光谱。在当前的研究中，我们使用GENEC代码计算的祖模型重新检查PISN属性。我们用FLASH和辐射流体力学代码STELLA计算超新星爆炸和光曲线演化。我们发现，金属丰度相对较高（Z=0.001）的高质量模型（200和250太阳质量）在外层不保留氢，并产生相对快速发展的ⅰ型PISNe，可能适合解释一些SLSNe。我们还研究了光曲线建模中由于编码、不透明、镍泡效应和前体结构和组成而产生的不确定性。
With an increasing number of superluminous supernovae (SLSNe) discovered the question of their origin remains open and causes heated debates in the supernova community. Currently, there are three proposed mechanisms for SLSNe: (1) pair-instability supernovae (PISN), (2) magnetar-driven supernovae, and (3) models in which the supernova ejecta interacts with a circumstellar material ejected before the explosion. Based on current observations of SLSNe, the PISN origin has been disfavoured for a number of reasons. Many PISN models provide overly broad light curves and too reddened spectra, because of massive ejecta and a high amount of nickel. In the current study we re-examine PISN properties using progenitor models computed with the GENEC code. We calculate supernova explosions with FLASH and light curve evolution with the radiation hydrodynamics code STELLA. We find that high-mass models (200 and 250 solar masses) at relatively high metallicity (Z=0.001) do not retain hydrogen in the outer layers and produce relatively fast evolving PISNe Type I and might be suitable to explain some SLSNe. We also investigate uncertainties in light curve modelling due to codes, opacities, the nickel-bubble effect and progenitor structure and composition.
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
银河中心的孤立大质量恒星：拱门和五重星团的动态贡献
DOI：
10.1051/0004-6361/201323030
发表时间：
2014
期刊：
arXiv: Solar and Stellar Astrophysics
影响因子：
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作者：
Habibi;Stolte;Harfst
通讯作者：
Harfst