论文标题
超新星双向光曲线来自双尼克分布
Supernovae double-peaked light curves from double-nickel distribution
论文作者
论文摘要
在不同的亮度的超新星（SNE）中，已经观察到许多双峰光曲线（LC），代表了广泛的形态学品种。在这项工作中，我们研究了哪些可以通过假设其放射性材料的双峰分布来建模，这最初是针对SN2005BF提出的。内部区域对应于常规的爆炸性核合成，并根据通常的混合情况向外延伸。富含56ni的外壳可能与射流样流出的效果有关，后者在SN冲击的到来之前与恒星更遥远的部分相互作用。由于外层被光学上较小的物质覆盖，因此其能量较早出现并产生辐射的第一峰。为了更详细地研究这种情况，我们应用了流体动力代码，该代码遵循祖细胞恒星的冲击传播，并考虑了放射性同位素衰减产生的伽马射线光子的效果。我们为56NI丰度曲线提供了一个简单的参数模型，并探讨了对LC的后果，该液体的后果是单独改变定义该分布的数量的液体，将我们的重点放在了剥离的Envelope祖细胞上。在第一项研究中，我们对该模型对尚未被归类为超浮性的SNE的适用性感兴趣，因此，我们已经相应地选择了我们的参数空间。然后，在56Ni-Profile的相同数学处方中，我们重新审视了一系列对象的建模过程：SN2005BF，PTF2011MNB，SN2019CAD和SN2008D。在某些情况下，需要减少伽马射线不透明度以适应晚期观察。我们还讨论了这种情况可能可以解释LC形态的其他情况。
Among supernovae (SNe) of different luminosities, many double-peaked light curves (LCs) have been observed, representing a broad morphological variety. In this work, we investigate which of these can be modelled by assuming a double-peaked distribution of their radioactive material, as originally proposed for SN2005bf. The inner zone corresponds to the regular explosive nucleosynthesis and extends outwards, according to the usual scenario of mixing. The outer 56Ni-rich shell may be related to the effect of jet-like outflows that have interacted with more distant portions of the star before the arrival of the SN shock. As the outer layer is covered by matter that is optically less thick, its energy emerges earlier and generates a first peak of radiation. To investigate this scenario in more detail, we have applied our hydrodynamic code that follows the shock propagation through the progenitor star and takes into account the effect of the gamma-ray photons produced by the decay of the radioactive isotopes. We present a simple parametric model for the 56Ni abundance profile and explore the consequences on the LC of individually varying the quantities that define this distribution, setting our focus onto the stripped-envelope progenitors. In this first study, we are interested in the applicability of this model to SNe that have not been classified as superluminous, thus, we have selected our parameter space accordingly. Then, within the same mathematical prescription for the 56Ni-profile, we revisited the modelling process for a series of objects: SN2005bf, PTF2011mnb, SN2019cad, and SN2008D. In some cases, a decrease in the gamma ray opacity is required to fit the late time observations. We also discuss the other cases in which this scenario might be likely to explain the LC morphology.
