We present generalized supernova (SN) light curve (LC) models for a variety of power inputs. We provide an expression for the power input that is produced by self-similar forward and reverse shocks in SN ejecta - circumstellar matter (CSM) interaction. We find that this ejecta-CSM interaction luminosity is in agreement with results from multi-dimensional radiation hydrodynamics simulations in the optically-thin case. We develop a model for the case of an optically-thick CSM by invoking an approximation for the effects of radiative diffusion. In the context of this model, we provide predictions for the time of forward shock break-out from the optically-thick part of the CSM envelope. We also introduce a hybrid LC model that incorporates ejecta-CSM interaction plus Ni-56 and Co-56 radioactive decay input. We fit this hybrid model to the LC of the Super-Luminous Supernova (SLSN) 2006gy. We find that this model provides a better fit to the LC of this event than previously presented models. We also address the relation between Type IIL and Type IIn SN with ejecta-CSM interaction models. Forward and reverse shock power input due to CSM interaction can produce the LCs of Type IIn SNe in terms of duration, shape and decline rate. This model can also produce LCs that are symmetric in shape around peak luminosity. We conclude that the observed LC variety of SNe Type IIn and of the SLSNe is likely to be a byproduct of the large range of conditions relevant to significant ejecta-CSM interaction as a power source.
Analytical modeling of polarization signals arising from confined circumstellar material in Type II supernovae
University of Turku（图尔库大学）；Aalto University Metsähovi Radio Observatory（阿尔托大学梅萨霍维射电天文台）；Aalto University Department of Electronics and Nanoengineering（阿尔托大学电子与纳米工程系）；Kyoto University（京都大学）；The University of Tokyo（东京大学）
Average opacity calculation for core-collapse supernovae
超新星（SNe）是现代天体物理学研究最深入的对象之一，但由于其复杂的物理性质，理论模型对于更好地理解这些爆炸恒星以及发射辐射的变化特性至关重要。SNe光变曲线建模的一种可能性是构造一个简化的半解析模型，该模型可用于获得SN性质的数量级估计。在大多数这些光变曲线模型中，最强的简化之一是假设可以确定为喷出物的平均不透明度的恒定埃里克森散射不透明度。在这里，我们提出了一个系统的分析，以估计在不同类型的核心坍缩超新星（CCSNe），可以用来作为恒定的不透明度的喷出物在简化的半解析模型的平均不透明度。为了在光变曲线（LC）拟合过程中自洽地使用这些平均不透明度，我们从流体动力学模拟中估计它们的值。在这项分析中，我们首先生成具有不同物理参数（初始质量，金属丰度，旋转）的MESA（Paxton et al. 2011，2013，2015，2018）恒星模型，这些参数决定了模型恒星的质量损失历史。然后，我们使用SNEC流体动力学代码（Morozova等人，2015）从这些模型合成SN LC，并计算每个质量元素中的Rosseland平均不透明度。最后，我们通过积分这些Rosseland平均不透明度来计算平均不透明度。因此，我们发现，平均不透明度从我们的计算显示出足够的协议，在以前的研究中通常使用的不透明度。
