A spectral synthesis code for rapid modelling of supernovae
A spectral synthesis code for rapid modelling of supernovae
复制标题
用于超新星快速建模的光谱合成代码
DOI：
10.1093/mnras/stu055
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发表时间：
2014
影响因子：
4.8
通讯作者：
S. Sim
中科院分区：
文献类型：
--
作者：
W. E. Kerzendorf;S. Sim
我们提出了TARDIS -一个开源代码的超新星（SNe）的快速光谱建模。我们的目标是开发一种工具，是足够快，允许探索复杂的参数空间的模型SN喷出物。这可用于分析瞬变测量获得的越来越多的高质量SN光谱。该代码使用蒙特卡罗方法来获得自洽的描述等离子体状态，并计算合成光谱。它有一个模块化的设计，以促进一系列的物理近似的实施，可以进行比较，以评估准确性和计算方便。这将允许用户选择适合其应用的复杂程度。在这里，我们描述了代码的操作，并与不同复杂程度的替代辐射传输代码（SYN++，PYTHON和ARTIS）进行比较。然后，我们探讨采用简单的处方计算原子激发的后果，专注于四个物种的相关Ia型超新星光谱-硅II，S II，镁II，钙II。我们还研究了三种方法治疗线相互作用对我们的合成光谱的影响，并需要在我们的计划准确的辐射率估计。
We present TARDIS - an open-source code for rapid spectral modelling of supernovae (SNe). Our goal is to develop a tool that is sufficiently fast to allow exploration of the complex parameter spaces of models for SN ejecta. This can be used to analyse the growing number of high-quality SN spectra being obtained by transient surveys. The code uses Monte Carlo methods to obtain a self-consistent description of the plasma state and to compute a synthetic spectrum. It has a modular design to facilitate the implementation of a range of physical approximations that can be compared to asses both accuracy and computational expediency. This will allow users to choose a level of sophistication appropriate for their application. Here, we describe the operation of the code and make comparisons with alternative radiative transfer codes of differing levels of complexity (SYN++, PYTHON, and ARTIS). We then explore the consequence of adopting simple prescriptions for the calculation of atomic excitation, focussing on four species of relevance to Type Ia supernova spectra - Si II, S II, Mg II, and Ca II. We also investigate the influence of three methods for treating line interactions on our synthetic spectra and the need for accurate radiative rate estimates in our scheme.
影响因子：
4.8
作者：
I. Seitenzahl;F. Ciaraldi-Schoolmann;F. Roepke;M. Fink;W. Hillebrandt;M. Kromer;R. Pakmor;A. Ruiter-A
通讯作者：
I. Seitenzahl;F. Ciaraldi-Schoolmann;F. Roepke;M. Fink;W. Hillebrandt;M. Kromer;R. Pakmor;A. Ruiter-A