评价Ia型超新星的系统演化：中心密度的影响
Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Central Density
摘要：
我们提出了一项研究，探索系统的影响Ia型超新星的亮度，采用数值模型，假设单简并范式。我们的研究改变了火焰点燃时的前身白矮星的中心密度，并考虑了它对爆炸产额的影响，特别是放射性Ni-56的产生和分布，它为光变曲线提供动力。我们进行了一系列随机初始条件的二维模拟，使我们能够描述我们呈现的统计趋势。模拟结果表明，铁族物质的产生在统计上与原始中心密度无关，但稳定的铁族同位素的质量与中心密度密切相关，在较高的中心密度下，Ni-56的产生减少。这些结果意味着具有较高中心密度的祖细胞产生较暗的事件。我们提供了爆炸后的镍-56的模型中的分布的细节，包括缺乏一个一致的中心定位的赤字的镍-56，这可能是比较观察到的残留物。通过对我们的模型产量进行自洽外推，并考虑到祖先恒星的主序星寿命和白矮星形成和吸积开始之间的时间，我们开发了一个亮度-年龄关系，提高了我们对单简并的预期趋势的预测，并将这种关系与观测进行了比较。
英文摘要：
We present a study exploring a systematic effect on the brightness of type Ia supernovae using numerical models that assume the single-degenerate paradigm. Our investigation varied the central density of the progenitor white dwarf at flame ignition, and considered its impact on the explosion yield, particularly the production and distribution of radioactive Ni-56, which powers the light curve. We performed a suite of two-dimensional simulations with randomized initial conditions, allowing us to characterize the statistical trends that we present. The simulations indicate that production of Fe-group material is statistically independent of progenitor central density, but the mass of stable Fe-group isotopes is tightly correlated with central density, with a decrease in the production of Ni-56 at higher central densities. These results imply progenitors with higher central densities produce dimmer events. We provide details of the post-explosion distribution of Ni-56 in the models, including the lack of a consistent centrally-located deficit of Ni-56, which may be compared to observed remnants. By performing a self-consistent extrapolation of our model yields and considering the main-sequence lifetime of the progenitor star and the elapsed time between the formation of the white dwarf and the onset of accretion, we develop a brightness-age relation that improves our prediction of the expected trend for single degenerates and we compare this relation with observations.
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