论文标题
祖细胞半径测量值对II型 - 帕拉托超新星的爆炸建模的值
The Value of Progenitor Radius Measurements for Explosion Modeling of Type II-Plateau Supernovae
论文作者
论文摘要
使用模块进行恒星天体物理学（MESA）+Stella的实验，我们表明非常不同的物理模型可以充分再现特定的观察到的II型II-Plateau Supernova（SN）。我们考虑使用SN2004A，SN2004ET，SN2009IB，SN2017EAW和SN2017GMR，镍含量（$ M_ \ Mathrm {ni}> 0.03m_ \ odot $），带有降低灯泡的事件，并从Plack中降低了降低。这些事件还通过祖细胞图像或SN2017GMR对祖细胞半径有限制，这是拟合减震模型的半径。 In general, many explosions spanning the parameter space of progenitors can yield excellent lightcurve and Fe line velocity agreement, demonstrating the success of scaling laws in motivating models which match plateau properties for a given radius and highlighting the degeneracy between plateau luminosity and velocity in models and observed events, which can span over 50% in ejecta mass, radius, and explosion energy.这可以帮助解释使用不同模型计算在同一事件报告的爆炸属性中的分歧。我们的计算与预探索前祖细胞半径测量结果或对材料的最外部$ <0.1 \，m_ \ odot $相结合时产生爆炸特性，这些理解是在爆炸后几天从SN观测中量化祖细胞半径的材料的M_ \ odot $。
Using Modules for Experiments in Stellar Astrophysics (MESA)+STELLA, we show that very different physical models can adequately reproduce a specific observed Type II-Plateau Supernova (SN). We consider SN2004A, SN2004et, SN2009ib, SN2017eaw, and SN2017gmr, Nickel-rich ($M_\mathrm{Ni}>0.03M_\odot$) events with bolometric lightcurves and a well-sampled decline from the plateau. These events also have constraints on the progenitor radius, via a progenitor image, or, in the case of SN2017gmr, a radius from fitting shock-cooling models. In general, many explosions spanning the parameter space of progenitors can yield excellent lightcurve and Fe line velocity agreement, demonstrating the success of scaling laws in motivating models which match plateau properties for a given radius and highlighting the degeneracy between plateau luminosity and velocity in models and observed events, which can span over 50% in ejecta mass, radius, and explosion energy. This can help explain disagreements in explosion properties reported for the same event using different model calculations. Our calculations yield explosion properties when combined with pre-explosion progenitor radius measurements or a robust understanding of the outermost $<0.1\,M_\odot$ of material that quantifies the progenitor radius from SN observations a few days after explosion.
