arXiv 1602.027742016-02astro-ph.HE

II型超新星的祖先和从总发射光的喷出物性质，ET

Type II supernovae progenitor and ejecta properties from the total emitted light, ET

Tomer Shussman, Ehud Nakar, Roni Waldman, Boaz Katz

备注：: 10 pages, 9 figures

摘要：

最近的研究表明，II型超新星（SNe）的热光变曲线允许在同源膨胀的早期阶段（$t\lesssim 10d$），对喷出物中的辐射能量$E_r$和爆炸后的时间$t$的乘积进行准确和可靠的测量。这个观测值，在这里表示为$ET \equiv E_rt$，在这段时间内是恒定的，只取决于原始结构和爆炸能量。我们使用1D流体动力学代码来找到$ET$的模拟爆炸的145红超巨星的祖先使用恒星演化代码MESA获得的，并与此可观察到的祖和爆炸能量的属性。我们发现，$ET$探测器的信封（速度，质量和初始结构）的属性，类似于其他观测依赖于光球相位发射。然而，对于包线支配喷射质量$M_{env}/M_{ej} \gtrsim 0.6$的爆炸，$ET$通过关系式$ET \approx 0.15 E_{exp}^{1/2} R_* M_{ej}^{1/2}$与爆炸能量$E_{exp}$和喷射质量$M_{ej}$直接相关，其中$R_*$是原始半径，其精确度优于$30\%$。我们还提供了$ET$和包络属性之间的关系，这些属性对于我们样本中的所有祖细胞都是准确的（在20%以内），包括那些丢失了大部分包络的祖细胞。我们表明，当包络线速度可以合理地测量所观察到的光谱中的线位移，包络线是直接从测热光变曲线（独立的$E_{exp}$）的约束。我们用它来比较观测的11 SNe与测量的$ET$和包络速度，我们的样本的数值祖先。这种比较表明，许多SNe祖细胞具有$\lesssim 500~R_\odot$的半径。在我们的模拟框架中，这表明，最有可能的是，一个相当高的值的混合长度参数。

英文摘要：

It was recently shown that the bolometric light curves of type II supernovae (SNe) allow an accurate and robust measurement of the product of the radiation energy in the ejecta, $E_r$, and the time since the explosion, $t$, at early phases ($t\lesssim 10d$) of the homologous expansion. This observable, denoted here $ET \equiv E_rt$ is constant during that time and depends only on the progenitor structure and explosion energy. We use a 1D hydrodynamic code to find $ET$ of simulated explosions of 145 red supergiant progenitors obtained using the stellar evolution code MESA, and relate this observable to the properties of the progenitor and the explosion energy. We show that $ET$ probes only the properties of the envelope (velocity, mass and initial structure), similarly to other observables that rely on the photospheric phase emission. Nevertheless, for explosions where the envelope dominates the ejected mass, $M_{env}/M_{ej} \gtrsim 0.6$, $ET$ is directly related to the explosion energy $E_{exp}$ and ejected mass $M_{ej}$ through the relation $ET \approx 0.15 E_{exp}^{1/2} R_* M_{ej}^{1/2}$, where $R_*$ is the progenitor radius, to an accuracy better than $30\%$. We also provide relations between $ET$ and the envelope properties that are accurate (to within 20\%) for all the progenitors in our sample, including those that lost most of their envelope. We show that when the envelope velocity can be reasonably measured by line shifts in observed spectra, the envelope is directly constrained from the bolometric light curve (independent of $E_{exp}$). We use that to compare observations of 11 SNe with measured $ET$ and envelope velocity to our sample of numerical progenitors. This comparison suggests that many SNe progenitors have radii that are $\lesssim 500~R_\odot$. In the framework of our simulations this indicates, most likely, a rather high value of the mixing length parameter.

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