论文标题
辐射超新星残留物和超新星反馈
Radiative Supernova Remnants and Supernova Feedback
论文作者
论文摘要
超新星（SN）爆炸是通过动量输入来调节星系中恒星形成的主要反馈机制。我们以银河系的方式回顾了SNR在辐射阶段的观察结果，以验证单个SN爆炸的动量/能量注入的理论结果。对于七个SNR，我们可以观察到快速扩张的原子辐射外壳，我们表明，从HI 21 cm线观测中推断出的外壳动量在（0.5---4.5）$ \ times 10^5 $ $ M_ \ odot $ $ $ $ $ km $ km s $ s $^{ - 1} $。在两个SNR（W44和IC 443）中，还观察到具有与原子SNR壳相当的动量的震动分子气体。我们比较了这七个SNR的动量和动力/热能与1D和3D数值模拟的结果。基于观察的动量和动能与$ \ sim 10^{51} $ erg的SN爆炸中的预期动量/能量输入非常吻合。使用热能的数据/模型比较来限制初始爆炸能量，因此，由于辐射SNR的热/冷界面上的复杂物理，因此很难限制初始爆炸能量。我们讨论了复杂环境中SNR的这些全局参数的观察和理论不确定性和爆炸能量估计。
Supernova (SN) explosions are a major feedback mechanism regulating star formation in galaxies through their momentum input. We review the observations of SNRs in radiative stages in the Milky Way to validate the theoretical results on the momentum/energy injection from a single SN explosion. For seven SNRs where we can observe fast-expanding, atomic radiative shells, we show that the shell momentum inferred from HI 21 cm line observations is in the range of (0.5--4.5)$\times 10^5$ $M_\odot$ km s$^{-1}$. In two SNRs (W44 and IC 443), shocked molecular gas with momentum comparable to that of the atomic SNR shells has been also observed. We compare the momentum and kinetic/thermal energy of these seven SNRs with the results from 1D and 3D numerical simulations. The observation-based momentum and kinetic energy agree well with the expected momentum/energy input from an SN explosion of $\sim 10^{51}$ erg. It is much more difficult to use data/model comparisons of thermal energy to constrain the initial explosion energy, however, due to rapid cooling and complex physics at the hot/cool interface in radiative SNRs. We discuss the observational and theoretical uncertainties of these global parameters and explosion energy estimates for SNRs in complex environments.
