标题： 超新星爆炸在结构化和电离分子云中的能量和动量输入 显示英文标题

标题： The energy and momentum input of supernova explosions in structured and ionised molecular clouds

摘要： 我们通过三维、高分辨率的流体动力学模拟研究了单次和双星超新星（SN）爆炸对致密气体云的早期影响。 测试了云结构、辐射冷却以及来自前身恒星的电离辐射对净动能输入 f_kin=E_kin/E_SN、热能输入 f_therm=E_therm/E_SN 和动量输入 f_P=P/P_SN 对星际介质（ISM）的影响。 对于密度 n=100 cm^{-3}的云，Sedov 阶段和压力驱动雪犁阶段的动量生成过程提前终止（~0.01 Myr），辐射冷却限制了耦合效率，使得 f_therm ~ 0.01，f_kin ~ 0.05，f_P ~ 9，远低于无冷却情况下的值。 对于预电离的云，这些数值仅增加约 50%，且与云结构无关。 这仅足以加速约 5% 的云到径向速度 >30 km/s。 如果第二次超新星延迟到第一次爆炸的 Sedov 阶段之后，可能会进一步提高耦合效率。 如此低的耦合效率对许多基于星系尺度的超新星反馈亚网格模型提出了质疑，其中大多数模型是事后通过星系属性与观测的定性一致性验证的。 电离辐射似乎并未显著增强超新星与周围气体的即时耦合，因为它将星际介质推向惰性密集壳层和冷团块，这一过程在星系尺度的模拟中未被解析。 我们的结果支持了先前的结论，即超新星可能仅在相当大比例在低密度环境中爆炸或由电离辐射以外的过程支持时才能驱动风。 显示英文摘要

摘要： We investigate the early impact of single and binary supernova (SN) explosions on dense gas clouds with three-dimensional, high-resolution, hydrodynamic simulations. The effect of cloud structure, radiative cooling, and ionising radiation from the progenitor stars on the net input of kinetic energy, f_kin=E_kin/E_SN, thermal energy, f_therm=E_therm/E_SN, and gas momentum f_P=P/P_SN to the interstellar medium (ISM) is tested. For clouds with n=100 cm^{-3}, the momentum generating Sedov and pressure-driven snowplough phases are terminated early (~ 0.01 Myr) and radiative cooling limits the coupling to f_therm ~ 0.01, f_kin ~ 0.05, and f_P ~ 9, significantly lower than for the case without cooling. For pre-ionised clouds these numbers are only increased by ~ 50%, independent of the cloud structure. This only suffices to accelerate ~ 5% of the cloud to radial velocities >30km/s. A second SN might further enhance the coupling efficiencies if delayed past the Sedov phase of the first explosion. Such very low coupling efficiencies cast doubts on many galaxy-scale sub-resolution models for supernova feedback, most of which are validated a posteriori by qualitative agreement of galaxy properties with observations. Ionising radiation appears not to significantly enhance the immediate coupling of SNe to the surrounding gas as it drives the ISM into inert dense shells and cold clumps, a process which is unresolved in galaxy scale simulations. Our results support previous conclusions that supernovae might only drive a wind if a significant fraction explodes in low-density environments or if they are supported by processes other than ionising radiation.