The deposition of energy and momentum by supernova explosions has been subject to numerous studies in the past few decades. However, while there has been some work that focused on the transition from the adiabatic to the radiative stage of a supernova remnant (SNR), the late radiative stage and merging with the interstellar medium (ISM) have received little attention. Here, we use three-dimensional, hydrodynamic simulations, focusing on the evolution of SNRs during the radiative phase, considering a wide range of physical explosion parameters ( nH,ISM∈0.1,100cm−3 and ESN∈1,14×1051erg ). We find that the radiative phase can be subdivided in four stages: A pressure-driven snowplow phase, during which the hot overpressurized bubble gas is evacuated and pushed into the cold shell; a momentum-conserving snowplow phase that is accompanied by a broadening of the shell; an implosion phase where cold material from the back of the shell is flooding the central vacuum; and a final cloud phase, during which the imploding gas is settling as a central, compact overdensity. The launching timescale for the implosion ranges from a few 100 kyr to a few Myr, while the cloud formation timescale ranges from a few to about 10 Myr. The highly chemically enriched clouds can become massive (M _cl ∼ 10³–10⁴ M _⊙) and self-gravitating within a few Myr after their formation, providing an attractive, novel pathway for supernova-induced star and planet formation in the ISM.

中文翻译：

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超新星内爆形成的云

在过去的几十年里，超新星爆炸引起的能量和动量的沉积受到了大量的研究。然而，虽然已经有一些工作重点关注超新星遗迹从绝热阶段到辐射阶段的转变（SNR），但晚期辐射阶段和与星际介质的合并（ISM）却很少受到关注。在这里，我们使用三维流体动力学模拟，重点关注辐射阶段信噪比的演变，并考虑各种物理爆炸参数（ nH,主义ε0.1,100厘米-3 和 乙序列号ε1,14×1051尔格 ）。我们发现辐射阶段可以细分为四个阶段：压力驱动的扫雪阶段，在此期间热的超压气泡气体被排出并推入冷壳中；动量守恒的扫雪阶段，伴随着壳体的扩大；内爆阶段，来自外壳后部的冷物质淹没中央真空；最后的云相，在此期间内爆气体沉降为中心、致密的超密度。内爆的启动时间范围从几百基尔到几马里尔，而云形成的时间范围从几马里尔到大约十马里尔。高度化学浓缩的云可能变得巨大（中号 _cl ~ 10 ³ –10 ⁴ 中号 _⊙ ) 并在形成后几密尔范围内产生自引力，为 ISM 中超新星引发的恒星和行星形成提供了一条有吸引力的、新颖的途径。