SN爆炸引发的恒星形成的勘误：对$β$ Pictuary星协的应用
Erratum to Star formation triggered by SN explosions: an application to the stellar association of $β$Pictoris
摘要：
在目前的研究中，考虑到物理条件是相关的超新星遗迹（SNRs）和致密的分子云之间的相互作用，触发恒星形成，我们已经建立了一个图的SNR半径与云密度在上面的限制划定一个阴影区，恒星形成是允许的。我们还进行了全三维辐射冷却数值模拟的影响之间的SNR和云在不同的初始条件下，以遵循这些相互作用的初始步骤。我们确定的条件，可能会导致云崩溃和恒星形成或完全云破坏，发现数值结果是一致的SNR云密度图。最后，我们将上述结果应用于$β-$风景如画的恒星协会，它是由低质量的后T金牛星的年龄为11万年。最近有人提出，它的形成可能是由一个SN爆炸产生的冲击波触发的，该爆炸发生在距离约62 pc的下半人马座Crux（LCC）或上半人马座Lupus（UCL），这两个地方都是该协会的较老的亚群附近（奥尔特加和同事）利用上述分析的结果，我们已经表明，在所提出的距离处，所建议的年轻缔合物的起源仅在母分子的初始条件的非常有限的范围内是合理的。云，即，一种半径为10 pc量级、密度为10 $-$ 20 cm $^{-3}$量级、温度为10 $-$ 100 K }量级的云。
英文摘要：
In the present study, considering the physical conditions that are relevant interactions between supernova remnants (SNRs) and dense molecular clouds for triggering star formation we have built a diagram of SNR radius versus cloud density in which the constraints above delineate a shaded zone where star formation is allowed. We have also performed fully 3-D radiatively cooling numerical simulations of the impact between SNRs and clouds under different initial conditions in order to follow the initial steps of these interactions. We determine the conditions that may lead either to cloud collapse and star formation or to complete cloud destruction and find that the numerical results are consistent with those of the SNR-cloud density diagram. Finally, we have applied the results above to the $β-$ Pictoris stellar association which is composed of low mass Post-T Tauri stars with an age of 11 Myr. It has been recently suggested that its formation could have been triggered by the shock wave produced by a SN explosion localized at a distance of about 62 pc that may have occurred either in the Lower Centaurus Crux (LCC) or in the Upper Centaurus Lupus (UCL) which are both nearby older subgroups of that association (Ortega and co-workers).Using the results of the analysis above we have shown that the suggested origin for the young association at the proposed distance is plausible only for a very restricted range of initial conditions for the parent molecular cloud, i.e., a cloud with a radius of the order of 10 pc, a density of the order of 10$-$20 cm$^{-3}$, and a temperature of the order of 10$-$100 K }.
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