发表机构
Lebedev Physical Institute, Russian Academy of Sciences（列别捷夫物理研究所，俄罗斯科学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过一维球对称拉格朗日模拟，发现超新星抛射物中大于约0.3微米的尘埃颗粒可穿越激波波前，在低密度环境中以1-2千公里/秒高速扩散至40-90秒差距，影响星系盘尘埃输运。
AI 中文摘要
受探测到速度超过300 km/s的流星（Afanasiev等人，2007年）的启发，我们研究了在超新星（SN）抛射物自由膨胀阶段形成的尘埃颗粒如何保持其从诞生这些颗粒的气体中获得的高速。使用一维球对称拉格朗日方法，我们追踪了超新星抛射物与周围星际气体相互作用期间颗粒的动力学。我们发现，大于约0.3微米的颗粒可以穿过超新星前向激波波前并到达周围星际介质。它们被破坏的效率很低，因此其尺寸保持接近初始尺寸。在密度小于约1 cm^-3的弥漫星际气体中，大于约1微米的颗粒以约1-2千公里/秒的速度移动，并在数万年内从超新星起源处扩散到超过约40-90秒差距的距离。在致密环境中，颗粒的传播受到显著抑制：即使是大颗粒也不会扩散到超过当前超新星遗迹尺寸50%的距离。在质量较小的抛射物中，诞生于超新星抛射物核心边缘附近的颗粒到达更远的距离。因此，预计高速颗粒形成于该部分抛射物中，其质量小于超新星遗迹约3个太阳质量，并在密度小于约1 cm^-3的弥漫气体中演化。我们讨论了尘埃从星系盘向外输运的可能后果。
英文摘要
Motivated by the discovery of a meteor with velocity more than 300~km/s (Afanasiev et al. 2007) we study how dust grains formed in the supernova (SN) ejecta at its free-expansion phase can keep their high velocity obtained from the gas, where these grains were born. Using a one-dimensional spherically symmetric Lagrangian approach we follow the dynamics of grains during the interaction of a SN ejecta with the ambient interstellar gas. We found that grains larger $\sim 0.3~μ$m can cross the SN forward shock front and reach the ambient interstellar medium. They are destroyed inefficiently, thus, their sizes remain close to the initial ones. In a diffuse interstellar gas of density $\lesssim 1$ cm$^{-3}$ grains larger as $\gtrsim 1~μ$m move with velocity around $1-2$ thousand km/s and spread over distances exceeding $\sim 40-90$ pc from the SN origin within tens of kiloyears. In dense environment the propagation of grains is significantly suppressed: even large grains do not spread over distances greater than 50% of the current SN remnant size. Grains born close to the edge of the SN ejecta core in less-massive ejecta reach greater distances. Thus, high-velocity grains are expected to be formed in this part of the ejecta with mass lower than $\sim 3~M_\odot$ of the SN remnant evolving in a diffuse gas with density $\lesssim 1$ cm$^{-3}$. We discuss possible consequences for dust transport out from galactic disks.
Comments18 pages, 12 figures
Journal refAstrophysical Bulletin, 2026, Vol. 81, pp. 424-439
