Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and Be Injected into the Early Interstellar Medium?
Evolution of Dust in Primordial Supernova Remnants: Can Dust Grains Formed in the Ejecta Survive and Be Injected into the Early Interstellar Medium?
复制标题
DOI：
10.1086/520621
复制
发表时间：
2007-06
期刊：
影响因子：
--
通讯作者：
T. Nozawa;T. Kozasa;A. Habe;E. Dwek;H. Umeda;N. Tominaga;K. Maeda;K. Nomoto
中科院分区：
文献类型：
--
作者：
T. Nozawa;T. Kozasa;A. Habe;E. Dwek;H. Umeda;N. Tominaga;K. Maeda;K. Nomoto
我们研究了在第三族超新星(SN)爆炸中形成的尘埃的演化，以及通过超新星喷出物与周围介质相互作用而产生的反向激波与碰撞的过程。特别是，我们研究了冲击尘埃在SNR内的传输及其对SNR中尘埃的化学成分、粒度分布和存活总质量的影响。我们发现，反向激波的演化，以及它对尘埃处理的影响，取决于前驱恒星保留的包层厚度。此外，尘埃粒子的输运和存活依赖于它们的初始半径、AINI和组成：对于扩展到密度为NH，0=1 cm-3的ISM的II型SNR，AINI≲为0.0 5μm的小粒子在激波后流中被溅射完全摧毁，而AINI=0.0 5-0.2μm的粒子被困在正激波后的致密壳层中。在没有明显减小尺寸的情况下，非常大的AlI≳0.2μm颗粒被喷射到ISM中。我们发现，被反向激波摧毁的尘埃的总质量分数从0.2到1.0，这取决于爆炸的能量和周围ISM的密度。我们的计算结果对形成在原始SNR致密壳层中的第二代恒星的丰度模式有重大影响。
We investigate the evolution of dust that formed at Population III supernova (SN) explosions and its processing through the collisions with the reverse shocks resulting from the interaction of the SN ejecta with the ambient medium. In particular, we investigate the transport of the shocked dust within the SNR and its effect on the chemical composition, the size distribution, and the total mass of dust surviving in SNRs. We find that the evolution of the reverse shock, and hence its effect on the processing of the dust, depends on the thickness of the envelope retained by the progenitor star. Furthermore, the transport and survival of the dust grains depend on their initial radius, aini, and composition: for Type II SNRs expanding into the ISM with a density of nH,0 = 1 cm-3, small grains with aini ≲ 0.05 μm are completely destroyed by sputtering in the postshock flow, while grains with aini = 0.05-0.2 μm are trapped into the dense shell behind the forward shock. Very large grains of aini ≳ 0.2 μm are ejected into the ISM without decreasing their sizes significantly. We find that the total mass fraction of dust that is destroyed by the reverse shock ranges from 0.2 to 1.0, depending on the energy of the explosion and the density of the ambient ISM. The results of our calculations have significant impact on the abundance pattern of the second-generation stars that form in the dense shell of primordial SNRs.