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Abstract: We consider the effect of a supernova SN explosion in a very massive binarythat is expected to form in a portion of Population III stars with the masshigher than 100$M \odot$. In a Population III binary system, a more massivestar can result in the formation of a BH and a surrounding accretion disc. SuchBH accretion could be a significant source of the cosmic reionization in theearly universe. However, a less massive companion star evolves belatedly andeventually undergoes a SN explosion, so that the accretion disc around a BHmight be blown off in a lifetime of companion star. In this paper, we explorethe dynamical impact of a SN explosion on an accretion disc around a massiveBH, and elucidate whether the BH accretion disc is totally demolished or not.For the purpose, we perform three-dimensional hydrodynamic simulations of avery massive binary system, where we assume a BH of $10^3 M {\odot}$ thatresults from a direct collapse of a very massive star and a companion star of$100 M {\odot}$ that undergoes a SN explosion. We calculate the remaining massof a BH accretion disc as a function of time. As a result, it is found that asignificant portion of gas disc can survive through three-dimensionalgeometrical effects even after the SN explosion of a companion star. Even ifthe SN explosion energy is higher by two orders of magnitude than the bindingenergy of gas disc, about a half of disc can be left over. The results implythat the Population III BH accretion disc can be a long-lived luminous source,and therefore could be an important ionizing source in the early universe.



Autor: Jun'ichi Sato, Masayuki Umemura, Keisuke Sawada

Fuente: https://arxiv.org/







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