论文标题
放射线项目
The RADIOSTAR Project
论文作者
论文摘要
放射性核是理解我们太阳诞生情况的关键，因为气象分析已证明当时有许多存在。然而，到目前为止，他们的起源一直难以捉摸。 ERC-COG-2016 RadioStar项目致力于通过恒星内部的核反应，它们在银河系中的发展以及它们在分子云中的存在来研究放射性核的产生。 So far, we have discovered that: (i) radioactive nuclei produced by slow ($^{107}$Pd and $^{182}$Hf) and rapid ($^{129}$I and $^{247}$Cm) neutron captures originated from stellar sources - asymptotic giant branch (AGB) stars and compact binary mergers, respectively - within the galactic environment that早于太阳出生的分子云的形成。 （ii）从云到太阳的诞生的时间为10 $^7 $年，（iii）非常短的核$^{26} $ al，$^{36} $ cl，$^{36} $ cl，以及$^{41} $可以在单个或by的系统中进行大规模的STAR SYRESS，如果这些系统可以直接在单个或Bely Systems中进行宣传，如果这些系统的频道是频繁的。 Our current and future work, as required to finalise the picture of the origin of radioactive nuclei in the Solar System, involves studying the possible origin of radioactive nuclei in the early Solar System from core-collapse supernovae, investigating the production of $^{107}$Pd in massive star winds, modelling the transport and mixing of radioactive nuclei in the galactic and molecular cloud medium, and calculating the galactic chemical $^{53} $ MN和$^{60} $ fe的演变以及P-Process同位素$^{92} $ nb和$^{146} $ sm。
Radioactive nuclei are the key to understanding the circumstances of the birth of our Sun because meteoritic analysis has proven that many of them were present at that time. Their origin, however, has been so far elusive. The ERC-CoG-2016 RADIOSTAR project is dedicated to investigating the production of radioactive nuclei by nuclear reactions inside stars, their evolution in the Milky Way Galaxy, and their presence in molecular clouds. So far, we have discovered that: (i) radioactive nuclei produced by slow ($^{107}$Pd and $^{182}$Hf) and rapid ($^{129}$I and $^{247}$Cm) neutron captures originated from stellar sources - asymptotic giant branch (AGB) stars and compact binary mergers, respectively - within the galactic environment that predated the formation of the molecular cloud where the Sun was born; (ii) the time that elapsed from the birth of the cloud to the birth of the Sun was of the order of 10$^7$ years, and (iii) the abundances of the very short-lived nuclei $^{26}$Al, $^{36}$Cl, and $^{41}$Ca can be explained by massive star winds in single or binary systems, if these winds directly polluted the early Solar System. Our current and future work, as required to finalise the picture of the origin of radioactive nuclei in the Solar System, involves studying the possible origin of radioactive nuclei in the early Solar System from core-collapse supernovae, investigating the production of $^{107}$Pd in massive star winds, modelling the transport and mixing of radioactive nuclei in the galactic and molecular cloud medium, and calculating the galactic chemical evolution of $^{53}$Mn and $^{60}$Fe and of the p-process isotopes $^{92}$Nb and $^{146}$Sm.
