Nuclear Astrophysics at TRIUMF-ISAC: Stellar Burning Reaction Studies with DRAGON and TUDA

目前公认的是，恒星中大多数比硼更重的化学元素是通过稳定的放射性原子核和放射性衰变的核反应而产生的。有助于这种核合成的恒星演化不同阶段的天体物理模型(例如，新星和超新星中看到的静止燃烧或爆炸过程)最近变得更加先进，使得能够很好地预测天文可观测对象。例如，冻结在组成太阳系的尘埃颗粒中的同位素丰度，合成的长寿命放射性核素的伽马射线通量，光学或X射线光度等。这些量可以与天文观测进行比较，包括来自轨道伽马射线观测站的观测或对流星颗粒的实验室测量。这种比较在天体物理学和宇宙学领域是一个强大的工具，为我们提供了最直接的恒星内部核过程及其爆炸的成像技术。为了改进模型，从而提高我们对这些强大而神秘的恒星事件的理解，需要对能量产生和核合成所涉及的核反应有一个精确的了解。

It is presently accepted that most of the chemical elements heavier than boron were produced in stars through nuclear reactions involving stable and radioactive nuclei and radioactive decays. Astrophysical models of the various stages of stellar evolution (e.g. quiescent burning, or explosive processes as seen in novae and supernovae) that contribute to this nucleosynthesis have recently become more advanced, enabling good predictions of astronomical observables. Examples of these are isotopic abundances frozen into dust grains that make up our solar system, gamma-ray fluxes from synthesized long-lived radionuclides, optical or x-ray luminosity etc. These quantities can be compared with astronomical observations, including those from orbiting gamma ray observatories or laboratory measurements on meteoric grains. This comparison is a powerful tool in the field of astrophysics and cosmology, giving us the most direct imaging technique of the nuclear processes inside stars and their explosions. In order to improve the models, and therefore advance our understanding of these powerful and mysterious stellar events, a precise knowledge of the nuclear reactions involved in energy generation and nucleosynthesis is required.