扩展核素图的东北界限
Extending the north-east limit of the chart of nuclides
摘要：
具有质子和中子的奇异组合的原子核的存在提供了关于核子之间作用力的基本信息。给定数量的质子所能结合的最大中子数，即中子滴线1，只知道最轻的化学元素，直到氧。对于较重的元素，它的原子序数越大，离这个极限越远，是已知的中子最丰富的同位素。重富中子核的性质也对理解我们宇宙中比铁重的化学元素的观测丰度有直接影响。这些元素丰度的一半以上被认为是在快速中子俘获反应中产生的，r-过程发生在剧烈的恒星星云2中，那里产生的重富中子核远远超过今天已知的核。在这里，我们提出了一个重大的一步，在生产重丰中子核：发现了73个新的富中子同位素的化学元素之间的钽（Z=72）和锕（Z=89）。这一结果证明，在相对论能量下的冷碎裂反应3受同位旋和能量耗散的大波动控制，使得大量产生重丰中子核成为可能，从而为全面了解我们宇宙中较重元素的起源铺平了道路。预计进一步的研究提供的基础和结构特性的核在这里提出将揭示进一步的细节沿Z=82和N=126的核壳演化，但也对周围的恒星nucleosynthitis r-过程的理解等待点在A~190定义的速度的物质流向较重的裂变核。
英文摘要：
The existence of nuclei with exotic combinations of protons and neutrons provides fundamental information on the forces acting between nucleons. The maximum number of neutrons a given number of protons can bind, neutron drip line1, is only known for the lightest chemical elements, up to oxygen. For heavier elements, the larger its atomic number, the farther from this limit is the most neutron-rich known isotope. The properties of heavy neutron-rich nuclei also have a direct impact on understanding the observed abundances of chemical elements heavier than iron in our Universe. Above half of the abundances of these elements are thought to be produced in rapid-neutron capture reactions, r-process, taking place in violent stellar scenarios2 where heavy neutron-rich nuclei, far beyond the ones known up today, are produced. Here we present a major step forward in the production of heavy neutron-rich nuclei: the discovery of 73 new neutron-rich isotopes of chemical elements between tantalum (Z=72) and actinium (Z=89). This result proves that cold-fragmentation reactions3 at relativistic energies are governed by large fluctuations in isospin and energy dissipation making possible the massive production of heavy neutron-rich nuclei, paving then the way for the full understanding of the origin of the heavier elements in our Universe. It is expected that further studies providing ground and structural properties of the nuclei presented here will reveal further details on the nuclear shell evolution along Z=82 and N=126, but also on the understanding of the stellar nucleosyntheis r-process around the waiting point at A~190 defining the speed of the matter flow towards heavier fissioning nuclei.
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