Presentation Materials
Understanding the equation of state (EOS) of asymmetric nuclear matter is of fundamental importance and underpins our knowledge of many aspects of nuclear physics and astrophysics. It governs the behaviour of cosmological events like of type II supernova explosions and neutron star mergers, and the properties neutron stars, as well as the characteristics of neutron rich nuclei and the process...
Nuclear physics research is at the dawn of a new era. After the Big Bang and billions years of evolution, the universe has provided us around 2000 nuclei. Based on the information from these nuclei, nuclear theory has been established in order to understand the structure of the nucleus. The steady progress over the past twenty years in the development of high intensity stable beams and of...
Halo nuclei are fascinating short-lived nuclear systems found near the driplines.
In standard reaction models, halo nuclei are usually described as an inert core with one or two weakly bound nucleons. However, some breakup data suggest that the dynamics of the reaction is influenced by the excitation of the core to its excited states in a significant way [1].
Halo-EFT has been shown to...
One of the yet unsettled problems in heavy-ion fusion near and below the barrier is the relative influence of nucleon transfer channels and couplings to collective modes on the cross sections. We recall two relevant papers [1] where that influence, and the moments of fusion-barrier distributions were investigated.
In this contribution, we present a new analysis of several systems, based on...
Beta-decaying, high-spin, spin-trap isomers have been observed in 96Y, 98Y and 100Y with half-lives ranging from 9 to 0.9 seconds [Ab08,Ch20,Si21]. However, in 102Y there are two beta-decaying states which have similar half lives (t 1/2 = 360(40) ms [Sh83] and 300(10) ms [Hi91]) and a small energy difference, making it difficult to measure their relative energy and to ascertain if the...
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