Nuclear structure studies for the astrophysical r-process

Collectivity evolution in the neutron-rich Pd isotopes toward theN=82shell closure

“…of the N = 82 shell closure has attracted much attention due to its relation to the nucleosynthesis in the rapid neutron capture process (r process) [10]. While 132 Sn is known to exhibit typical characteristics of a doubly magic nucleus, such as a high-lying first excited state [11] and a sudden drop in neutron separation energy for the neighboring, heavier isotope [12]; the structure of more proton-deficient nuclei is poorly known.…”

The Hamburg/ESO R-process enhanced star survey (HERES)

“…The parameters of r-process models therefore had to be defined site-independently; they were nevertheless able to reproduce observed abundance patterns of heavy neutron-capture elements in the Sun and metalpoor stars (see, e.g., papers by Kratz et al 1993;Pfeiffer et al 2001;Wanajo et al 2002;and Kratz et al 2007). Recent studies showed that lighter elements such as strontium, yttrium and zirconium exhibit more complex behavior, which cannot be explained in a simple r-process scenario.…”

Identification of shell-model states inSb135populated viaβ−decay ofShergur1, Cederkäll2 2005Phys. Rev. CSelf Cite

“…Study of the structures and decay of Ag, Cd, In, Sn, Sb, and Te nuclides with 125 < A < 140 have taken on new importance in recent years owing to the vital role that these properties play in r-process nucleosynthesis calculations [1]. Data for nuclides in this mass region that lie directly in the r-process path are essential for such calculations, and also serve to test models that must be used to describe nuclides not yet accessible to experimental measurements.…”