Now 50 years since the existence of the neutron star crust was proposed, we review the
current understanding of the nuclear physics of the outer layers of accreting neutron stars …

To a high degree many aspects of the large-scale behavior of objects in the Universe are
governed by the underlying nuclear physics. In fact the shell structure of nuclear physics is …

Type-I X-ray bursts can be used to determine properties of accreting neutron stars via
comparisons between model calculations and astronomical observations, exploiting the …

The rate of the final step in the astrophysical α p process, the Ar 34 (α, p) K 37 reaction,
suffers from large uncertainties due to a lack of experimental data, despite having a …

The Ar 34 (α, p) K 37 reaction is believed to be one of the last in a sequence of (α, p) and (p,
γ) reactions within the T z=− 1, sd-shell nuclei, known as the α p-process. This process is …

Nuclear processes not only generate the energy and drive the evolution of stars, but also are
responsible for the synthesis of the elements in the Universe. Helium (4 He, or α) is the …

The S 30 (α, p) Cl 33 reaction has been identified in several type-1 x-ray burst (XRB)
sensitivity studies as a significant reaction within the α p process, possibly influencing not …

A multihit capacity setup was used to study the decay of the dripline nucleus 31 Ar, produced
at the ISOLDE facility at CERN. A spectroscopic analysis of the β-delayed three-proton …

Resonances just above the proton threshold in 30 S affect the 29 P (p, γ) 30 S reaction
under astrophysical conditions. The (p, γ)-reaction rate is currently determined indirectly and …

We present results for levels in 30 S (the mirror nucleus of 30 Si) that are used for the 29 P
(p, γ) rp reaction rate calculations. The resonance energies used in the reaction rate …