2016 CAP Congress / Congrès de l'ACP 2016

Session

M3-1 Nuclear Astrophysics (DNP) / Astrophysique nucléaire (DPN)

M3-1

13 Jun 2016, 15:45

University of Ottawa

Conveners

M3-1 Nuclear Astrophysics (DNP) / Astrophysique nucléaire (DPN)

• Barry Davids (TRIUMF)

985. Neutron star mergers: neutrino emission and nucleosynthesis

Olga Caballero

13/06/2016, 15:45

Nuclear Physics / Physique nucléaire (DNP-DPN)

Invited Speaker / Conférencier invité

Neutron-star binary mergers are interesting for several reasons: they are proposed as the progenitors of short gamma-ray bursts, they have been speculated to be a site for the synthesis of heavy elements, and they emit gravitational waves possibly detectable at terrestrial facilities. Our current understanding of the merger evolution and the production of new elements is linked to details of...

1046. Constraining neutron capture rates far from stability and astrophysical implications

Artemis Spyrou (Michigan State University)

13/06/2016, 16:15

Nuclear Physics / Physique nucléaire (DNP-DPN)

Invited Speaker / Conférencier invité

The astrophysical r-process is responsible for the synthesis of about half of the isotopes of the heavy elements. Despite its well-known role in nucleosythesis, the astrophysical site where it takes place has not been unambiguously determined. Efforts for the better understanding of this important process span across many fields, from astronomical observations of metal-poor stars, and modeling...

1152. **WITHDRAWN** Phase-imaging mass measurements with the Canadian Penning trap mass spectrometer

Rodney Orford (McGill University)

13/06/2016, 16:45

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral (Student, In Competition) / Orale (Étudiant(e), inscrit à la compétition)

Roughly half of the elements heavier than iron are thought to be produced through the astrophysical rapid-neutron capture process of nucleosynthesis. Despite its large influence in explaining the observed abundance of heavy elements, much of the *r* process is still poorly understood. A more thorough library of nuclear data, particularly masses, of neutron-rich nuclei is needed to improve the...

1224. Decay Spectroscopy of Neutron-Rich Cd Around the N = 82 Shell Closure

Nikita Bernier (TRIUMF)

13/06/2016, 17:00

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral (Student, In Competition) / Orale (Étudiant(e), inscrit à la compétition)

The neutron-rich region around A = 132 is of special interest for nuclear astrophysics and nuclear structure. From an astrophysics perspective, this region is connected with the second r-process abundance peak at A$\approx$130 and the waiting-point nuclei around N = 82. For nuclear structure studies, the neighbours of the doubly-magic ${}^{132}$Sn (Z = 50, N = 82) are an ideal test ground for...