Data
Unveiling the engine of the Sun: the measurements of the pp-chain and CNO-cycle solar neutrinos with Borexino featuring Alessandra Carlotta Re (University of Milan, Italy) (Opens in a new window)
Hosted by Erin Good (Michigan State University)
The n-process in Core-Collapse Supernovae featuring Marco Pignatari (Konkoly Observatory) (Opens in a new window)
The n-process is a neutron-capture process activated in Core-Collapse Supernovae (CCSNe), when the Supernova shock is passing through the deepest He-rich layers of the massive star progenitor. The peak neutron density generated is typically larger than 1018 neutrons cm-3, and the dominant neutron source is the Ne22(alpha,n)Mg25 reaction where the Ne22 available was left in the ashes of the hydrostatic convective He shell.
The 18th Russbach School on Nuclear Astrophysics (Opens in a new window)
The 18th Russbach School on Nuclear Astrophysics will take place in the village of Rußbach am Paß Gschütt, southeast of Salzburg, Austria. The school dates will be from March 12 (arrival and registration) to March 18 (departure) 2023.
The Viability of Novae as Sources of Galactic Lithium featuring Alex Kemp (KU Leuven, Belgium) (Opens in a new window)
Understanding the behavior of white dwarfs in interacting binary systems is critical to determining the rates, distributions, and chemical contributions from transients such as novae and type Ia supernovae. In this talk I will be presenting results from my recent work on novae, which combines population synthesis (binary_c) and galactic chemical evolution modeling (OMEGA+).
Studying the origins of the heavy elements through neutron capture. Aaron Couture, LANL (Opens in a new window)
Understanding how the heavy elements came into being in the universe presents one of the greatest challenges in nuclear physics and astrophysics. For some time we have known that elements beyond iron on the periodic table must have been made through neutron-induced reactions, but the environments where they are made and what they can tell us about this history of our galaxy remain a mystery.
Neutron-upscattering enhancement of the triple-alpha process featuring Jack Bishop (Texas A&M University) (Opens in a new window)
Carbon is produced in stars mainly via the triple-alpha process where three helium nuclei fuse to form an excited state of carbon-12 known as the Hoyle state. This is a nuclear resonance (an excited form of a nucleus) that has properties that guide the rate that the triple alpha process takes place. Primarily, the key property is how often the Hoyle state is able to lose energy and end up in the ground state of carbon-12 – known as the radiative width.
Learning from cosmic gamma-ray spectroscopy featuring Roland Diehl (MPE, Germany) (Opens in a new window)
Gamma rays from nuclear lines are the most-direct astronomical messenger for the occurrence of nuclear reactions in cosmic sites, next to neutrinos.
Characteristic lines from radioactive decays have been measured with space-borne telescopes, most-recently with ESA’s INTEGRAL mission, for the isotopes 56Ni, 57Ni, 44Ti, 26Al, and 60Fe.
ICONS workshop 2019 - Investigating Crusts of Neutron Stars (Opens in a new window)
This is a CeNAM supported workshop that aims to bring together different areas of research that all involve studies of heated neutron star crusts. This includes observations of different manifestations of neutron stars, theoretical calculations and simulations, and nuclear experiments. One of the primary goals of this dedicated workshop is to have a facilitated discussion about the puzzling source of shallow crustal heating, and what observations/experiments/calculations are needed to move forward.