2026 CAP Congress / Congrès de l'ACP 2026

Session

(DNP) M2-6 Nuclear Astrophysics | Astrophysique nucléaire (DPN)

M2-6

22 Jun 2026, 14:15

U. Ottawa - Learning Crossroads (CRX) Building

503. (α,n) reactions and the origin of the first r-process peak

Thanassis Psaltis (Saint Mary's University)

22/06/2026, 14:15

Nuclear Physics / Physique nucléaire (DNP-DPN)

Invited Speaker / Conférencier(ère) invité(e)

The origin of the heavy elements of the first r-process peak, between strontium and silver, observed in Galactic halo stars (limited-r stars) remains an open question [1]. Neutrino-driven winds of explosive environments, either neutron- (weak r-process/α-process) or proton-rich (νp-process) present a viable option. In this talk, I will discuss how we can distinguish between different...

530. Absolute cross section measurements for astrophysical reactions with the EMMA recoil mass spectrometer at TRIUMF

Dr Barry Davids (TRIUMF)

22/06/2026, 14:45

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral (Non-Student) / Orale (non-étudiant(e))

The transmission efficiency of the EMMA recoil mass spectrometer at TRIUMF has been measured to enable direct absolute cross section measurements of astrophysical reactions. I will describe the measurements, the mathematical models of the spectrometer acceptance as a function of angle and energy/charge derived from them, and some recent determinations of astrophysical reaction cross sections.

576. The 18O(α, γ)22Ne reaction measurement with DRAGON in inverse kinematics

Dhruval Shah (McMaster University)

22/06/2026, 15:00

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral Competition (Graduate Student) / Compétition orale (Étudiant(e) du 2e ou 3e cycle)

Have you ever wondered how all the elements we find here on Earth and in the universe were created? Nearly all naturally occurring elements are produced via nuclear reactions in the interiors of the stars. Half of the elements heavier than iron are synthesized in the slow neutron capture process (s-process), which occurs mainly in two astrophysical sites: asymptotic giant branch (AGB) stars...

654. Investigation of Decay Channels from the 6.15 MeV Resonance in ¹⁸Ne Using the ¹⁷F+p Reaction with ACTAR TPC

Fatima Aljarrah (University of Regina)

22/06/2026, 15:15

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral not-in-competition (Graduate Student) / Orale non-compétitive (Étudiant(e) du 2e ou 3e cycle)

Type I X-ray bursts and classical novae are powered by thermonuclear reactions on the surface of accreting compact objects, where breakout reactions from the hot CNO cycle play a critical role. One such reaction is ¹⁴O(α,p)¹⁷F, which at typical novae temperatures is dominated by a resonant state at Ex = 6.15 MeV in ¹⁸Ne. While the energy and spin of this resonance are well established, its...

692. Beta-Delayed Charged-Particle From 20Mg

Sydney Plante (University of Regina)

22/06/2026, 15:30

Nuclear Physics / Physique nucléaire (DNP-DPN)

Oral Competition (Graduate Student) / Compétition orale (Étudiant(e) du 2e ou 3e cycle)

One of the most important nuclear reactions in astrophysics is the 15O(α,γ)19Ne(p,γ)20Na reaction, which provides a possible breakout pathway from the hot CNO cycle in stars. Studying this reaction directly in the laboratory is challenging, instead, an indirect study using β-decay proton and α decays of 20Mg was recently performed at TRIUMF. The experiment used the Gamma-Ray Infrastructure for...