CaNPAN Jam 2024

Session

Morning

1 May 2024, 09:00

Auditorium (TRIUMF)

Conveners

Morning: Student Day

• Stephanie Ciccone (University of Guelph)
• Mallory Loria (University of Victoria/TRIUMF)

Morning: Day 2

• There are no conveners in this block

Morning

• There are no conveners in this block

Presentation materials

ISAC Experimental Facilities - Nuclear Astrophysics.pptx

9. Introduction & Opening Remarks

Mallory Loria (University of Victoria/TRIUMF), Stephanie Ciccone (University of Guelph)

01/05/2024, 09:00

10. Introduction to CaNPAN: Goals, Activities, Accomplishments and Future Plans

Falk Herwig (University of Victoria)

01/05/2024, 09:20

The Canadian Nuclear Physics for Astrophysics Network is bringing together the multiple disciplines needed to investigate the origin of the elements. The emphasis is on nuclear physics experiments and theory for astrophysics applications. For example, CaNPAN tries to investigate, as new astrophysics scenarios are developed in response to astronomical observations, what is the impact of nuclear...

11. Amanda Edwin: Direct Measurement of Resonance Properties of 23Mg(p,γ)24Al Reaction Occurring in Classical Novae using DRAGON Recoil Separator and an Optimized Array of BGO, LaBr and CeBr Gamma Ray Detectors

Amanda Edwin (Saint Mary's University)

01/05/2024, 10:00

One of the reactions that has an observable effect on classical nova nucleosynthesis is the proton capture on radioactive 23Mg, resulting in 24Al plus a γ. The 23Mg(p, γ)24Al has been investigated through a variety of experimental and theoretical means in the past. These investigations include a direct measurement of the strength and energy of the dominant resonance in this reaction, using a...

12. Maeve Cockshutt: Using Cool-Bottom Processing in RGB and AGB stars to explain Isotopic Ratios in Presolar Grains

Maeve Cockshutt (University of Victoria)

01/05/2024, 10:20

Current stellar nucleosynthesis models fail to reproduce the measured
isotopic abundances in group 2 oxygen-rich presolar grains, which are
characterized by large 18O depletions. It was proposed that cool bottom
processing in low-mass AGB stars is responsible for the observed isotopic
abundances. We modeled cool-bottom processing during the RGB and the
AGB of 1.2M⊙ stars to predict...

1. Nuclear Astrophysics Experimental Facilities at ISAC

Chris Ruiz (TRIUMF)

02/05/2024, 09:00

An overview of experimental nuclear physics facilities at ISAC. Aimed at the CaNPAN students, I'll provide a brief intro to the subject of measurement of nuclear observables relevant to astrophysics, before a virtual tour of the ISAC facilities and how they enable these measurements with exotic radioactive beams from the ISAC facility. In the afternoon, attendees will get to see the facilities...

2. Radiative Capture on a Nuclear Isomer: 26mAl(p,g)27Si

Annika Lennarz (TRIUMF)

02/05/2024, 09:30

"In explosive astrophysical environments, such as novae, supernovae and neutron star mergers, a significant fraction of atomic nuclei are expected to exist in excited quantum states. These elevated levels participate in nucleosynthesis much in the same way as nuclear ground states and, as such, play an essential role in determining the abundance of chemical elements in our Galaxy.

In this...

3. 86Kr(α,n)89Sr and the weak r-process

Cameron Angus (TRIUMF)

02/05/2024, 09:50

The r-process is responsible for half of all heavier-than-iron elements in the universe today.
However, while models have been able to reproduce the abundance distributions of the
heaviest elements observed in ultra-metal poor stars, intermediate-mass elements (36 < Z < 47) have been observed to be more abundant than expected from model predictions. The weak r-process in early core-collapse...

4. (*R) The 22Ne(a,n) Reaction at DRAGON

Ben Reed (TRIUMF/SMU)

02/05/2024, 10:10

Almost half of the elements heavier than iron are believed to be produced in the r-process. It is now understood that one r-process sight is neutron star mergers. However, observations suggest the r-process must be occurring in addition sights. One possibility is core-collapse supernovae, which are predicted to be driven by the weak r-process, in which heavy elements are produced by a series...

22. Welcome

Falk Herwig (University of Victoria)

03/05/2024, 09:00

23. Nuclear physics and r-process observables

Rebecca Surman (University of Notre Dame)

03/05/2024, 09:15

Our understanding of the formation of the heaviest elements via rapid neutron capture (r-process) nucleosynthesis is built up through the detection and analysis of a variety of astrophysical observables: isotopic and elemental abundance patterns, electromagnetic signatures, and radioisotopes. The interpretation of each type of observable is complicated by the unknown nuclear physics of the...

24. Illuminating astrophysical actinide production using MeV gamma-rays and metal-poor stars

Nicole Vassh (TRIUMF)

03/05/2024, 09:55

Fingerprints of the properties of exotic nuclei on nucleosynthesis observables have been used for decades to frame our picture of how the heaviest elements in our Solar System came to be. The abundance of elements in our Sun, as well as nearby metal-poor stars, hints at multiple neutron capture nucleosynthesis processes, the slow (s), intermediate (i) and rapid (r) neutron capture processes....

25. Capture of degenerate neutrons

Liliana Caballero Suarez (University of Guelph)

03/05/2024, 10:20

Neutron stars, accreting matter from a companion, contribute to the inventory of systems that can be explored through multimessenger astronomy. As the accreted matter interacts with ions in the neutron star atmosphere and crust, it triggers nuclear reactions, generating X-rays, p-nuclei, and potentially gravitational wave emissions. Gravity draws the newly synthesized nuclei into deeper layers...