Nuclear Science Seminar Speaker Schedule Sign Up

Current Schedule

Speaker = Dr. Julian Kahlbow of Lawrence Berkeley National Laboratory

Host = Revel, Aldric revel@frib.msu.edu

When = 2025-04-23 Wednesday 15:30

Where = FRIB 1300

Please feel free to sign up below, but note that some slots may need to be re-assigned to accommodate those with a specific need to meet the speaker. If this happens, the Admin or Speaker Host will reach out to you via email.

Start Time End Time Name Building Room
09:00 09:30 Aldric Revel FRIB 1014
09:30 10:00 Jaideep Taggart Singh FRIB 2016
10:00 10:30 Personal Time FRIB 2102
10:30 11:00 Filomena Nunes FRIB 2107
11:00 11:30 Thomas Baumann FRIB 6304
11:30 12:00 George Zimba FRIB 2003
12:00 13:00 Lunch with Graduate Students FRIB 2311
13:00 13:30 Personal Time FRIB 2102
13:30 14:00 Patrick McGlynn FRIB 2120
14:00 14:30 Personal Time FRIB 2102
14:30 15:00 Alex Brown FRIB 2043
15:00 15:30 Speaker Prep time FRIB 1300
15:30 16:30 Seminar FRIB 1300

Context

Title = Magicity vs Superfluidity, and the structure of extremely neutron-rich O & F isotopes

Abstract

The atomic nucleus is an intricate, strongly-interacting quantum many-body system with fascinating structure rooted in Quantum Chromodynamics. The shell model has been a successful cornerstone describing effectively nuclear structure and predicting magic numbers. However, in extremely neutron-rich nuclei, nuclear structure undergoes significant changes with often surprising effects due to neutron excess and weak binding. One particularly interesting region is around the isotope 28O. In this talk, I will discuss nuclear structure studies of neutron-rich Fluorine isotopes using high-resolution invariant-mass spectroscopy at the SAMURAI setup at RIBF/RIKEN (Japan). We measured the isotope 30F for the first time, confirming the breakdown of the neutron magic number N = 20. Based on shell-model calculations this causes a superfluid behavior. This finding leads to new questions about neutron correlations in a low-density environment, similar to conditions in the crust of neutron stars.

Relevant background with commentary from Dr. Kahlbow: