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Dr Laetitia Canete

Research Fellow in Experimental Nuclear Astrophysics

Academic and research departments

Department of Physics.


My qualifications

PhD (Experimental Nuclear Astrophysics)
University of Jyväskylä (Finland)
M.Sc. (Physics Subatomic and Astrophysics)
Université Lyon 1 (France)


D.A. Nesterenko, A. Kankainen, J. Kostensalo, C.R. Nobs, A.M. Bruce, O. Beliuskina, L. Canete, T. Eronen, E.R. Gamba, S. Geldhof, R. de Groote, A. Jokinen, J. Kurpeta, I.D. Moore, L. Morrison, Zs. Podolyak, I. Pohjalainen, S. Rinta-Antila, A. de Roubin, M. Rudigier, J. Suhonen, M. Vilén, V. Virtanen, J. Äystö (2020)Three beta-decaying states in 128In and 130In resolved for the first time using Penning-trap techniques, In: Physics Letters B135642 Elsevier

Isomeric states in 128In and 130In have been studied with the JYFLTRAP Penning trap at the IGISOL facility. By employing state-of-the-art ion manipulation techniques, three different beta-decaying states in 128In and 130In have been separated and their masses measured. JYFLTRAP was also used to select the ions of interest for identification at a post-trap decay spectroscopy station. A new beta-decaying high-spin isomer feeding the isomer in 128Sn has been discovered in 128In at 1797.6(20) keV. Shell-model calculations employing a CD-Bonn potential re-normalized with the perturbative G-matrix approach suggest this new isomer to be a 16⁺ spin-trap isomer. In 130In, the lowest-lying (10⁻) isomeric state at 58.6(82) keV was resolved for the first time using the phase-imaging ion cyclotron resonance technique. The energy difference between the 10⁻ and 1⁻ states in 130In, stemming from parallel/antiparallel coupling of (π0g-19/2) ⊗ (v0h-111/2), has been found to be around 200 keV lower than predicted by the shell model. Precise information on the energies of the excited states determined in this work is crucial for producing new improved effective interactions for the nuclear shell model description of nuclei near 132Sn.

LAETITIA CANETE, GAVIN JAMES LOTAY, G. Christian, DANIEL THOMAS DOHERTY, WILTON NEIL CATFORD, SAMUEL JAMES HALLAM, D. Seweryniak, H.M Albers, S Almaraz-Calderon, E.A Bennett, M.P. Carpenter, C.J. Chiara, JP Greene, C Hoffman, R. V. F. Janssens, J Jose, A Kankainen, T. Lauritsen, S Ota, A. Matta, A Saastamoinen, Ryan Wilkinson, M. Moukaddam, S. Zhu (2021)New constraints on the Al 25 ( p , γ ) reaction and its influence on the flux of cosmic γ rays from classical nova explosions, In: Physical review. C104L022802 American Physical Society (APS)

The astrophysical 25Al(p,γ) 26Si reaction represents one of the key remaining uncertainties in accurately modeling the abundance of radiogenic 26Al ejected from classical novae. Specifically, the strengths of key proton-unbound resonances in 26Si, that govern the rate of the 25Al(p,γ) reaction under explosive astrophysical conditions, remain unsettled. Here, we present a detailed spectroscopy study of the 26Si mirror nucleus 26Mg. We have measured the lifetime of the 3+, 6.125-MeV state in 26Mg to be 19(3) fs and provide compelling evidence for the existence of a 1– state in the T = 1, A = 26 system, indicating a previously unaccounted for ℓ = 1 resonance in the 25Al(p,γ) reaction. Using the presently measured lifetime, together with the assumption that the likely 1– state corresponds to a resonance in the 25Al + p system at 435.7(53) keV, we find considerable differences in the 25Al(p,γ) reaction rate compared to previous works. Furthermore, based on current nova models, we estimate that classical novae may be responsible for up to ≈ 15% of the observed galactic abundance of 26Al.