Collectivity at the prolate-oblate transition: The <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si1.svg"><mml:msubsup><mml:mrow><mml:mn>2</mml:mn></mml:mrow><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mo linebreak="badbreak" linebreakstyle="after">+</mml:mo></mml:mrow></mml:msubsup></mml:math> lifetime of 190W

Şahin, E.; Werner, V.; Mistry, A.K.; Rudigier, M.; Nomura, K.; Jolie, J.; Pietralla, N.; Regan, P.H.; Ağgez, G.; Albers, H.M.; Ahmed, U.; Aktaş, Ö.; Algora, A.; Alhomaidhi, S.; Appleton, C.; Arıcı, T.; Armstrong, M.; Banerjee, A.; Benito, J.; Benzoni, G.; Blazhev, A.; Boutachkov, P.; Bruce, A.M.; Cederwall, B.; Chishti, M.M.R.; Cortés, M.L.; Crespi, F.; Das, B.; Davinson, T.; Dickel, T.; Doncel, M.; Ertoprak, A.; Esmaylzadeh, A.; Fraile, L.M.; Gamba, E.R.; Gerl, J.; Górska, M.; Ha, J.; Haettner, E.; Hall, O.; Heggen, H.; Hornung, C.; Hubbard, N.; Jazrawi, S.; John, P.R.; Jones, C.E.; Karayonchev, V.; Kazantseva, E.; Kern, R.; Knafla, L.; Kojouharov, I.; Koseoglou, P.; Kosir, G.; Kostyleva, D.; Kurz, N.; Kuzminchuk, N.; Llanos-Expósito, M.; Lozeva, R.; Mengoni, D.; Mertzimekis, T.J.; Mikolajczuk, M.; Morales, A.I.; Mukha, I.; Murias, J.R.; Nara-Singh, B.S.; Orrigo, S.E.A.; Pellumaj, J.; Pelonis, S.; Pietri, S.; Pigliapoco, S.; Podolyák, Zs.; Polettini, M.; Rezynkina, K.; Rösch, H.A.; Schaffner, H.; Scheidenberger, Ch.; Sexton, L.; Söderström, P.-A.; Tanaka, Y.K.; Valiente-Dobón, J.J.; Vasileiou, P.; Vasiljević, J.; Vesic, J.; Weick, H.; Wiederhold, J.; Yaneva, A.; Zhang, G.; Zhao, J.; Zyriliou, A.

doi:10.1016/j.physletb.2024.138976

Physics Letters B

2024

DOI: 10.1016/j.physletb.2024.138976

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Collectivity at the prolate-oblate transition: The 21+ lifetime of 190W

E. Şahin,

V. Werner,

A.K. Mistry

et al.

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Cited by 2 publications

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γ-γ fast timing with high-performance LaBr3(Ce) scintillat

Régis,

Fraile,

Rudigier

2025

Progress in Particle and Nuclear Physics

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γ-γ fast timing with high-performance LaBr3(Ce) scintillat

Régis,

Fraile,

Rudigier

2025

Progress in Particle and Nuclear Physics

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Structure and astrophysical role of the neutron-rich $$55 \le Z \le 92$$ isotopes: status and perspectives

Kiss,

Podolyák

2024

Eur. Phys. J. A

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Heavy neutron-rich nuclei are of great interest. Phenomena like shell evolution ($$N\sim 126$$ N ∼ 126 , $$Z\sim 82$$ Z ∼ 82 ), prolate–triaxial–oblate–spherical shape evolution ($$Z=$$ Z = 70–80), possible deformed shell closures or structure change in the rare-earth region are under intense scrutiny. This latter is closely linked to the rare-earth r-process peak, while the $$N \sim 126$$ N ∼ 126 nuclei are connected to the third r-process peak at $$A \sim 195$$ A ∼ 195 . Recent technical developments (e.g. increasing beam intensities at fragmentation facilities, new detection systems) provided huge amount of new experimental data, published in the last decade, allowing to probe structure and astrophysical models. Experimental methods and recent results are reviewed and future opportunities discussed.

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Collectivity at the prolate-oblate transition: The 21+ lifetime of 190W

Cited by 2 publications

References 61 publications

γ-γ fast timing with high-performance LaBr3(Ce) scintillat

γ-γ fast timing with high-performance LaBr3(Ce) scintillat

Structure and astrophysical role of the neutron-rich $$55 \le Z \le 92$$ isotopes: status and perspectives

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