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β decay of 61v and its role in cooling accreted neutron star crusts

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dc.contributor.author Ong, W.-J.
dc.contributor.author Brown, E. F.
dc.contributor.author Browne, J.
dc.contributor.author Ahn, S.
dc.contributor.author Childers, K.
dc.contributor.author Crider, B. P.
dc.contributor.author Dombos, A. C.
dc.contributor.author Gupta, S. S.
dc.contributor.author Hitt, G. W.
dc.contributor.author Langer, C.
dc.contributor.author Lewis, R.
dc.contributor.author Liddick, S. N.
dc.contributor.author Lyons, S.
dc.contributor.author Meisel, Z.
dc.contributor.author Möller, P.
dc.contributor.author Montes, F.
dc.contributor.author Naqvi, F.
dc.contributor.author Pereira, J.
dc.contributor.author Prokop, C.
dc.contributor.author Richman, D.
dc.contributor.author Schatz, H.
dc.contributor.author Schmidt, K.
dc.contributor.author Spyrou, A.
dc.date.accessioned 2021-06-08T17:15:32Z
dc.date.available 2021-06-08T17:15:32Z
dc.date.issued 2021-06-08
dc.identifier.uri http://localhost:8080/xmlui/handle/123456789/1768
dc.description.abstract The interpretation of observations of cooling neutron star crusts in quasipersistent x-ray transients is affected by predictions of the strength of neutrino cooling via crust Urca processes. The strength of crust Urca neutrino cooling depends sensitively on the electron-capture and β-decay ground-state-to-groundstate transition strengths of neutron-rich rare isotopes. Nuclei with a mass number of A ¼ 61 are predicted to be among the most abundant in accreted crusts, and the last remaining experimentally undetermined ground-state-to-ground-state transition strength was the β decay of 61V. This Letter reports the first experimental determination of this transition strength, a ground-state branching of 8.1þ4.0 −3.1%, corresponding to a log ft value of 5.5þ0.2 −0.2 . This result was achieved through the measurement of the β-delayed γ rays using the total absorption spectrometer SuN and the measurement of the β-delayed neutron branch using the neutron long counter system NERO at the National Superconducting Cyclotron Laboratory at Michigan State University. This method helps to mitigate the impact of the pandemonium effect in extremely neutronrich nuclei on experimental results. The result implies that A ¼ 61 nuclei do not provide the strongest cooling in accreted neutron star crusts as expected by some predictions, but that their cooling is still larger compared to most other mass numbers. Only nuclei with mass numbers 31, 33, and 55 are predicted to be cooling more strongly. However, the theoretical predictions for the transition strengths of these nuclei are not consistently accurate enough to draw conclusions on crust cooling. With the experimental approach developed in this work, all relevant transitions are within reach to be studied in the future. en_US
dc.language.iso en_US en_US
dc.title β decay of 61v and its role in cooling accreted neutron star crusts en_US
dc.type Article en_US


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