Gamow-Teller strength for the analog transitions to the first T=1/2, J^pi=3/2- states in 13C and 13N and the implications for Type Ia supernovae

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dc.creatorZegers, R. G. T.
dc.creatorBrown, E. F.
dc.creatorAkimune, H.
dc.creatorAustin, Sam M.
dc.creatorBerg, A. M. van den
dc.creatorBrown, B. A.
dc.creatorChamulak, D. A.
dc.creatorFujita, Y.
dc.creatorFujiwara, M.
dc.creatorGal`es, S.
dc.creatorHarakeh, M. N.
dc.creatorHashimoto, H.
dc.creatorHayami, R.
dc.creatorHitt, G. W.
dc.creatorItoh, M.
dc.creatorKawabata, T.
dc.creatorKawase, K.
dc.creatorKinoshita, M.
dc.creatorNakanishi, K.
dc.creatorNakayama, S.
dc.creatorOkamura, S.
dc.creatorShimbara, Y.
dc.creatorUchida, M.
dc.creatorUeno, H.
dc.creatorYamagata, T.
dc.creatorYosoi, M.
dc.date2007-10-16
dc.date2008-03-27
dc.date.accessioned2026-07-07T11:12:15Z
dc.date.available2026-07-07T11:12:15Z
dc.descriptionThe Gamow-Teller strength for the transition from the ground state of 13C to the T=1/2, J^pi=3/2- excited state at 3.51 MeV in 13N is extracted via the 13C(3He,t) reaction at 420 MeV. In contrast to results from earlier (p,n) studies on 13C, a good agreement with shell-model calculations and the empirical unit cross section systematics from other nuclei is found. The results are used to study the analog 13N(e-,v_e)13C reaction, which plays a role in the pre-explosion convective phase of type Ia supernovae. Although the differences between the results from the (3He,t) and (p,n) data significantly affect the deduced electron-capture rate and the net heat-deposition in the star due to this transition, the overall effect on the pre-explosive evolution is small.
dc.description11 pages, 4 figures
dc.identifierhttps://arxiv.org/abs/0710.2944
dc.identifierhttp://arxiv.org/abs/0710.2944
dc.identifierPhys.Rev.C77:024307,2008
dc.identifierdoi:10.1103/PhysRevC.77.024307
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/191320
dc.subjectNuclear Experiment
dc.titleGamow-Teller strength for the analog transitions to the first T=1/2, J^pi=3/2- states in 13C and 13N and the implications for Type Ia supernovae
dc.typetext

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