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首页> 外文期刊>Physical Review C >First measurement of the ~(34)S( p,γ )~(35)Cl reaction rate through indirect methods for presolar nova grains
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First measurement of the ~(34)S( p,γ )~(35)Cl reaction rate through indirect methods for presolar nova grains

机译：首先测量〜（34）S（P，γ）〜（35）Cl反应速率通过间接方法进行预寄存的诺瓦谷物

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摘要

Sulphur isotopic ratio measurements may help to establish the astrophysical sites in which certain presolar grains were formed. Nova model predictions of the 34S/32S ratio are, however, unreliable due to the lack of an experimental ~(34)S(p,γ )~(35)Cl reaction rate. To this end, we have measured the ~ (34)S(~3He,d)~(35)Cl reaction at 20 MeV using a high resolution quadrupole-dipole-dipole-dipolemagnetic spectrograph. Twenty- two levels over 6.2 MeV < Ex (~(35)Cl) < 7.4 MeV were identified, ten of which were previously unobserved. Proton-transfer spectroscopic factors have been measured for the first time over the energy range relevant for novae.With this new spectroscopic information a new ~(34)S(p,γ )~(35)Cl reaction rate has been determined using a Monte Carlo method. Hydrodynamic nova model calculations have been performed using this new reaction rate. These models show that remaining uncertainties in the ~(34)S(p,γ ) rate affect nucleosynthesis predictions by less than a factor of 1.4, and predict a ~(34)S/~(32)S isotopic ratio of 0.014–0.017. Since recent type Ⅱ supernova models predict ~(34)S/~(32)S = 0.026−0.053, the ~(34)S/~(32)S isotopic ratio may be used, in conjunction with other isotopic signatures, to distinguish presolar grains from oxygen-neon nova and type II supernova origin. Our results address a key nuclear physics uncertainty on which recent considerations discounting the nova origin of several grains depend.
机译：硫同位素比率测量可能有助于建立形成某些预寄生晶粒的天体物理位点。然而，由于缺乏实验〜（34）S（P，γ）〜（35）Cl反应速率，Nova模型预测是不可靠的。为此，我们已经测量了〜（34）S〜（35）在20兆电子伏氯反应使用高分辨率四极 - 偶极 - 偶极-dipolemagnetic摄谱仪（〜氦-3，d）。确定了超过6.2 meV

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  • 来源
    《Physical Review C》 |2017年第2017期|025801.1-025801.8|共8页
  • 作者

    S. A. Gillespie; A. Parikh; C. J. Barton; T. Faestermann; J. Jose; R. Hertenberger; H.-F. Wirth; N. de Sereville; J. E. Riley; M. Williams;

  • 作者单位

    Department of Physics University of York York United Kingdom;

    Departament de Fisica Universitat Politecnica de Catalunya Barcelona Spain Institut d’Estudis Espacials de Catalunya (IEEC) E-08034 Barcelona Spain;

    Department of Physics University of York York United Kingdom;

    Physik Department E12 Technische Universitaet Muenchen D-85748 Garching Germany Maier- Leibnitz-Laboratorium der Muenchner Universitaeten (MLL) D-85748 Garching Germany;

    Departament de Fisica Universitat Politecnica de Catalunya Barcelona Spain Institut d’Estudis Espacials de Catalunya (IEEC) E-08034 Barcelona Spain;

    Maier- Leibnitz-Laboratorium der Muenchner Universitaeten (MLL) D-85748 Garching Germany Fakultaet fuer Physik Ludwig-Maximilians-Universitaet Muenchen D- 85748 Garching Germany;

    Maier- Leibnitz-Laboratorium der Muenchner Universitaeten (MLL) D-85748 Garching Germany Fakultaet fuer Physik Ludwig-Maximilians-Universitaet Muenchen D- 85748 Garching Germany;

    Institut de Physique Nucleaire d’Orsay UMR8608 IN2P3-CNRS Universite Paris Sud 11 91406 Orsay France;

    Department of Physics University of York York United Kingdom;

    Department of Physics University of York York United Kingdom TRIUMF Vancouver British Columbia Canada V6T 2A3;

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