Ground State Gamow-Teller Strength in 64Ni (n,p) 64Co

  • A. Ling
  • R. C. Haight
  • N. S. P. King
  • P. W. Lisowski
  • D. S. Sorenson
  • J. L. Ullmann
  • X. Aslanoglou
  • R. W. Finlay
  • B. K. Park
  • J. Rapaport
  • F. P. Brady
  • J. L. Romero
  • C. R. Howell
  • W. Tornow

Abstract

An important process occuring in presupernova stars is e- capture on free protons and nuclei.1,2 As e- capture and the charge exchange reaction (n,p) between same initial and final states are both To → To + 1 transitions involving the same nuclear matrix element, the (n,p) reaction can be used to provide the input required to calculate e- capture rates. Specifically, the e- capture rate λ if for a nucleus going from an initial state i to a final state f is proportional to the Gamow-Teller strength Bif(GT)3:
$${\lambda ^{if}}\alpha {B^{if}}\left( {GT} \right)$$
Where Bif(GT) is given by4
$${B^{if}}\left( {GT} \right) = \frac{1}{{2{J_i} + 1}}{\left| { < f\left| {\sigma \tau } \right|i >} \right|^2}$$
.

Keywords

Calorimeter 

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Copyright information

© Springer Science+Business Media New York 1991

Authors and Affiliations

  • A. Ling
    • 1
  • R. C. Haight
    • 1
  • N. S. P. King
    • 1
  • P. W. Lisowski
    • 1
  • D. S. Sorenson
    • 1
  • J. L. Ullmann
    • 1
  • X. Aslanoglou
    • 2
  • R. W. Finlay
    • 2
  • B. K. Park
    • 2
  • J. Rapaport
    • 2
  • F. P. Brady
    • 3
  • J. L. Romero
    • 3
  • C. R. Howell
    • 4
  • W. Tornow
    • 4
  1. 1.Los Alamos National LaboratoryLos AlamosUSA
  2. 2.Ohio UniversityAthensUSA
  3. 3.University of CaliforniaDavisUSA
  4. 4.Duke UniversityDurhamUSA

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