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Table 5.

Sensitive: species most impacted by the modification of individual weak rates.

[AZ/56Fe](a) influencers and Di, j
4He −7.2 55Fe (0.40); 54Mn (0.34); 56Co (0.34); 56Ni (-0.07)
48Ca −3.7 57Fe (0.50); 55Mn (0.44); 54Mn (0.42); 56Fe (0.42); 55Fe (0.34); 58Co (0.20); 56Mn (0.18); 57Co (0.17); 54Fe (0.16); 61Ni (0.15)
50Ti 0.47 56Fe (0.09); 54Mn (0.09); 55Fe (0.09); 57Fe (0.09); 55Mn (0.07); 58Co (0.04)
54Cr 0.87 55Fe (0.07); 56Fe (0.07); 54Mn (0.06); 57Fe (0.06); 55Mn (0.04)
58Fe 0.34 55Fe (0.06); 56Fe (0.05); 54Mn (0.04)
58Ni −0.16 56Ni (0.04)
61Ni −1.3 55Fe (0.12); 54Mn (0.09); 56Co (0.08)
62Ni −0.09 55Fe (0.06)
64Ni −1.1 57Fe (0.22); 54Mn (0.20); 56Fe (0.20); 55Mn (0.19); 55Fe (0.17); 58Co (0.10); 57Co (0.08); 54Fe (0.08); 56Mn (0.07); 61Ni (0.07)
64Zn −2.1 55Fe (0.04)
67Zn −2.5 57Fe (0.05)

Notes. Listed are those species for which |Di, j| ≥ 0.045.

(a)

[AZ/56Fe]=log[n(AZ)/n(AZ)] − log[n(56Fe)/n(56Fe)], with n(AZ) the number fraction of isotope AZ in the supernova ejecta, and n(AZ) its abundance in the solar system (Lodders 2003)

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