| Summary: | <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni-<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Cu region nuclei play important roles in core-collapse supernovae and the slow neutron-capture (<i>s</i>) process. In this work, the stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates for <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni are studied within the projected shell model where the effects of thermally populated parent-nucleus excited states are analyzed. For <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Co, the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates are lower than the results of the conventional shell model. For the <i>s</i>-process branching point <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>63</mn></msup></semantics></math></inline-formula>Ni, the <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rate under a terrestrial condition is well described, and the calculated stellar <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mi>β</mi><mo>−</mo></msup></semantics></math></inline-formula> decay rates in the <i>s</i>-process condition turn out to increase with stellar temperature due to the contribution from parent-nucleus excited states.
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