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For a given \u0394\u03bd, \u0394\u03a01 depends not only on the stellar mass, but also on mixing processes that can affect the structure of the core. We find that in the case of more evolved red-giant-branch stars and regardless of the transport processes occurring in their interiors, the observed \u0394\u03a01 can provide information as to their stellar luminosity, within\u00a0\u223c10\u201320\u00a0per\u00a0cent. In general, the trends of \u0394\u03a01 with respect to mass and metallicity that are observed in Kepler red-giant stars are well reproduced by the models.<\/jats:p>","DOI":"10.1093\/mnrasl\/slv201","type":"journal-article","created":{"date-parts":[[2016,1,15]],"date-time":"2016-01-15T10:56:29Z","timestamp":1452855389000},"page":"L59-L63","source":"Crossref","is-referenced-by-count":20,"title":["Testing the cores of first ascent red giant stars using the period spacing of g 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