On the Models of Early Main Sequence Evolution of Moderately Massive Stars with growing Inhomogeneous Convection Zone

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The models similar to those proposed by Sakashita and Hayashi to represent the main sequence evolution of massive stars have been studied for the evolution of moderately massive star. Each of the models consists of the inhomogeneous convection zone developing between the outer radiative envelope of initial chemical composition and the homogeneous convection core of the diminishing hydrogen content. In actual computation, such an inhomogeneous convection zone is approximated by the treatment of Sakashita and Hayashi's semiconvection zone. The models are examined for two cases of simplified opacity law. Along the evolutionary sequence of such models, the intermediate inhomogeneous convection zone extends steadily inward and chemically homogeneous central core shrinks without changing the outermost boundary of the convection core. Though it has not been made sure exactly yet, the central homogeneous core disappears when the central hydrogen content becomes a critical value which is still appreciably high and depends on the adopted opacity law and initial chemical composition. In general, it may be said that the central hydrogen content at such a critical stage should be smaller for the star of larger mass. Until arriving at the critical stage defined here, the present scheme of evolution does not bring about any appreciable change in stellar luminosity, radius and the internal run of physical quantities such as mass, pressure and density except the temperature which increases in a way of just compensating the increase of the mean molecular weight in the equation of state for pressure. Some speculations have been briefly made of the model characters of the subsequent evolution.Stellar structureStellar evolutionMain sequenceConvection coreSemiconvection zone
東北大学の論文
1983-12-26

On the Models of Early Main Sequence Evolution of Moderately Massive Stars with growing Inhomogeneous Convection Zone

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