Effect of Composition on the Post-Red Evolution of a 5 M_{sun} Star
Abstract
Calculations are presented of the evolution of three stellar models from main sequence through core-helium exhaustion. The compositions of the three models are V = 0.30, Z = 0.03 (Population I); V = 0.20, Z = 0.03 (helium poor); V = 0.30, Z = 0.015 (metal poor). The main purpose of the calculations was to examine the effect of composition on the loops in the H-R diagram during core-helinm burning, by the use of three compositions instead of only two (as previous investigations have done). We find that (1) the existence of the loops appears to be independent of composition; (2) the blue end of of the loop becomes cooler and brighter as V increases (at constant Z) and cooler and fainter as Z increases (at constant V). Comparison with previous calculations suggests that the detailed properties of the calculated loops depend more strongly on the computational methods and assumptions than on the composition.
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