Overshooting from convective cores and the occurrence of loops in the HRD. II - Evolution of 5 solar masses stars to the Cepheid phase

Astronomy and Astrophysics – Astrophysics

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Cepheid Variables, Hertzsprung-Russell Diagram, Mass Transfer, Stellar Evolution, Stellar Mass, Stellar Spectra, Convection, H Lines, Main Sequence Stars, Red Giant Stars

Scientific paper

In addition to the calculations presented and discussed in Paper I (Matraka et al., 1982), evolutionary calculations have been carried out for an extreme Population I star of total mass 5 solar masses. Overshooting at the border of the convective core during central H-burning is taken into account using two different values (0.5 and 1) of the ratio alpha (i) of mixing length to pressure scale height in the interior. For both of these sequences, the evolution through the red giant region is then calculated assuming a variety of values (0.5. . . 1.7) for alpha (0), which denotes the corresponding mixing length ratio in the outer convective zone. A variation of alpha (0) changes the penetration depth of the outer convective zone in a characteristic way; alpha (0) determines therefore the resulting X-profile which in turn influences the length of the loop in the H-R diagram. For overshooting with alpha (i) = 1, the loop does not cross the Cepheid strip unless alpha (0) is reduced to less than 0.5. Such crossings occur, however, for alpha (i) = alpha (0) = 0.5 (and possibly up to 0.7). Larger overshooting could be allowed without a suppression of the Cepheid phase, when smaller concentrations of the heavy elements were assumed, which is known to give larger loops.

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