Free Access
Issue
A&A
Volume 578, June 2015
Article Number A117
Number of page(s) 15
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201525929
Published online 15 June 2015

Online material

Appendix A: Content of electronic tables for the grid

Table A.1

Description of table containing the results of our evolution models.

We provide files containing relevant evolution characteristics (Table A.1) for the 224 models of the present grid9. For each mass and initial helium content, models predictions are provided from the beginning of the pre-main sequence (along the Hayashi track) up to the brightest point of the evolution on the AGB. For each model, we have selected 500 points to allow a good description of the full raw tracks. First, the most important evolution keypoints are determined:

  • 1.

    the beginning of the pre-main sequence;

  • 2.

    the zero age main-sequence defined as the time when the central hydrogen abundance has decreased by 0.003 in mass fraction compared to its initial value.

  • 3.

    the turning point when the central mass fraction of hydrogen is equal to 0.06 on the main sequence;

  • 4.

    the end of core H-burning

  • 5.

    the bottom of the red giant branch (RGB);

  • 6.

    the RGB-tip;

  • 7.

    the local minimum of luminosity during central He-burning;

  • 8.

    the local maximum of Teff during central He-burning;

  • 9.

    the bottom of AGB: the point with the local minimum of luminosity after the loop on HB;

  • the brightest point on the AGB.

Then, we chose points from the results of evolutionary computation as follows:

  • 100 points are determined alongside the pre-main sequence withconstant time-steps. The value of each quantity given in Table A.1is computed from their values taken from the two nearest modelscalculated with STAREVOL.

  • The same procedure is applied between points 2 and 3 and points 3 and 4 where we use step in XC instead of time; 85 and 25 points are selected, respectively.

  • Between keypoints 4 and 5 we interpolate 60 points with equal time steps.

  • Then 20 points are determined between keypoints 5 and 6 with equal intervals of log L.

  • 20, 70, and 70 points are selected with equal central helium abundance YC steps between keypoints 6 and 7, keypoints 7 and 8, and keypoints 8 and 9.

  • 50 points are selected between keypoints 9 and 10 with the same log L step on the AGB.


© ESO, 2015

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