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Home All issues Volume 581 (September 2015) A&A, 581 (2015) A22 Online Material
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Issue
A&A
Volume 581, September 2015
Article Number A22
Number of page(s) 23
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201525876
Published online 26 August 2015

Online material

Appendix A: Tables

In this section we summarise the observed and modelled properties of the 67 CEMP-s stars in our sample. Table A.1 shows the observed temperatures, surface gravities and abundances of selected elements. The parameters of the best-fitting models to the CEMP-s stars with at least of two degrees of freedom (ν ≥ 2), as computed with model sets A–C, are shown in Tables A.2–A.4, as follows.

  • Columns 2–5: the fitted parameters M1,i, MPMZ, M2,i and Pi.

  • Columns 6–8: the mass accreted by the secondary star, ΔMacc, the orbital period of the binary when the secondary star best reproduces the observed log g and surface abundances, Pf, and for stars with observed orbital periods, the final period determined in Paper I.

  • Columns 9–11: , the number of degrees of freedom of the fit, ν, and the reduced χ2 of the best fit, i.e. .

In Tables A.5–A.7 the physical parameters of the best-fitting models of stars with ν ≤ 1 are shown.The confidence intervals of the input parameters of our models with and ν ≥ 2 computed with model set A are shown in Table A.8.

Table A.1

Surface gravities, temperatures and chemical properties observed in the 67 CEMP-s stars of our sample.

Table A.2

Physical parameters of the model CEMP-s stars with number of degrees of freedom ν ≥ 2 computed with model set A with WRLOF wind-accretion efficiency and spherically symmetric wind.

Table A.3

Physical parameters of the model CEMP-s stars with number of degrees of freedom ν ≥ 2 computed with model set B in which we adopt an efficient BHL model of wind mass transfer and efficient angular momentum loss.

Table A.4

Physical parameters of the model CEMP-s stars with number of degrees of freedom ν ≥ 2 computed with model set C in which we adopt the WRLOF wind-accretion efficiency and efficient angular momentum loss.

Table A.5

Physical parameters of the model CEMP-s stars with number of degrees of freedom ν ≤ 1 computed with model set A.

Table A.6

Physical parameters of the model CEMP-s stars with number of degrees of freedom ν ≤ 1 computed with model set B.

Table A.7

Physical parameters of model CEMP-s with number of degrees of freedom ν ≤ 1 computed with model set C.

Table A.8

Confidence ranges of the input parameters of the modelled CEMP-s stars with χ2/ν ≤ 3 and ν ≥ 2 computed with model set A with WRLOF wind-accretion efficiency and spherically symmetric wind.


© ESO, 2015

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