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2 results for “Barium stars”
MESA Inlists for: Barium Surface Abundances of Blue Straggler Stars in the Open Clusters NGC 7789 and M67
<p>These are the MESA v15140 inlists and Python script associated with the models presented in Nine et al. (2024). The files are as follows:</p> <p>inlist, inlist_start_header, inlist_to_end_core_h_burn_header, inlist_to_start_he_core_flash_header, inlist_to_end_core_he_burn_header, inlist_to_end_agb_header, inlist_to_wd_header: Pointer files to tell MESA which inlists to read for control, kappa, and PGStar commands.</p> <p>inlist_start, inlist_to_end_core_h_burn, inlist_to_start_he_core_flash, inlist_to_end_core_he_burn, inlist_to_end_agb, inlist_to_wd: MESA inlist files with control, kappa, and PGStar commands for each stage.</p> <p>turnoff_masses.py: a Python script that takes in the file inlist_start_base and rewrites it to create a starting model with the mass of a turnoff star in NGC 7789 (1.8 solar masses), NGC 6819 (1.5 solar masses), M67 (1.3 solar masses), and NGC 188 (1.1 solar masses). This starting model is then used in the following inlists to create AGB star models with these masses.</p> <p>inlist_start_base: The base starting inlist that turnoff_masses.py reads in and alters to create inlist_start.</p>
Correlations between the abundances of Barium stars, the AGB model residuals and the delta parameter
<p>Additional figures for Világos et al. 2024, Sect. 3.2. For the sample of Barium stars, correlations between the observationally dervied abundances; the residuals between the AGB models and the abundances; and the delta parameter.</p> <p>The figures are divided into the following directories:</p> <ul> <li>'1-obs_feh': Abundances and elemental ratios of different peaks as a function of the [Fe/H] (Sect. 3.2.1 and Fig. 5).</li> <li>'2-res_feh': Residuals of the abundances and elemental ratios as a function of the [Fe/H] (Sect. 3.2.2 and Fig. 6).</li> <li>'3-obs_obs': Abundances as a function of the other abundances (Sect. 3.2.3 and Fig. 7).</li> <li>'4-res_res': Residuals of the abundances as a function of the other residuals (Sect. 3.2.4 and Fig. 8).</li> <li>'5-res_obs': Residuals of the abundances as a function of the abundances (see Sect. 3.2.5 and Fig. 9).</li> <li>'6-delta': Abundances and residuals as a function of the delta parameter, that indicates the fraction of AGB material in the Ba star envelope (Sect. 3.2.6 and Fig. 10).</li> </ul> <p>For figures in directories 1-2, we refer to some elements as [A/B], although sometimes [B/A] vs. [Fe/H] is shown. Visually, this swapping of the numerator and denominator elements means a vertical reflection around the y = 0 axis. Thus, $r_S$ and $a$ for [B/A] vs. [Fe/H] have the same absolute value but different sign than for [A/B] vs. [Fe/H].</p> <p>For figures in directories 3-5, if we refer to [A/Fe] vs [B/Fe], but plot [B/Fe] vs [A/Fe], the sign of the relationship (correlation or anti-correlation) remains the same. The swap of the two axes results in a reflection around a diagonal line with a slope of 1. The resulting slope is therefore $1/a$, while $r_S$ is the same in both cases.</p>
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