Chemical compositions of four barium stars

Abstract

Chemical compositions of four barium stars HD 26886, HD 27271, HD 50082 and HD 98839 are studied based on high resolution, high signal-to-noise Echelle spectra. Results show that all of them are disk stars. Their αand iron peak elements are similar to the solar abundances. The neutron-capture process elements are overabundant relative to the Solar. The heavy-element abundances of the strong Ba star HD 50082 are higher than those of other three mild Ba stars. Its mass is 1.32Msun (+0.28,-0.22Msun), and is consistent with the average mass of strong Ba stars (1.5Msun). For mild Ba star HD 27271 and HD 26886, the derived masses are 1.90Msun (+0.25,-0.20Msun) and 2.78Msun (+0.75,-0.78M_sun), respectively, which are consistent with the average mass of mild Ba stars. We also calculate the theoretical abundances of Ba stars by combining the AGB stars nucleosynthesis and wind accretion formation scenario of Ba binary systems. The comparisons between the observed abundance patterns of the sample stars with the theoretical results show that wind accretion scenario can explain the abundance patterns of HD 50082 and HD 27271 well, but fail to explain the abundances of HD 26886. It means that the mild Ba star HD 26886, with shorter orbital period (P<1600 d), may be formed from other scenarios. The high mass mild Ba star HD 98839, with 3.62M_sun, and with very long orbital period (P>11000 d), may be either a star with the heavy elements enriched by itself or a "true Ba" star.

13 pages, Accepted for publication in A&A

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