Orbital elements of barium stars formed through a wind accretion scenario

2); (2)Shijianzhuang Teachers' College; (3) Beijing Astro. Obs. (4) Nanjing Univ. (5) BAC); 5); 5) ((1) Hebei Normal Univ.; B. Zhang (1; J. H. Liu (1; Q. H. Peng (4; Y. C. Liang (3)

arxiv: astro-ph/0011120 · v1 · submitted 2000-11-06 · 🌌 astro-ph

Orbital elements of barium stars formed through a wind accretion scenario

J. H. Liu (1 , 2) , B. Zhang (1 , 5) , Y. C. Liang (3) , Q. H. Peng (4 , 5) ((1) Hebei Normal Univ. , (2)Shijianzhuang Teachers' College

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(3) Beijing Astro. Obs. (4) Nanjing Univ. (5) BAC)

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keywords bariumorbitalstarsaccretionbinariesscenariowindconservation

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Taking the total angular momentum conservation in place of the tangential momentum conservation, and considering the square and higher power terms of orbital eccentricity e, the changes of orbital elements of binaries are calculated for wind accretion scenario. These new equations are used to quantitatively explain the observed (e,logP) properties of normal G, K giants and barium stars. Our results reflect the evolution from G, K giant binaries to barium binaries, moreover, the barium stars with longer orbital periods P>1600 days may be formed by accreting part of the ejecta from the intrinsic AGB stars through wind accretion scenario.

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Unveiling the nature of barium stars. I. Asteroseismic masses and the evolutionary link between Ba dwarfs and giants
astro-ph.SR 2026-06 unverdicted novelty 7.0

Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.