Adiabatic Mass Loss In Binary Stars. IV. Low and Intermediate Mass Helium Binary Stars

2024/06/19 by Lifu Zhang, Zhang, Lifu, Hongwei Ge +5 · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies

paper · pdf · doi:10.48550/arxiv.2406.13146

openalex publication_date 2024/06/19 · openalex created_date 2024/06/22 · openalex updated_date 2026/08/01

Abstract

The unstable mass transfer situation in binary systems will asymptotically cause the adiabatic expansion of the donor star and finally lead to the common envelope phase. This process could happen in helium binary systems once the helium donor star fills its Roche-lobe. We have calculated the adiabatic mass loss model of naked helium stars with a mass range of 0.35 M_\odot to 10 M_\odot, and every mass sequence evolved from the He-ZAMS to the cooling track of white dwarf or carbon ignition. In consideration of the influence of stellar wind, massive helium stars are not considered in this paper. Comparing stellar radius with the evolution of the Roche-lobe under the assumption of conservative mass transfer, we give the critical mass ratio q_\textrmcrit=M_\textrmHe/M_\textrmaccretor as the binary stability criteria of low and intermediate-mass helium binary stars. On He-MS, the result shows 1.0

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