1988/06/01 by Mario Livio, Noam Soker · 355 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Binary number #Binary star #Common envelope #Physics #Planetary nebula #Stars #Stellar evolution #Stellar mass loss #Stellar, planetary, and galactic studies #Supergiant #White dwarf
paper · doi:10.1086/166419
published in The Astrophysical Journal 329, 764 (IOP Publishing)
openalex publication_date 1988/06/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/04
The common envelope phase in the evolution of binary systems is examined. Three parameters are identified which characterize the efficiency of energy deposition, the importance of three-dimensional effects, and the efficiency of spin-up of the envelope. It is demonstrated that the efficiency of deposition of orbital energy into envelope ejection can be quite low. It is found that significant spin-up of the envelope can be expected to occur in relatively early stages, when the spiralling-in occurs inside evolved supergiant envelopes. In normal giants spin-up can occur only in the final stages of the spiralling-in process. The results of a simplified three-dimensional numerical calculation of the common envelope phase are presented, and the implications of the results for the formation of planetary nebulae with binary nuclei, double white dwarf systems, and FK Com stars are discussed.