2003/11/07 by Noam Soker · 2 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1016/j.newast.2004.01.004
published as New Astron. 9 (2004) 399-408 · Work prepared to IAU Colloquium 194: Compact Binaries in the Galaxy and Beyond, La Paz, Baja California Sur, Mexico, November 17, 2003
arxiv created 2003/11/07 · openalex publication_date 2004/02/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
I consider three processes which enhance mass loss rate from a common envelope of a giant star with a main sequence or a white dwarf companion spiraling-in inside its envelope. I consider deposition of orbital energy and orbital angular momentum to the giant's envelope, and in more detail the formation of jets by an accreting companion and their propagation in the envelope. I find that in many cases the deposition of orbital angular momentum to the envelope may be more important to the mass loss process than the deposition of orbital energy. Jets blown by an accreting companion, in particular a white dwarf, orbiting inside the outer regions of the giant's envelope may also dominate over orbital energy deposition at early stage of the common envelope evolution. These imply that studies which ignore the deposition of angular momentum to the envelope and the effects of the accreting companion may reach wrong conclusions.