Jets in common envelopes: a low-mass main-sequence star in a red giant

• Main Authors: De Colle, F. (Author), Iaconi, R. (Author), López-Cámara, D. (Author), Moreno Mndez, E. (Author), Shiber, S. (Author)
• Format: Article
• Language: English
• Published: Oxford University Press 2022
• Subjects: accretion, accretion discs; Accretion: accretion disks; binaries: close; Binaries: close; binaries: general; Binaries:general; Giant stars; hydrodynamics; Hydrodynamics; Large scale simulations; Low-mass; Main sequence stars; Method: numerical; methods: numerical; Numerical methods; Secondary stars; Small scale; Stars: Be
• Online Access: View Fulltext in Publisher

 We present small-scale 3D hydrodynamical simulations of the evolution of a 0.3 M ⊙main-sequence (MS) star that launches two perpendicular jets within the envelope of a 0.88 M ⊙red giant (RG). Based on previous large-scale simulations, we study the dynamics of the jets either when the secondary star is grazing, when it has plunged-in, or when it is well within the envelope of the RG (in each stage for ∼11 d). The dynamics of the jets through the common envelope (CE) depend on the conditions of the environment as well as on their powering. In the grazing stage and the commencement of the plunge self-regulated jets need higher efficiencies to break out of the envelope of the RG. Deep inside the CE, on the time-scales simulated, jets are choked independently of whether they are self-regulated or constantly powered. Jets able to break out of the envelope of the RG in large-scale simulations, are choked in our small-scale simulations. The accreted angular momentum on to the secondary star is not large enough to form a disc. The mass accretion on to the MS star is 1-10 per cent of the Bondi-Hoyle-Littleton rate ( ∼10 −3 -10 −1 M ⊙yr −1 ). High-luminosity emission, from X-rays to ultraviolet and optical, is expected if the jets break out of the CE. Our simulations illustrate the need for inclusion of more realistic accretion and jet models in the dynamical evolution of the CEs. © 2022 The Author(s)