Inclined jets inside a common envelope of a triple stellar system

Abstract

We conduct a three-dimensional hydrodynamical simulation to study the interaction of two opposite inclined jets inside the envelope of a giant star, and find that the jets induce many vortexes inside the envelope and that they efficiently remove mass from the envelope and form a very clumpy outflow. We assume that this very rare type of interaction occurs when a tight binary system enters the envelope of a giant star, and that the orbital plane of the tight binary system and that of the triple stellar system are inclined to each other. We further assume that one of the stars of the tight binary system accretes mass and launches two opposite jets and that the jets' axis is inclined to the angular momentum axis of the triple stellar system. The many vortexes that the jets induce along the orbit of the tight binary system inside the giant envelope might play an important role in the common envelope evolution (CEE) by distributing energy in the envelope. The density fluctuations that accompany the vortexes lead to an outflow with many clumps that might facilitate the formation of dust. This outflow lacks any clear symmetry, and it might account for very rare types of 'messy' planetary nebulae and 'messy' nebulae around massive stars. On a broader scope, our study adds to the notion that jets can play important roles in the CEE, and that they can form a rich variety of shapes of nebulae around evolved stars.

Spin-orbit misalignment from triple-star common envelope evolution

“…The case of an AGB star that engulfs a tight binary system of two MSSs or of a white dwarf with a MSS is relevant to the formation of planetary nebulae, and in particular to planetary nebulae with 'messy' morphologies, i.e, that lack any kind of symmetry. 'Messy' planetary nebulae most like result from triple star interaction (e.g., Bear & Soker 2017;Danehkar et al 2018;Jones et al 2019;Miszalski et al 2019;Schreier et al 2019;Rechy-García et al 2020;Henney et al 2021). The spinning-up of the AGB envelope to have a rotation that is inclined to the triple star orbital angular momentum that I studied here adds to the 'messy' mass loss morphology.…”

“…The large fraction of triple and higher order star systems among massive stars (e.g., Sana et al 2014;Moe & Di Stefano 2017) and the rich triple star interaction outcomes (e.g., Toonen et al 2021) have motivated studies of CEJSNe in triple stars systems (e.g., Soker 2021a,b; Akashi & Soker 2021) as well as other triple-star CEE (e.g., Sabach & Soker 2015;Hillel et al 2017;Schreier et al 2019;Comerford & Izzard 2020;Glanz & Perets 2021;Soker & Bear 2021).…”

Can stellar-mass black hole growth disrupt disks of active galactic nuclei? The role of mechanical feedback

“…On the other hand, when the spin direction of the sBH is misaligned with respect to the angular momentum direction of the AGN disk (e.g. Schreier et al 2019, for the inclined JFM in common envelope evolution), it takes a longer time for the jet-cocoon to break out. Then, the depletion region by the cocoon is effectively enhanced to r dep = f ext H AGN θ c /cosi, where i is the inclination angle of the jet with respect to the orbital angular momentum of the AGN disk.…”

Three-dimensional simulations of the jet feedback mechanism in common envelope jets supernova

“…These omissions allow us to follow the system for years, unlike simulations that include the accretion process onto the NS/BH and are therefore limited to evolution time of several days or less (e.g., Moreno Méndez et al 2017;López-Cámara et al 2019. To reach our goal we set the numerical scheme in a similar manner to earlier studies of jet-induced outflow in CEE (e.g., Shiber & Soker 2018;Schreier et al 2019, but in the present study we include jets from a NS rather than from a main sequence star. We follow the flow structure in sections 4 and in section 5 we study the negative feedback process.…”