2017/12/19 by Muhammad Akashi, Ealeal Bear, Noam Soker +1
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Barrel (horology) #Gamma-ray bursts and supernovae #Instability #Jet (fluid) #Mechanics #Nebula #Physics #Planetary nebula #Shell (structure) #Stars #Stellar evolution #Supernova #astro-ph.SR
paper · pdf · doi:10.1093/mnras/sty029
28 pages, 12 figures. Submitted
arxiv created 2017/12/19 · openalex publication_date 2018/01/06 · arxiv updated 2018/01/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We conduct three-dimensional hydrodynamical simulations of two opposite jets with large opening angles launched from a binary stellar system into a previously ejected shell and show that the interaction can form barrel-like and H-like shapes in the descendant nebula. Such features are observed in planetary nebulae (PNe) and supernova remnants. Under our assumption, the dense shell is formed by a short instability phase of the giant star as it interacts with a stellar companion, and the jets are then launched by the companion as it accretes mass through an accretion disc from the giant star. We find that the H-shaped and barrel-shaped morphological features that the jets form evolve with time, and that there are complicated flow patterns, such as vortices, instabilities, and caps moving ahead along the symmetry axis. We compare our numerical results with images of 12 PNe, and show that jet–shell interaction that we simulate can account for the barrel-like or H-like morphologies that are observed in these PNe.