2004/02/29 by Martin Krause, Martin G. H. Krause · 3 citations
Physics and Astronomy · #Active galactic nucleus #Astrophysical Phenomena and Observations #Astrophysical jet #Astrophysics #Astrophysics and Cosmic Phenomena #Bow shock (aerodynamics) #Cluster (spacecraft) #Computational physics #Cosmology #Galaxy #Gamma-ray bursts and supernovae #Jet (fluid) #Length scale #Mechanics #Phase (matter) #Physics #Scale (ratio) #Shock (circulatory) #Shock wave #astro-ph
paper · pdf · doi:10.1023/b:astr.0000044674.57913.c9
published in Astrophysics and Space Science 293(1-2), 255-262 (Springer Science+Business Media) · 8 pages, 5 figures, ApSS accepted, proceedings of the virtual jets 2003 conference in Dogliani/Italy, v3: funny and unimportant bug corrected, one reference added
arxiv created 2004/04/22 · openalex publication_date 2004/08/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In a parameter study extending to jet densities of 10-5 times the ambient one, I have recently shown that light large scale jets start their lives in a spherical bow shock phase. This allows an easy description of the sideways bow shock propagation in that phase. Here, I present new, bipolar, simulations of very light jets in 2.5D and 3D, reaching the observationally relevant scale of >200 jet radii. Deviations from the early bow shock propagation law are expected because of various effects. The net effect is, however, shown to remain small. I calculate the X-ray appearance of the shocked cluster gas and compare it to Cygnus A and 3C 317. Rings, bright spots and enhancements inside the radio cocoon may be explained.