Galactic-scale evolution of classical and complex radio galaxies. Impact of ambient morphology and jet geometry

Extragalactic jets, following their launching, exhibit a wide range of propagation orientations relative to the host galaxy's principal axis. This initial (mis)alignment has been shown to exert a substantial influence on a jet’s subsequent large-scale evolution. With this study, our aim is to investigate the spatiotemporal evolution of jets as a function of their propagation direction within their triaxial hosts, which introduces varying degrees of environmental hindrance, and as a function of internal jet properties (while maintaining identical jet power: 3 erg/s), which introduces varying collimation and thrust. 10^ 44 Observational data on extended radio sources were reanalyzed to identify key morphological and dynamical traits arising from variations in jet orientation and intrinsic properties. These findings were then systematically tested using a suite of 3D relativistic magneto-hydrodynamic simulations through the generation of dynamical and radiative maps. When a jet propagates along its host's major axis (the path of maximal environmental resistance), it produces an X-shaped morphology, with a secondary lobe that aligns along the minor axis and co-evolves actively alongside the active jet. At intermediate angles to the major axis, the jet morphology transitions into a double-boomerang structure with notably curved lobes. Such lobes are interestingly regenerative due to both backflow and jet precession mechanisms, making it difficult to disentangle their origin. Jets propagating along the minor axis (path of minimal resistance) exhibit faster propagation, forming classical double-lobed sources. With increased thrust and improved collimation (keeping jet power constant), these jets advance even more rapidly and potentially evolve into giant radio galaxy candidates. Counterexample sources that deviate from these traits were also modeled. The spatial variation of internal turbulence showed significant fluctuations below ∼ 1 kpc, with stronger magnetic fields further suppressing these irregularities. The magnetic field plays a key role in the radiative appearance of these sources, modulating features such as missing or one-sided (wing) lobe emission, filamentary structures, and warmspot versus hotspot formation.