Abstract
We investigate the plasmoid knot formation in stratified relativistic jet by means of relativistic magneto-hydrodynamics simulations. Indeed, astrophysical jets in active galactic nuclei (AGN) seem to be transversely stratified, with a fast inner jet and a slower outer jet. It is likely that the launching mechanism for each component is different. On the other hand, the steady and moving knots’ properties are observed along these jets. With the proposed model, we were able to link the different types of observed knot in various radio loud AGN with specific stratified jet characteristics. We showed that the increase energy flux at the outer edge of the jet induces a steady knot near the core and a moving knot at a greater distance.
Highlights
There is growing evidence of transverse stratification of relativistic astrophysical jets with clear indication of a fast inner jet embedded in a slower outer flow
In many active galactic nuclei (AGN), a limb-brightened jet morphology is observed on pc scales [1], which is interpreted as an outcome of the differential Doppler boosting between the jet spine and layer [2]
Numerous standing and moving radio knots in AGN jets have been observed over the last decades in very long baseline interferometry (VLBI) thanks to dedicated long-term monitoring programs such as MOJAVE or TANAMI
Summary
There is growing evidence of transverse stratification of relativistic astrophysical jets with clear indication of a fast inner jet (spine) embedded in a slower outer flow (layer). We adopt a two-component jet model with various kinetic energy flux distributions between the inner–outer jets [9]. In all the other investigated cases, we set a transverse structured jet with an overpressured inner jet.
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