Gaëtan Fichet (UV) — The complex dance between relativistic outflows and their host galaxies
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💡A RES Success Story about the influence of cosmic jets in galaxy evolution💡
📋 "The complex dance between relativistic outflows and their host galaxies" led by Gaëtan Fichet de Clairfontaine from Universitat de València
Powerful extragalactic jets are relativistic (almost as fast as light) streams of plasma launched near supermassive black holes. These jets greatly influence the evolution of their host galaxies by heating their surrounding gas, carving cavities in interstellar and intergalactic medium and suppressing the formation of new stars.
High-power jets are known to heat their surroundings through violent shock waves, but the heating mechanisms of intermediate and low-power jets are still not clear. The team examined how these jets interact with the material they encounter in detail; not only the diffuse interstellar medium, where they showed that mild shocks are also efficient heating mechanisms, but also individual stars and their stellar winds. Particularly, they also focused on the effects of multiple stars entering the jet sequentially, as it has been largely unexplored before.
🖥️ Thanks to RES supercomputer hashtagMareNostrum5 from Barcelona Supercomputing Center, the team performed high-resolution 3D simulations of realistic cosmic jets, including stars entering the jet sequentially.
The simulations revealed that the stellar winds strongly interact with the jet, forming overlapping tails of mixed, shocked gas. These interactions produce significant turbulence and deceleration of the jet material, suggesting that these kind of jets also transfer energy to the environment with gentler mechanisms such as mild shocks, turbulence and gradual thermal conduction.
The videos show, in order:
🔹Rest-mass density in the XY plane at z=0 where the 3 stars are located. The movie shows the entrance of 3 stars in the jet through the jet-ISM boundary represented by the green-blue/dark blue gradient. The jet flow propagates from the left to the right in dark blue.
🔹Density distribution in the XY plane at z = 0. The movie shows the injection and evolution of an underdense jet within the environment of a galaxy cluster, propagating from left to right.
🔹 Density contour surfaces from one of our 3D simulations. The movie shows the injection and evolution of an underdense jet within the environment of a galaxy cluster, propagating from left to right.
📋 "The complex dance between relativistic outflows and their host galaxies" led by Gaëtan Fichet de Clairfontaine from Universitat de València
Powerful extragalactic jets are relativistic (almost as fast as light) streams of plasma launched near supermassive black holes. These jets greatly influence the evolution of their host galaxies by heating their surrounding gas, carving cavities in interstellar and intergalactic medium and suppressing the formation of new stars.
High-power jets are known to heat their surroundings through violent shock waves, but the heating mechanisms of intermediate and low-power jets are still not clear. The team examined how these jets interact with the material they encounter in detail; not only the diffuse interstellar medium, where they showed that mild shocks are also efficient heating mechanisms, but also individual stars and their stellar winds. Particularly, they also focused on the effects of multiple stars entering the jet sequentially, as it has been largely unexplored before.
🖥️ Thanks to RES supercomputer hashtagMareNostrum5 from Barcelona Supercomputing Center, the team performed high-resolution 3D simulations of realistic cosmic jets, including stars entering the jet sequentially.
The simulations revealed that the stellar winds strongly interact with the jet, forming overlapping tails of mixed, shocked gas. These interactions produce significant turbulence and deceleration of the jet material, suggesting that these kind of jets also transfer energy to the environment with gentler mechanisms such as mild shocks, turbulence and gradual thermal conduction.
The videos show, in order:
🔹Rest-mass density in the XY plane at z=0 where the 3 stars are located. The movie shows the entrance of 3 stars in the jet through the jet-ISM boundary represented by the green-blue/dark blue gradient. The jet flow propagates from the left to the right in dark blue.
🔹Density distribution in the XY plane at z = 0. The movie shows the injection and evolution of an underdense jet within the environment of a galaxy cluster, propagating from left to right.
🔹 Density contour surfaces from one of our 3D simulations. The movie shows the injection and evolution of an underdense jet within the environment of a galaxy cluster, propagating from left to right.