Speaker
Description
This study investigates the impact of dark matter halo rotation on satellite orbital decay rates and tidal stream formation, with a focus on the role of dynamical friction and energy loss. Using N-body simulations and analytical models, the effects of varying halo spin isotropies on satellite motion and the resulting tidal streams are examined. The results show that co-rotation with the satellite’s orbit reduces the orbital decay rate, while counterrotation accelerates it. The strength of rotation is directly related to the intensity of dynamical friction, with stronger rotations leading to greater changes in the rate of energy loss. These findings suggest that tidal stream dynamics are sensitive to the rotational properties of dark matter halos, and indicate that tidal streams can serve as effective tracers of halo rotation. This highlights their potential as a tool for probing the dynamical state of dark matter halos.
| Keyword-1 | Dark Matter Halos |
|---|---|
| Keyword-2 | Dynamical Friction |
| Keyword-3 | N-Body Simulations |