SIMBAD references

Context. Winds from the accretion disk in tidal disruption events (TDEs) play a key role in determining their observed emission. While winds from the super-Eddington accretion phase in TDEs have recently been studied, the properties of winds from the sub-Eddington accretion disk remain unclear.
Aims. We aimed to investigate the properties of winds from the circularized sub-Eddington accretion disk in TDEs and study the line-force-driven accretion disk wind.
Methods. We performed two-dimensional hydrodynamic simulations using the PLUTO code to study the line-force-driven wind from the circularized accretion disk around a 10⁶ solar mass black hole in TDEs.
Results. We find that although the disk is very small in TDEs, a strong wind can be driven by line force when the disk has a luminosity greater than 20% of the Eddington luminosity. The maximum velocity of the wind can reach up to 0.3 times the speed of light. The kinematic power of wind ranges from 1 - 6% of the Eddington luminosity.
Conclusions. Strong winds can be driven by line force from the thin disk around a 10⁶ solar mass black hole in TDEs. We briefly discuss the possible radio emission from the shock when the wind collides with the surrounding medium.