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A tidal radius is a distance from a satellite orbiting in a host potentialbeyond which its material is stripped by the tidal force. We derive a revisedexpression for the tidal radius of a rotating satellite which properly takesinto account the possibility of prograde and retrograde orbits of stars.Besides the eccentricity of the satellite orbit, the tidal radius depends alsoon the ratio of the satellite internal angular velocity to the orbital angularvelocity. We compare our formula to the results of two $N$-body simulations ofdwarf galaxies orbiting a Milky Way-like host on a prograde and retrogradeorbit. The tidal radius for the retrograde case is larger than for theprograde. We introduce a kinematic radius separating stars still orbiting thedwarf galaxy from those already stripped and following the potential of thehost galaxy. We find that the tidal radius matches very well the kinematicradius. Our results provide a connection between the formalism of the tidalradius derivation and the theory of resonant stripping.

On the tidal radius of satellites on prograde and retrograde orbits