We investigate structure and kinematics of the second generation of stars ( SG ) formed from gaseous ejecta of the first generation of stars ( FG ) in forming globular clusters ( GCs ) .
We consider that SG can be formed from gaseous ejecta from AGB stars of FG with the initial total mass of 10 ^ { 6 } -10 ^ { 8 } { M } _ { \odot } to explain the present masses of the Galactic GCs .
Our 3D hydrodynamical simulations with star formation show that SG formed in the central regions of FG can have a significant amount of rotation ( V / \sigma \approx 0.8 - 2.5 ) .
The rotational amplitude of SG can depend strongly on the initial kinematics of FG .
We thus propose that some GCs composed of FG and SG had a significant amount of rotation when they were formed .
We also suggest that although later long-term ( \sim 10 Gyr ) dynamical evolution of stars can smooth out the initial structural and kinematical differences between FG and SG to a large extent , initial flattened structures and rotational kinematics of SG can be imprinted on shapes and internal rotation of the present GCs .
We discuss these results in terms of internal rotation observed in the Galactic GCs .