We present a case study of a early-type galaxy ( ETG ) hosting a kinematically distinct core ( KDC ) formed in a binary high resolution 1:1 spiral galaxy merger simulation .
The runtime of the simulation is pushed up to 10 ~ { } \mathrm { Gyr } to follow the complete evolution of various physical properties .
To investigate the origin of the KDC , the stellar component residing within the KDC is dissected , revealing that the rotational signal is purely generated by stars that belong to the KDC for at least 0.5 ~ { } \mathrm { Gyr } and are newly formed during the merging process .
Following the orientation of the total stellar angular momentum of the KDC , we show that it performs a motion comparable to the precession of a gyroscope in a gravitational potential .
We draw the conclusion that the motion of the KDC is a superposition of an intrinsic rotation and a global precession that gets gradually damped over cosmic time .
Finally , the stability of the KDC over the complete runtime of the simulation is investigated by tracing the evolution of the widely used \lambda _ { R } parameter and the misalignment angle distribution .
We find that the KDC is stable for about 3 ~ { } \mathrm { Gyr } after the merger and subsequently disperses completely on a timescale of \approx 1.5 \mathrm { Gyr } .