Nuclear stellar clusters are common in the center of galaxies. We consider the possibility that their progenitors assumed to be globular clusters may have formed elsewhere, migrated to, and assembled near their present location. The main challenge for this scenario is whether globular clusters can withstand the tidal field of host galaxies. Our analysis suggests that provided the mass-density distribution of galactic potential is shallow, the tidal field near the center of galaxies is able to compress rather than disrupt a globular cluster at a distance from the center much smaller than the conventionally defined "tidal disruption radius". To do so, we consider the secular evolution of star clusters with a homogeneous mass-density distribution. We analytically solve the secular equations in the limit that the mass density of stars in the galactic center approaches a uniform distribution. Our model indicates that a star cluster could travel to very small distances without disruption, thus potentially contributing to the formation of the nuclear cluster. However, appropriate numerical N-body simulations are needed to confirm our analytic findings.

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