We investigate the long-term dynamical evolution of star clusters in a steadytidal field produced by its parent galaxy. In this paper, we focus on theinfluence of mass profile of the parent galaxy. The previous studies were donewith the simplification where the parent galaxy was expressed by point mass. Weexpress different mass profiles of the parent galaxy by the tidal fields inwhich the ratios of the epicyclic frequency to the angular velocity aredifferent. We compare the mass-loss timescale of star clusters whose tidalradii are identical but in parent galaxies with different mass profile, bymeans of orbits calculations in fixed cluster potential and N-body simulations.In this situation, a cluster rotates around the parent galaxy more rapidly asthe parent galaxy has shallower mass profile. We found that the mass-losstimescale increase 20% and 50% for the cases that the mass density profile ofthe parent galaxies are proportional to R^-2 and R^-1.5 where R is the distancefrom the galaxy center, compared to the point-mass case, in moderately strongtidal field. Counterintuitively, a cluster which rotates around the parentgalaxy more rapidly has a longer lifetime. The increase of lifetime is due tothe fact that the fraction occupied by regular-like orbit increases inshallower profile. Finally, we derive an evaluation formula for the mass-losstimescale of clusters. Our formula can explain a property of the population ofthe observed galactic globular clusters that their half-mass radii becomesmaller as their distances from the galactic center become smaller.
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