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We use direct $N$-body calculations to investigate the impact of primordialmass segregation on the size scale and mass-loss rate of star clusters in agalactic tidal field. We run a set of simulations of clusters with varyingdegrees of primordial mass segregation at various galactocentric radii and showthat, in primordially segregated clusters, the early, impulsive mass-loss fromstellar evolution of the most massive stars in the innermost regions of thecluster leads to a stronger expansion than for initially non-segregatedclusters. Therefore, models in stronger tidal fields dissolve faster due to anenhanced flux of stars over the tidal boundary. Throughout their lifetimes, thesegregated clusters are more extended by a factor of about 2, suggesting that(at least) some of the very extended globular clusters in the outer halo of theMilky Way may have been born with primordial mass segregation. We finallyderive a relation between star-cluster dissolution time, $T_{diss}$, andgalactocentric radius, $R_G$, and show how it depends on the degree ofprimordial mass segregation.

The effect of primordial mass segregation on the size scale of globular clusters