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The relaxation time at the half-mass radius of Galactic globular clusters(GGCs) is typically within a few Gyr. Hence, the majority of GGCs are expectedto be well relaxed systems, given their age is around 12-13 Gyr. So any initialradial segregation between stars of the same initial mass on the main sequence(MS), in particular, the progenitors of the present day sub-giant and red-giantbranch (SGB, RGB) stars should already have dissipated. However, a body ofevidence contradicting to these expectations has been accumulated to date. Theparadox could be solved by taking into account the effect of stellarcollisions. They occur at particularly high rate in collapsing nuclei of GGCsand seem to be mainly responsible for unrelaxed central regions and the radialsegregation observed. We draw attention that actually observed collisional bluestragglers should be less numerous than their lower-mass counterparts formedand accumulated at and below the present day MS turnoff. The effect of this isthat MS/SGB/RGB stars of a given luminosity are not of the same mass but fallin a range of mass.

Radial trends in Galactic globular clusters and their possible origin