The mass evaporation rate of globular clusters evolving in a strong Galactic tidal field is derived through the analysis of large , multi-mass N -body simulations .
For comparison , we also study the same evaporation rates using MOCCA Monte Carlo models for globular cluster evolution .
Our results show that the mass evaporation rate is a dynamical value ; that is , far from a constant single number found in earlier analytical work and commonly used in the literature .
Moreover , the evaporation rate derived with these simulations is higher than values previously published .
These models also show that the value of the mass evaporation rate depends on the strength of the tidal field .
We give an analytical estimate of the mass evaporation rate as a function of time and galactocentric distance \xi ( R _ { GC } ,t ) .
Upon extrapolating this formula to smaller R _ { GC } values , our results provide tentative evidence for a very high \xi value at small R _ { GC } .
Our results suggest that the corresponding mass loss in the inner Galactic potential could be high and it should be accounted for when star clusters pass within it .
This has direct relevance to nuclear cluster formation/growth via the infall of globular clusters through dynamical friction .
As an illustrative example , we estimate how the evaporation rate increases for a \sim 10 ^ { 5 } M _ { \odot } globular cluster that decays through dynamical friction into the galactic centre .
We discuss the findings of this work in relation to the formation of nuclear star clusters by inspiraling globular clusters .