Using high-resolution N-body simulations , we examine whether a major dry merger mitigates the difference in the radial density distributions between red and blue globular clusters ( GCs ) .
To this end , we study the relation between the density slope of the GCs in merger progenitors and that in a merger remnant , when the density distribution is described by n _ { GC } \propto r ^ { - \alpha } .
We also study how our results depend on the merger orbit and the size of the core radius of the initial GC density distribution .
We find that a major dry merger makes the GC profile flatter , and the steeper initial GC profile leads to more significant flattening , especially if the initial slope is steeper than \alpha \sim 3.5 .
Our result suggests that if there is a major dry merger of elliptical galaxies whose red GCs have a steeper radial profile than the blue GCs , as currently observed , and their slopes are steeper than \alpha \sim 3.5 , the difference in the slopes between two populations becomes smaller after dry mergers .
Therefore , the observed slopes of red and blue GCs can be a diagnostic of the importance of dry merger .
The current observational data show that the red and blue GCs have more comparable and shallower slopes in some luminous galaxies , which may indicate that they have experienced dry mergers .