  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 $n_{\rm GC}\propto
r^{-\alpha}$. 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 $\alpha\sim3.5$. 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
$\alpha\sim3.5$, 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.
