  It has long been known that the radial density profiles of globular cluster
systems (GCSs) in elliptical galaxies vary with the total luminosities of their
host galaxies. In order to elucidate the origin of this structural non-homology
in GCSs, we numerically investigate the structural properties of GCSs in
elliptical galaxies formed from a sequence of major dissipationless galaxy
merging. We find that the radial density profiles of GCSs in elliptical
galaxies become progressively flatter as the galaxies experience more major
merger events. The density profiles of GCSs in ellipticals are well described
as power-laws with slopes (${\alpha}_{\rm gc}$) ranging from -2.0 to -1.0. They
are flatter than, and linearly proportional to, the slopes (${\alpha}_{\rm s}$)
of the stellar density profiles of their host galaxies. We also find that the
GCS core radii ($r_{\rm c}$) of the density profiles are larger in ellipticals
that experienced more mergers. By applying a reasonable scaling relation
between luminosities and sizes of galaxies to the simulation results, we show
that ${\alpha}_{\rm gc} \approx -0.36 M_{\rm V}-9.2$, $r_{\rm c} \approx -1.85
M_{\rm V}$, and ${\alpha}_{\rm gc} \approx 0.93 {\alpha}_{\rm s}$, where
$M_{\rm V}$ is the total $V$-band absolute magnitude of a galaxy.
