Structural Parameters for Globular Clusters in the Outer Halo of M31
  In this paper, we present internal surface brightness profiles, using images
in the F606W and F814W filter bands observed with the Advanced Camera for
Surveys on the {\it Hubble Space Telescope}, for ten globular clusters (GCs) in
the outer halo of M31. Standard King models are fitted to the profiles to
derive their structural and dynamical parameters. The results show that, in
general, the properties of clusters in M31 and the Milky Way fall in the same
regions of parameter spaces. The outer halo GCs of M31 have larger
ellipticities than most of GCs in M31 and the Milky Way. Their large
ellipticities may be due to galaxy tides coming from satellite dwarf galaxies
of M31 or may be related to the apparently more vigorous accretion or merger
history that M31 has experienced. The tight correlation of cluster binding
energy $E_b$ with mass $M_{\rm mod}$ indicates that, the "fundamental plane"
does exist for clusters, regardless of their host environments, which is
consistent with previous studies.
