  We investigate the tidal interactions of a red giant with a main sequence in
the dense stellar core of globular clusters by Smoothed Particle Hydrodynamics
method. Two models of $0.8 \msun$ red giant with the surface radii 20 and $85
R_\sun$ are used with 0.6 or $0.8M_\sun$ main sequence star treated as a point
mass. We demonstrate that even for the wide encounters that two stars fly
apart, the angular momentum of orbital motion can be deposited into the red
giant envelope to such an extent as to trigger rotational mixing and to explain
the fast rotation observed for the horizontal branch stars, and also that
sufficient mass can be accreted on the main sequence stars to disguise their
surface convective zone with the matter from the red giant envelope. On the
basis of the present results, we discuss the parameter dependence of these
transfer characteristics with non-linear effects taken into account, and derive
fitting formulae to give the amounts of energy and angular momentum deposited
into the red giant and of mass accreted onto the perturber as functions of
stellar parameters and the impact parameter of encounter. These formulae are
applicable to the encounters not only of the red giants but also of the main
sequence stars, and useful in the study of the evolution of stellar systems
with the star-star interactions taken into account.
