  In previous papers, we developed a technique for estimating the inner
eccentricity in hierarchical triple systems, with the inner orbit being
initially circular. We considered systems with well separated components and
different initial setups (e.g. coplanar and non-coplanar orbits). However, the
systems we examined had comparable masses. In the present paper, the validity
of some of the formulae derived previously is tested by numerically integrating
the full equations of motion for systems with smaller mass ratios (from
${10^{-3} \hspace{0.2cm} \mbox{to} \hspace{0.2cm} 10^{3}}$, i.e. systems with
Jupiter-sized bodies). There is also discussion about HD217107 and its
planetary companions.
