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 } \hskip { 5.690551 pt } \mbox { to } \hskip { 5.690551 pt } 10 ^ { 3 } } , i.e .
systems with Jupiter-sized bodies ) .
There is also discussion about HD217107 and its planetary companions .