We consider the general problem of the tidal capture or circularisation from large eccentricity of a uniformly rotating object .
We extend the self-adjoint formalism introduced in our recent paper ( Papaloizou & Ivanov 2005 hereafter PI ) ) to derive general expressions for the energy and angular momentum transfered when the planet or a star passes through periastron in a parabolic or highly eccentric orbit around a central mass .
These can be used without making a low frequency approximation as was done in PI .
We show how these can be adapted to the low frequency limit in which only inertial modes contribute for baratropic planet models .
In order to make quantitative estimates , we calculate the inertial mode eigenspectrum for planet models of one and five Jupiter masses M _ { J } , without a solid core , with different radii corresponding to different ages .
The spectra are found in general to be more complex than of a polytrope with index n = 1.5 , considered in PI , because of the existence global modes associated with the transition from molecular to metallic Hydrogen .
Nonetheless the main tidal response is still found to be determined by two global modes which have polytropic counterparts .

These also determine the uniform angular velocity in a state of pseudo synchronisation , for which the angular momentum transfered during an encounter is zero .
This is found to be close to 1.55 times the circular orbit angular velocity at periastron for all models considered .
This is in contrast to the situation when only the f mode is considered ( Ivanov & Papaloizou 2004 , hereafter IP ) and the equilibrium angular velocity is found to be much larger .

We consider the multi-passage problem when there is no dissipation finding that stochastic instability resulting in the stochastic gain of inertial mode energy over many periastron passages occurs under similar conditions to those already found by IP for the f modes .
We find that this requires circularisation to start with a semi-major axis exceeding \sim 30 AU, for final periods of \sim 3 days .
reducing to \sim 1 - 2 AU for final periods \sim 1.2 days .

Finally we apply our calculations of the energy transfer during a periastron passage to the problem of the tidal circularisation of the orbits of the extrasolar planets in a state of pseudo synchronisation , expected because of the relatively small inertia of the planet , and find that inertial mode excitation dominates the tidal interaction for 1 M _ { J } planets that start with semi- major axes less than 10 AU and end up on circular orbits with final period in the 4 - 6 day range .
It is potentially able to account for initial circularisation up to a final 6 day period within a few Gyr But in the case of 5 M _ { J } oscillation modes excited in the star are more important .