  We study the secular evolution of a particle in deep mean motion resonance
(MMR) with a planet in the planar elliptic restricted three body problem. We do
not consider any restriction neither in the planet's eccentricity $e_p$ nor in
the particle's eccentricity $e$. The methodology used is based on a
semi-analytical model that consists on calculating the averaged resonant
disturbing function numerically, assuming for this that in the resonant scale
of time all the orbital elements of the particle are constant. In order to
obtain the secular evolution inside the MMR, we make use of the adiabatic
invariance principle, assuming a zero-amplitude resonant libration. We
construct two-dimensional surfaces (called $\mathcal{H}$ surfaces) in the
three-dimensional space $(\sigma, e, \varpi)$ that allow us to predict the
secular evolution of these three variables. The 2:1 MMR is used as example to
show some results. We found four apsidal corotation resonance (ACR) families,
two symmetric and two asymmetric. One of the symmetric families exists for
almost any $e_p$ value. The other one for $e_p>0.3$ and the asymmetric ones for
$e_p>0.44$. We corroborate the secular variations in $e$ and $\varpi$ predicted
by the model through numerical integrations even when the initial conditions
are displaced from those ACR. Some peculiar examples are presented for the 3:1
and 3:2 MMR showing large excursions in eccentricity. As an application, the
Planet 9 is investigated as a possible responsible of high eccentric distant
TNOs.
