  In this work UV and white light (WL) coronagraphic data are combined to
derive the full set of plasma physical parameters along the front of a shock
driven by a Coronal Mass Ejection. Pre-shock plasma density, shock compression
ratio, speed and inclination angle are estimated from WL data, while pre-shock
plasma temperature and outflow velocity are derived from UV data. The
Rankine-Hugoniot (RH) equations for the general case of an oblique shock are
then applied at three points along the front located between $2.2-2.6$
R$_\odot$ at the shock nose and at the two flanks. Stronger field deflection
(by $\sim 46^\circ$), plasma compression (factor $\sim 2.7$) and heating
(factor $\sim 12$) occur at the nose, while heating at the flanks is more
moderate (factor $1.5-3.0$). Starting from a pre-shock corona where protons and
electrons have about the same temperature ($T_p \sim T_e \sim 1.5 \cdot 10^6$
K), temperature increases derived with RH equations could better represent the
protons heating (by dissipation across the shock), while the temperature
increase implied by adiabatic compression (factor $\sim 2$ at the nose, $\sim
1.2-1.5$ at the flanks) could be more representative of electrons heating: the
transit of the shock causes a decoupling between electron and proton
temperatures. Derived magnetic field vector rotations imply a draping of field
lines around the expanding flux rope. The shock turns out to be super-critical
(sub-critical) at the nose (at the flanks), where derived post-shock plasma
parameters can be very well approximated with those derived by assuming a
parallel (perpendicular) shock.
