  We present the first three dimensional (3D) Morpho-Kinematic (MK) model of a
supernova remnant (SNR), using as a case study the Galactic SNR VRO 42.05.01.
We employed the astrophysical code SHAPE in which wide field imaging and high
resolution spectroscopic data were utilized, to reconstruct its 3D morphology
and kinematics. We found that the remnant consists of three basic distinctive
components that we call: a "shell", a "wing" and a "hat". With respect to their
kinematical behaviour, we found that the "wing" and the "shell" have similar
expansion velocities (V exp = $115$$\pm 5$ km/s). The "hat" presents the lowest
expansion velocity of the remnant (V exp = $90$$\pm 20$ km/s), while the upper
part of the "shell" presents the highest velocity with respect to the rest of
the remnant (V exp = $155$$\pm 15$ km/s). Furthermore, the whole nebula has an
inclination of ~$3{\deg}- 5{\deg}$ with respect to the plane of the sky and a
systemic velocity of V sys = -$17$$\pm 3$ km/s . We discuss the interpretation
of our model results regarding the origin and evolution of the SNR and we
suggest that VRO 42.05.01 had an interaction history with an inhomogeneous
ambient medium most likely shaped by the mass outflows of its progenitor star.
