  Coronal Mass Ejections (CMEs) are the most energetic expulsions of magnetized
plasma from the Sun that play a crucial role in space weather dynamics. This
study investigates the diverse kinematics and thermodynamic evolution of two
CMEs (CME1: 2011 September 24 and CME2: 2018 August 20) at coronal heights
where thermodynamic measurements are limited. The peak 3D propagation speed of
CME1 is high (1,885 km/s) with two-phase expansion (rapid and nearly constant),
while the peak 3D propagation speed of CME2 is slow (420 km/s) with only a
gradual expansion. We estimate the distance-dependent variations in the
polytropic index, heating rate, temperature, and internal forces implementing
the revised FRIS model, taking inputs of 3D kinematics estimated from the GCS
model. We find CME1 exhibiting heat-release during its early-rapid acceleration
decrease and jumps to the heat-absorption state during its constant
acceleration phase. In contrast to CME1, CME2 shows a gradual transition from
the near-adiabatic to the heat-absorption state during its gradually increasing
acceleration. Our analysis reveals that although both CMEs show differential
heating, they experience heat-absorption during their later propagation phases,
approaching the isothermal state. The faster CME1 achieves an adiabatic state
followed by an isothermal state at smaller distances from the Sun than the
slower CME2. We also find that the expansion of CMEs is primarily influenced by
centrifugal and thermal pressure forces, with the Lorentz force impeding
expansion. Multi-wavelength observations of flux-ropes at source regions
support the FRIS model-derived findings at initially observed lower coronal
heights.
