Coronal mass ejections (CMEs) are among the most energetic and powerful solar phenomena. The CMEs transfer solar energetic particles to the Earth and cause geomagnetic storms, which can produce severe space weather conditions. Previous studies have found that the CME plasmas are strongly heated in the low solar corona. Also, ion charge compositions from in situ measurements have shown that ionization state models require strong and rapid heating around 2 R⊙. In addition, solar coronal plasma is often interpreted assuming equilibrium ionization and Maxwellian electron velocity distributions. But, if the thermodynamical timescale in a rapidly evolving system is shorter than the ionization and recombination timescale, then the plasma can be far from the equilibrium ionization state because of rapid heating or cooling. Non-Maxwellian electron distributions can be caused by particle acceleration, turbulence, or shocks. High-energy observations show that their particle velocity distributions reveal suprathermal tails, which Kappa (κ) distribution functions can represent. In this talk, I introduce previous studies of the heating of CME plasmas using the observations by UV coronagraph spectrometer and EUV and X-ray imaging observations. And I present how we study the heating of the nonequilibrium state coronal plasmas by comparing in situ observations such as interplanetary coronal mass ejection and solar wind.