  We present the analysis of publicly available NuSTAR, Suzaku and XMM-Newton
observations of the symbiotic recurrent nova T CrB covering the 2006.77-2022.66
yr period. The X-ray spectra are analysed by adopting a model that includes a
reflection component produced by the presence of a disk that mimics the
accretion disk and the immediate surrounding medium. Our best-fit model
requires this disk to have a radius of 1 AU, effective thickness of 0.1 AU,
averaged column density 10$^{25}$ cm$^{-2}$ and orientation of 50$^{\circ}$
with respect to the line of sight. This disk is about a factor of two larger
than recent estimations for the accretion disk and its presence contributes
significantly via reflection to the total X-ray flux detected from T CrB, which
naturally produces the emission of the 6.4 keV Fe line. Our analysis suggests
that the temperature of the boundary layer evolved from 14.8 keV in the
steady-state phase (before 2016), to 2.8 keV in the 2017.24 epoch, to finally
stabilise to about $\sim$8 keV in the subsequent epochs. These variations in
the plasma temperature of the boundary layer are attributed to the evolution of
the mass accretion rate ($\dot{M}_\mathrm{acc}$), which is estimated to have an
averaged value of $\dot{M}_\mathrm{acc}$=2.6$\times10^{-8}$ M$_\odot$ yr$^{-1}$
for the current active phase. The presence of emission lines in the XMM-Newton
RGS spectrum of 2017.24 prevents from adopting a black body emission model to
fit the soft X-ray range. Instead, we use plasma emission models that suggest
the presence of adiabatically-shocked gas produced by gas velocities of 110-200
km s$^{-1}$, very likely tracing jet-like ejections similar to what is found in
other symbiotic systems. The analysis of X-ray and optical data together show
that T CrB has a similar evolution as black hole binaries, accreting neutron
stars and AGN in the hardness-intensity diagram.
