  The analysis of the mid-infrared spectra helps understanding the composition
of the gas in the inner, dense and warm terrestrial planet forming region of
disks around young stars. ALMA has detected hydrocarbons in the outer regions
of the planet forming disk and Spitzer detected \ce{C2H2} in the inner regions.
JWST- MIRI provides high spectral resolution observations of \ce{C2H2} and a
suite of more complex hydrocarbons are now reported. Interpreting the fluxes
observed in the spectra is challenging and radiation thermo-chemical codes are
needed to properly take into account the disk structure, radiative transfer,
chemistry and thermal balance. Various disk physical parameters like the
gas-to-dust ratio, dust evolution including radial drift, dust growth and
settling can affect the fluxes observed in the mid-IR. Still, thermo-chemical
disk models were not always successful in matching all observed molecular
emission bands simultaneously. The goal of this project is two-fold. We analyse
the warm carbon chemistry in the inner regions of the disk, i.e. within 10 au
to find pathways forming \ce{C2H2} potentially missing from the existing
chemical networks. Second, we analyse the effect of the new chemistry on the
line fluxes of acetylene. We use radiative thermo-chemical disk code {P{\small
RO}D{\small I}M{\small O}} to expand the hydrocarbon chemistry that occurs in a
typical standard T Tauri disks. We used the UMIST and the KIDA rate databases
for collecting reactions for the species. We include a number of three-body and
thermal decomposition reactions from STAND2020 network. We included isotopomers
for the species that were present in the databases. The chemistry is then
analysed in the regions that produce observable features in the mid-infrared
spectra. The effect of expanding the hydrocarbon chemistry on the mid-infrared
spectra is studied. Acetylene is formed via two ....
