  We explore the chemistry and observability of nitrogen dominated atmospheres
for ultra-short-period super-Earths. We base the assumption, that super-Earths
could have nitrogen filled atmospheres, on observations of 55 Cnc e that favour
a scenario with a high-mean-molecular-weight atmosphere. We take Titan's
elemental budget as our starting point and using chemical kinetics compute a
large range of possible compositions for a hot super-Earth. We use analytical
temperature profiles and explore a parameter space spanning orders of magnitude
in C/O \& N/O ratios, while always keeping nitrogen the dominant component. We
generate synthetic transmission and emission spectra and assess their potential
observability with the future James Webb Space Telescope and ARIEL. Our results
suggest that HCN is a strong indicator of a high C/O ratio, which is similar to
what is found for H-dominated atmospheres. We find that these worlds are likely
to possess C/O > 1.0, and that HCN, CN, CO should be the primary molecules to
be searched for in thermal emission. For lower temperatures (T < 1500 K), we
additionally find NH3 in high N/O ratio cases, and C2H4, CH4 in low N/O ratio
cases to be strong absorbers. Depletion of hydrogen in such atmospheres would
make CN, CO and NO exceptionally prominent molecules to look for in the 0.6 -
5.0 $\mu$m range. Our models show that the upcoming JWST and ARIEL missions
will be able to distinguish atmospheric compositions of ultra-short period
super-Earths with unprecedented confidence.
