  We introduce ECCOplanets, an open-source Python code that simulates
condensation in the protoplanetary disk. Our aim is to analyse how well a
simplistic model can reproduce the main characteristics of rocky planet
formation. For this purpose, we revisited condensation temperatures ($T_c$) as
a means to study disk chemistry, and explored their sensitivity to variations
in pressure (p) and elemental abundance pattern. We also examined the bulk
compositions of rocky planets around chemically diverse stars. Our
T-p-dependent chemical equilibrium model is based on a Gibbs free energy
minimisation. We derived condensation temperatures for Solar System parameters
with a simulation limited to the most common chemical species. We assessed
their change ($\Delta T_c$) as a result of p-variation between $10^{-6}$ and
0.1 bar. To analyse the influence of the abundance pattern, key element ratios
were varied, and the results were validated using solar neighbourhood stars. To
derive the bulk compositions of planets, we explored three different planetary
feeding-zone (FZ) models and compared their output to an external n-body
simulation. Our model reproduces the external results well in all tests. For
common planet-building elements, we derive a Tc that is within $\pm5$ K of
literature values, taking a wider spectrum of components into account. The Tc
is sensitive to variations in p and the abundance pattern. For most elements,
it rises with p and metallicity. The tested pressure range ($10^{-6} - 0.1$
bar) corresponds to $\Delta T_c \approx +350$ K, and for -0.3 $\leq$ [M/H]
$\leq$ 0.4 we find $\Delta T_c \approx +100$ K. An increase in C/O from 0.1 to
0.7 results in a decrease of $\Delta T_c \approx -100$ K. Other element ratios
are less influential. Dynamic planetary accretion can be emulated well with any
FZ model. Their width can be adapted to reproduce gradual changes in planetary
composition.
