  Eclipsing systems, such as transiting exoplanets, allow one to measure the
mean stellar density of the host star under various idealized assumptions.
Asterodensity Profiling (AP) compares this density to an independently
determined value in order to check the validity of the assumptions and
ultimately derive useful parameters. Several physical effects can cause said
assumptions to become invalid, with the most well-known example being the
so-called photo-eccentric effect. In this work, we provide analytic expressions
for five other effects which induce AP deviations: the photo-blend, -spot,
-timing, -duration and -mass effects. We find that these effects can easily
reproduce large AP deviations and so we caution that extracting the
eccentricity distribution is only viable with careful consideration of the
prior distributions for these other effects. We also re-investigate the
photo-eccentric effect and derive a single-domain minimum eccentricity
expression and the parameter range for which analytic formulae are valid. This
latter result shows that the assumptions underlying the analytic model for the
photo-eccentric effect break down for close-in, highly-eccentric planets,
meaning that extreme care must be taken in this regime. Finally, we demonstrate
that contaminated light fraction can be solved for, indicating that AP could be
a potent tool for planet validation.
