In principle, everything in the Universe affects everything else. On the other hand, the strength of these "nonlinear" effects is typically exponentially suppressed. In order to become noticeable, one should overcome some characteristic threshold. So in the case of electromagnetic interactions, you can imagine that if the temperature $T$ of the system you atoms is in (think of some cavity filled with radiation) is such that $k_B T> 2 m_e c^2$, where $m_e$ is the mass of an electron (the lightest known charged particle), then your vacuum will be full of fluctuating electron-positron pairs, which will very efficiently screen any charge, thus turning your long-range Coulomb interaction into a short-ranged screened one.
The same goes for all other interactions, provided the temperatures reach the levels $k_B T \sim Mc^2$, where $M$ now is the mass of the lightest particle that feels the interaction in question (has non-zero corresponding charge).