  The quasi-metric manifold $\cal N$ is equipped with two one-parameter
families of metric tensors ${\bf {\bar g}}_t$ and ${\bf g}_t$, each
parametrized by the global time function $t$. Moreover, in $({\cal N},{\bf
{\bar g}}_t)$ one must define two different electromagnetic field tensor
families corresponding to the active electromagnetic field tensor family ${\bf
{\tilde F}}_t$ and the passive electromagnetic field tensor family ${\bf {\bar
F}}_t$, respectively. The active electromagnetic field tensor family ${\bf
{\tilde F}}_t$ couples to gravity. By construction, the norm of the passive
electromagnetic field tensor family ${\bf {\bar F}}_t$ experiences a secular
decrease, defining a global cosmic attenuation (not noticeable locally) of the
electromagnetic field. Local conservation laws for passive electromagnetism
imply that ${\bf {\bar {\nabla}}}{\cdot} {\bf {\bar F}}_t=0$ in electro-vacuum,
ensuring that photons move on null geodesics of $({\cal N},{\bf {\bar g}}_t)$.
From ${\bf {\bar F}}_t$, one may construct the passive electromagnetic field
tensor family ${\bf F}_t$ in $({\cal N},{\bf g}_t)$ in the same way as ${\bf
g}_t$ is constructed from ${\bf {\bar g}}_t$. This ensures that photons move on
null geodesics of $({\cal N},{\bf g}_t)$ as well. As a simple example, the
(exact) quasi-metric counterpart to the Reissner-Nordstr\"{o}m solution in
General Relativity is calculated. Besides, it is found that a classical charged
test particle electromagnetically bound to a central charge will participate in
the cosmic expansion. But since quantum-mechanical states should be unaffected
by the expansion, this classic calculation is hardly relevant for
quantum-mechanical systems such as atoms, so there is no reason to think that
the cosmic expansion should apply to them. Finally, it is shown that the main
results of geometric optics hold in quasi-metric space-time.
