  We propose a toy model of Dark Energy in which the degrees of freedom
currently dominating the energy density of the universe are described by a
pseudo-scalar "axion field" linearly coupled to the Pontryagin density, $
\text{tr}(F \wedge F)$, i.e., the exterior derivative of the Chern-Simons form,
of a gauge field. We assume that the axion has self-interactions corresponding
to an exponential potential. We argue that a non-vanishing magnetic helicity of
the gauge field leads to slow-rolling of the axion at field values far below
the Planck scale. Our proposal suggests a "Tracking Dark Energy Scenario" in
which the contribution of the axion energy density to the total energy density
is constant (and small), during the early radiation phase, until a secular
growth term proportional to the Pontryagin density of the gauge field becomes
dominant. The initially small contribution of the axion field to the total
energy density is related to the observed small baryon-to-entropy ratio.
