  Although radio relics are understood to originate in intracluster shock waves
resulting from merger shocks, the most widely used model for describing this
(re-)acceleration process at shock fronts, the diffusive shock acceleration
(DSA) model, has several challenges, including the fact that it is inefficient
at low shock Mach numbers. In light of these challenges, it is worthwhile to
consider alternative mechanisms. One possibility is the adiabatic compression
by a shock wave of a residual fossil electron population which has been left
over from a radio galaxy jet. This paper applies this model to the relic hosted
in the merging galaxy cluster Abell 3411-3412, where a radio bridge between the
relic and a radio galaxy has been observed, with the aim to reproduce the
spatial structure of the spectral index of the relic. Four scenarios are
presented, in which different effects are investigated, such as effects behind
the shock front and different shock strengths. The results show that the
adiabatic compression model can reproduce the observed spectral indices across
the relic for a shock Mach number that is lower than the value required by the
DSA-type modelling of this relic and is in accordance with the values derived
from X-ray observations, if other mechanisms, such as an expansion phase or
post-shock turbulence, are effective behind the shock front.
