  The development of space-borne missions has significantly improved the
quality of the measured spectra of solar-like oscillators. Their $p$-mode line
profiles can now be resolved, and the asymmetries inferred for a variety of
stars other than the Sun. However, it has been known for a long time that the
asymmetries of solar $p$-modes are reversed between the velocity and the
intensity spectra. Understanding the origin of this reversal is necessary in
order to use asymmetries as a tool for seismic diagnosis. For stars other than
the Sun, only the intensity power spectrum is sufficiently resolved to allow
for an estimation of mode asymmetries. We recently developed an approach
designed to model and predict these asymmetries in the velocity power spectrum
of the Sun and to successfully compare them to their observationally derived
counterparts. In this paper we expand our model and predict the asymmetries
featured in the intensity power spectrum. We find that the shape of the mode
line profiles in intensity is largely dependent on how the oscillation-induced
variations of the radiative flux are treated, and that modelling it
realistically is crucial to understanding asymmetry reversal. Perturbing a
solar-calibrated grey atmosphere model, and adopting the quasi-adiabatic
framework as a first step, we reproduce the asymmetries observed in the solar
intensity spectrum for low-frequency modes. We conclude that, unlike previously
thought, it is not necessary to invoke an additional mechanism (e.g.
non-adiabatic effects, coherent non-resonant background signal) to explain
asymmetry reversal. This additional mechanism is necessary, however, to explain
asymmetry reversal for higher-order modes.
