  We investigate whether triggering of the magnetorotational instability (MRI)
in protoplanetary discs can account for the wide diversity of observed
accretion outbursts. We show that short-lived, relatively low accretion rate
events probably result from triggering in the inner disc and can occur at low
surface densities, comparable to or smaller than the minimum mass solar nebula,
and thus are very unlikely to result from MRI triggering by gravitational
instability. We develop time-dependent accretion disc models using an
$\alpha$-viscosity approach and calculate light curves to compare with
observations. Our modeling indicates that the lag time between infrared and
optical bursts seen in Gaia 17bpi can be explained with an outside-in
propagation with an $\alpha \sim 0.1$ in the MRI-active region, consistent with
other estimates. While outbursts in inner discs can show time delays of a few
years between infrared and optical light curves, our models indicate that
large, FU Ori-like bursts can exhibit infrared precursors decades before
optical bursts. Detecting such precursors could enable analysis of the central
star before it is overwhelmed by the rapid accreting material, as well as
constraining outburst physics. Our results emphasize the importance of
near-infrared monitoring of young stellar objects in addition to optical
surveys. In addition, our findings emphasize the need for more sophisticated,
three-dimensional, non-ideal magnetohydrodynamic simulations to fully exploit
observational results.
