  Numerical simulations were carried out to study the origin of multiple
stellar populations in the intermediate-age clusters NGC 411 and NGC 1806 in
the Magellanic Clouds. We performed NBODY6++ simulations based on two different
formation scenarios, an ad hoc formation model where second-generation (SG)
stars are formed inside a cluster of first-generation (FG) stars using the gas
accumulated from the external intergalactic medium and a minor merger model of
unequal mass ($M_{SG}$/$M_{FG}$ ~5-10%) clusters with an age difference of a
few hundred million years. We compared our results such as the radial profile
of the SG-to-FG number ratio with observations on the assumption that the SG
stars in the observations are composed of cluster members, and confirmed that
both the ad hoc formation and merger scenarios reproduce the observed radial
trend of the SG-to-FG number ratio which shows less centrally concentrated SG
than FG stars. It is difficult to constrain the formation scenario for the
multiple populations by only using the spatial distribution of the SG stars. SG
stars originating from the merger scenario show a significant velocity
anisotropy and rotational features compared to those from the ad hoc formation
scenario. Thus, observations aimed at kinematic properties like velocity
anisotropy or rotational velocities for SG stars should be obtained to better
understand the formation of the multiple populations in these clusters. This
is, however, beyond current instrumentation capabilities.
