  Recent observations have revealed that many solar coronal jets involve the
eruption of miniature versions of large-scale filaments. Such "mini-filaments"
are observed to form along the polarity inversion lines of strong, magnetically
bipolar regions embedded in open (or distantly closing) unipolar field. During
the generation of the jet, the filament becomes unstable and erupts. Recently
we described a model for these mini-filament jets, in which the well-known
magnetic-breakout mechanism for large-scale coronal mass ejections is extended
to these smaller events. In this work we use three-dimensional
magnetohydrodynamic simulations to study in detail three realisations of the
model. We show that the breakout-jet generation mechanism is robust and that
different realisations of the model can explain different observational
features. The results are discussed in relation to recent observations and
previous jet models.
