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The interaction between a YSO stellar magnetic field and its protostellardisc can result in stellar accretional flows and outflows from the inner discrim. Gas flows with a velocity component perpendicular to disc midplane subjectparticles to centrifugal acceleration away from the protostar, resulting inparticles being catapulted across the face of the disc. The ejected materialcan produce a "dust fan", which may be dense enough to mimic the appearance ofa "puffed-up" inner disc rim. We derive analytic equations for the timedependent disc toroidal field, the disc magnetic twist, the size of the stabletoroidal disc region, the jet speed and the disc region of maximal jet flowspeed. We show how the observed infrared variability of the pre-transition discsystem LRLL~31 can be modelled by a dust ejecta fan from the inner-most regionsof the disc whose height is partially dependent on the jet flow speed. Thegreater the jet flow speed, the higher is the potential dust fan scale height.An increase in mass accretion onto the star tends to increase the height andoptical depth of the dust ejection fan, increasing the amount of 1--8~$\mu$mradiation. The subsequent shadow reduces the amount of light falling on theouter disc and decreases the 8-- 40~$\mu$m radiation. A decrease in theaccretion rate reverses this scenario, thereby producing the observed "see-saw"infrared variability.

Infrared Variability due to Magnetic Pressure Driven Jets, Dust Ejection and Quasi-Puffed-Up Inner Rims