  Variable accretion has been well studied in evolved stages of low-mass stars
formation. However, the accretion history in the initial phases of star
formation is still a seldom studied topic. The outflows and jets emerging from
protostellar objects could shed some light onto their accretion history. We
consider the recently studied case of W43-MM1, a protocluster containing 46
outflows driven by 27 protostellar cores. The outflow kinematics of the
individual cores and associated knots in W43-MM1 indicate episodic protostellar
ejection. We took the observed parameters of an individual core system (core
#8) and performed 3D hydrodynamic simulations of such system including episodic
changes in the velocity of the outflow. The simulations consist of a collimated
jet emerging from a core taking into account one- and two-velocity modes in the
variation of the ejection velocity of the jet. In addition, we investigated the
effect of including the precession of the jet to the one- and two-velocity mode
models. From the simulations, we constructed position-velocity diagrams and
compared them with the observations. We find that including a second mode in
the ejection velocity, as well as the precession, are required to explain the
positions of the outflow knots and other position-velocity features observed in
the outflow of core #8 in W43-MM1.
