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tokens: shock front with high velocity, overtakes the older bullets and decelerates. In the last panel, the newly ejected bullet E is in a comparable position as former bullet D in the first frame. The protostar launches outflow bullets labelled A through E corresponding to the left and right outflow lobe. In the remainder of the paper, we will only refer to the left lobe and therefore we drop the subscript L henceforth. The outflow bullets form an S-shaped chain of Herbig–Haro objects. The S-shape is due to the varying orientation of the angular momentum, , caused by anisotropic accretion onto the IAD from core (Ybarra et al. 2006 ; Wu, Takakuwa Lim 2009 ; Zhang et al. 2013 ; Frank et al. 2014 ). The first two bullets interact with the collapsing dense core material and are thus not visible in Fig. 8 . The timespan from 115 kyr to 122 kyr is chosen to capture the end of a cycle of an outflow bullet, here bullet D, when it hits the leading shock front. This cycle happens in a similar fashion for all other bullets, except the first bullet A. This is the first bullet that breaks out of the core and survives as a coherent structure. Bullets B and C have higher velocity and have overtaken A. Bullet D starts off faster still, and by the final frame it has overtaken all the others and hit the leading shock, where it is slowed down. Bullet E is even faster, but by the final frame it has not yet caught up with D and is in a similar position as former bullet D in the first frame. A sixth bullet has been launched, but is still inside the core, and therefore can not be seen on Fig. 8 . Fig. 9 shows the accretion rates onto the sink, and onto the protostar, , between (when the protostar forms) and . is relatively constant, between ∼2 × 10 −5 and . The accretion rate tends to decrease over time. It drops briefly, following an outburst, because the outburst heats the accretion disc (cf. Lomax et al. 2014 , 2015 ). The accretion rate of the protostar is low in the quiescent phase, , but approaches during an outburst. Note that the time resolution in Fig. 9 is too coarse to resolve the very short outbursts. The downtime between outbursts is and the duration of an outburst is (Stamatellos et al. 2007 , 2011b ). Figure 9. Evolution of the accretion rates onto the sink particle, (green), and the protostar, (blue). The labels, A–F, correspond to the outflow bullets formed in the individual outbursts (see Figs. 8 and 10 ). Note that the time resolution in this figure is too coarse to fully resolve the very short outbursts. 4.1 Position–velocity diagrams In order to determine whether the simulated outflow reproduces the ‘Hubble-Law’ relation, and individual ‘Hubble Wedges’, as observed, for example, by Bachiller et al. ( 1990 ); Arce Goodman ( 2001 ); Tafalla et al. ( 2004 ); Santiago-García et al. ( 2009 ); Wang et al. ( 2014 ), we construct PV-diagrams, i.e. false-colour plots of on the plane. Here, r is radial distance, and is radial velocity, both measured from the