Paper detail

Waterfalls around protostars: Infall motions towards Class 0/I envelopes as probed by water

Abridged abstract: For stars to form, material must fall inwards from core scales through the envelope towards the central protostar. The velocity profile around protostars is poorly constrained. 6 Class 0 protostars and one Class I protostars observed with HIFI on board Herschel as part of the "Water in star-forming regions with Herschel" (WISH) survey show infall signatures in water line observations. We use 1-D non-LTE RATRAN radiative transfer models of the observed water lines to constrain the infall velocity and chemistry in the protostellar envelopes of these sources. We assume a free-fall velocity profile and, having found the best fit, vary the radii over which infall takes place. In the well-studied Class 0 protostar NGC1333-IRAS4A we find that infall takes place over the whole envelope to which our observations are sensitive (r>~1000 AU). For 4 sources infall takes place on core to envelope scales (i.e. ~10000-3000 AU). In 2 sources the inverse P-Cygni profiles seen in the ground-state lines are more likely due to larger-scale motions or foreground clouds. Models including a simple consideration of the chemistry are consistent with the observations, while using step abundance profiles are not. The non-detection of excited water in the inner envelope in 6/7 protostars is further evidence that water must be heavily depleted from the gas-phase at these radii. Infall in four of the sources is supersonic and infall in all sources must take place at the outer edge of the envelope, which may be evidence that collapse is global or outside-in rather than inside-out. The mass infall rate in IRAS4A is large (>~10^-4 msol\yr), higher than the mass outflow rate and expected mass accretion rates onto the star, suggesting that any flattened disk-like structure on small scales will be gravitationally unstable, potentially leading to rotational fragmentation and/or episodic accretion.