Going with the Outflow

Title: Zooming into the Collimation Zone in a Massive Protostellar Jet

Authors: Carlos Carrasco-González, Alberto Sanna, Adriana Rodríguez-Kamenetzky, Luca Moscadelli, Melvin Hoare, José M. Torrelles, Roberto Galván-Madrid, and Andrés F. Izquierdo

First Author’s Institution: Instituto de Radioastronomía y Astrofísica (IRyA-UNAM), Morelia, Mexico

Status: accepted for publication in ApJ Letters

Stars do not form quietly. As clumps of gas collapse in on themselves within the densest, coldest depths of interstellar molecular clouds, the precursors to stars (protostars) accrete mass from their surroundings, but they also launch matter away at incredible speeds (up to hundreds of kilometers per second!) in beam-like or conical formations of interstellar wind. These “protostellar jets,” also known as “outflows” or “bipolar winds” are powerful influences on the surrounding interstellar medium, and are thought to be powered by the interaction of the matter falling onto the protostar and the magnetic fields surrounding the protostar. The exact nature of how protostellar jets are launched remains an area of active research. A particularly elusive mystery is whether the physical mechanism responsible for launching these jets might act differently depending on the mass of the protostar. Today’s paper takes the closest look yet at the outflows from a massive protostar, a critical step in understanding the intricacies of the early stages of star formation.

Figure 1: an artist’s rendering of the dust enshrouded origins of a protostellar jet. As gas accretes onto the central protostar, a high velocity wind of matter is accelerated in a beam perpendicular to the disk. Image credit: NASA/JPL-Caltech/R. Hurt (SSC)

Low Mass vs. High Mass Jets

Studying the origin of protostellar jets is really tricky. These jets travel enormous distances and can affect their surroundings up to parsecs away, but if we want to understand the physics behind driving them, we must carefully observe the region where they originate, in close proximity to their parent protostar. Unfortunately, even with the most powerful radio telescopes, we can’t observe down to those kinds of physical scales for all but a handful of nearby star forming regions. Recent high resolution surveys of star forming regions have revealed many of the details of protostellar outflows around the precursors of lower mass stars (M < 8 solar masses or so), as described in this recent bite! More massive O and B type stars, however, are considerably more rare, and in astronomy, rarer things tend to be further away, on average. That means we don’t have a lot of nearby massive protostars to study, and the further away the protostar is, the better the angular resolution required to resolve the fine details needed to understand how these jets are launched.

However, the outflows from massive (O / B type) protostars are thought to be notably different from the winds from their low mass counterparts. It seems the the outflows from massive protostars are commonly less beam-like, (or “collimated“) and it is thought that they might have an entirely different physical mechanism responsible for the large scale parallel structure of their jets. Instead of the protostar’s local magnetic field being responsible for the beam-like linearity of the outflow, it’s possible that massive stars eject mass wildly in nearly all directions, and the ambient magnetic fields of the protostar’s surroundings are responsible for collimating the beam. It’s impossible to determine the truth of the matter without high resolution observations of the immediate surroundings of massive protostars.

Figure 2: the authors’ modeling of the innermost hundred au of the massive protostellar jet Cepheus A HW2. Upper left: the VLA radio image of the protostellar jet. The right three panels show the piecewise construction of the outflow model for a collimated jet, a conical wind, and the combination of both. The bottom left panel shows the model adjusted to fit the outflow angles and mass loss rates of the observed source.

The Closest Look Yet…

Today’s paper takes the highest resolution look yet at the massive protostar Cepheus A HW2, one of the nearest massive protostars with a known outflow. Using the Very Large Array (VLA), the authors are able to resolve the inner workings of the protostellar jet’s origin, on scales down to 20 astronomical units (au). The inner 100 au of this protostar has some key differences to the morphology of its low-mass counterparts, and is visualized in figure 1. By modeling the observed jets, the authors characterize the outflow as having both a cone-like component nearby to the protostar as well as a collimated, beam-like component that kicks in further out.

Figure 3: a comparison of the VLA image of Cepheus A HW2 (upper) with a cartoon schematic showing how a disordered distribution of protostellar winds might be collimated into a beam-like jet of outflowing mass.

The authors suggest a couple interpretations for this fascinating system. Firstly, it’s possible that the same physics is responsible for launching highly collimated jets for both high and low mass stars, but the high mass stars tend to become collimated further away from the protostar. Secondly it might be that the high mass protostars produce more disordered winds on their own, blowing away mass in wide cones or even spherically, and the magnetic ambient environment is responsible for turning the cone-like winds into a nice beam-like jet. Since so many massive protostars seem to have disordered outflows, it might be that a particularly opportune magnetic field structure in the surrounding cloud is needed to produce collimated jets so commonly seen for their low mass protostars. While this is only one example of such an outflow, it brings us one big step closer to understanding the mysterious and elusive jets from massive protostars.

Astrobite edited by Mitchell Cavanagh

Featured image credit: Figure 3 of the article.

About H Perry Hatchfield

I'm a NASA Postdoctoral Fellow at JPL, where I study star formation and gas structure in the Milky Way's Galactic Center. I do this using multi-wavelength observations of molecular clouds as well as hydrodynamic simulations, and I'm all about trying to find ways to compare these two exciting means of exploring the universe.

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