EPoS Contribution

The interaction between outflows and filaments, and its effect on star formation Seamus Clarke ASIAA, Taipei, TW
It is well known that the majority of stars are born in dense gas filaments, and that the primary feedback mechanism of low-mass protostars is the launching of outflows. However, it is not clear how these two features interact and what effect this interaction has on the star formation process. In this work, I will present a set of 18 simulations of accreting, non-equilibrium filaments which fragment into multiple cores, half of which include outflow feedback and half without (see figure). These simulations cover the evolution of ~ 1 pc long filaments down to 2 AU resolution, covering the filament scale down to the protostellar disk. The embedded nature of the cores mean that the continuous gas flows from the parent filament promote the formation of highly unstable multiple systems, with no clear preferred orientation between the outflows and the filament axis. Thus, on the large-scale the majority of the outflows quickly puncture the filament and escape into the surrounding gas. This leads to the outflows having little effect on a filament's internal structure, radius or line-mass. Further, because of their rapid escape from the filament (~1-2 kyrs) outflows are unable to drive and maintain long-term turbulence in the dense gas. However, on the core scale, outflows shape the accretion of material from the filament down to the disk which ultimately reduces the star formation efficiency by a factor of 2. We find that this reduction is remarkably constant over time (across ~200 kyrs after the first star formed), suggesting a form of self-regulation between the outflows and the accretion flows.

Caption: A time evolution (from top to bottom) of two identical simulations of an accreting filament with (right) and without (left) outflow feedback included.
Collaborators: T. Wendt, UzK, DE S. Walch, UzK, DE	Key publication Relevant topic(s): Filaments Outflows
Relevant Big Question: How do outflows affect the star formation process in the filament paradigm?