Disk Wind Feedback from High-mass Protostars
Artikel i vetenskaplig tidskrift, 2019

We perform a sequence of 3D magnetohydrodynamic (MHD) simulations of the outflow-core interaction for a massive protostar forming via collapse of an initial cloud core of 60 M-circle dot. This allows us to characterize the properties of disk-wind-driven outflows from massive protostars, which can allow testing of different massive star formation theories. It also enables us to assess quantitatively the impact of outflow feedback on protostellar core morphology and overall star formation efficiency (SFE). We find that the opening angle of the flow increases with increasing protostellar mass, in agreement with a simple semianalytic model. Once the protostar reaches similar to 24 M-circle dot, the outflow's opening angle is so wide that it has blown away most of the envelope, thereby nearly ending its own accretion. We thus find an overall SFE, of similar to 50%, similar to that expected from low-mass protostellar cores. Our simulation results therefore indicate that the MHD disk wind outflow is the dominant feedback mechanism for helping to shape the stellar initial mass function from a given prestellar core mass function.

stars: formation

stars: massive

stars: winds, outflows

Författare

Jan E. Staff

Univ Virgin Isl, Coll Sci & Math

Kei E.I. Tanaka

National Astronomical Observatory of Japan

Osaka University

Jonathan Tan

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik, Galaktisk astrofysik

Astrophysical Journal

0004-637X (ISSN) 1538-4357 (eISSN)

Vol. 882 2 123

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.3847/1538-4357/ab36b3

Mer information

Senast uppdaterat

2019-11-11