Massive Star Formation via High Accretion Rates and Early Disk-driven Outflows

@article{Banerjee2007MassiveSF,
  title={Massive Star Formation via High Accretion Rates and Early Disk-driven Outflows},
  author={Robi Banerjee and Ralph E. Pudritz},
  journal={The Astrophysical Journal},
  year={2007},
  volume={660},
  pages={479 - 488}
}
We present an investigation of the massive star formation that results from the gravitational collapse of massive, magnetized molecular cloud cores. We investigate this by means of highly resolved, numerical simulations of initial magnetized Bonnor-Ebert-spheres that undergo collapse and cooling. By comparing three different cases—an isothermal collapse, a collapse with radiative cooling, and a magnetized collapse—we show that massive stars assemble quickly, with mass accretion rates exceeding… 
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References

SHOWING 1-10 OF 40 REFERENCES
Supersonic turbulence, filamentary accretion and the rapid assembly of massive stars and discs
We present a detailed computational study of the assembly of protostellar discs and massive stars in molecular clouds with supersonic turbulence. We follow the evolution of large-scale filamentary
Collapse-Driven Outflow in Star-Forming Molecular Cores
Dynamical collapses of magnetized molecular cloud cores are studied with magnetohydrodynamic simulations from the runaway collapse phase to the accretion phase. In the runaway collapse phase, a disk
Outflows and Jets from Collapsing Magnetized Cloud Cores
Star formation is usually accompanied by outflow phenomena. There is strong evidence that these outflows and jets are launched from protostellar disks by magnetorotational processes. Here we report
The formation of a massive protostar through the disk accretion of gas
TLDR
Observations that clearly show a massive star being born from a large rotating accretion disk, where the protostar has already assembled about 20 solar masses, and the accretion process is still going on.
Massive star formation in 100,000 years from turbulent and pressurized molecular clouds
TLDR
It is shown that t*f is determined by the conditions in the star's natal cloud, and is typically ∼105 yr, which is sufficient to overcome radiation pressure from ∼100M[circdot] protostars, while simultaneously driving intense bipolar gas outflows.
On the Formation of Massive Stars
We calculate numerically the collapse of slowly rotating, nonmagnetic, massive molecular clumps of masses 30, 60, and 120 M☉, which conceivably could lead to the formation of massive stars. Because
The Formation of Massive Stars from Turbulent Cores
Observations indicate that massive stars in the Galaxy form in regions of very high surface density, Σ ~ 1 g cm-2. Clusters containing massive stars and globular clusters have a column density
A Remnant Disk around a Young Massive Star
While the formation of low-mass stars has become a well-studied process, it is still difficult to verify a similar evolutionary sequence for massive stars. Although several young stages from massive
The Formation of the First Star in the Universe
TLDR
It is concluded that at most one massive metal-free star forms per pregalactic halo, consistent with recent abundance measurements of metal-poor galactic halo stars.
First MHD simulation of collapse and fragmentation of magnetized molecular cloud cores
This is the first paper about fragmentation and mass outflow in molecular clouds by using three-dimensional magnetohydrodynamical (MHD) nested-grid simulations. The binary star formation process is
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