Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles

@article{Sun2018SimulatingTM,
  title={Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles},
  author={Lunan Sun and M. Ruiz and S. Shapiro},
  journal={Physical Review D},
  year={2018},
  volume={98},
  pages={103008}
}
Collapsing supermassive stars (SMSs) with masses $M \gtrsim 10^{4-6}M_\odot$ have long been speculated to be the seeds that can grow and become supermassive black holes (SMBHs). We previously performed GRMHD simulations of marginally stable magnetized $\Gamma = 4/3$ polytropes uniformly rotating at the mass-shedding limit to model the direct collapse of SMSs. These configurations are supported entirely by thermal radiation pressure and model SMSs with $M \gtrsim 10^{6}M_\odot$. We found that… Expand

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