http://arxiv.org/abs/1712.08295
We run two GRRMHD simulations of super-Eddington accretion disks around a black hole and a neutron star. We observe the formation of a boundary layer in the neutron star simulation which leads to a larger mass outflow rate and a lower radiative luminosity over the black hole case. Sphereization of the flow leads to an observable luminosity at infinity around the Eddington value for the neutron star case, contrasting to the black hole case where collimation of the emission leads to observable luminosities about an order of magnitude higher. We find the outflow to be optically thick to scattering, which would lead to the obscuring of any neutron star pulsations observed in corresponding ULXs.
D. Abarca, W. Kluzniak and A. Sadowski
Mon, 25 Dec 17
33/37
Comments: 13 pages, 11 figures, submitted to Monthly Notices of the Royal Astronomical Society
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