SIMBAD references

Numerical simulations of radiative two-temperature hot accretion flows (HAFs) around Neutron stars (NSs) are performed. We assume that all of the energy carried by the HAF around a NS will be thermalized and radiated out at the surface of the NS. The thermal photons will propagate outwards radially and cool the HAF via Comptonization. We define {dot}m as the mass accretion rate at the surface of the central object in unit of Eddington accretion rate ({dot}M_Edd=10L_Edd/c², with L_Edd and c being Eddington luminosity and speed of light, respectively). When {dot}m is lower than ∼10^–4, the cooling of the HAF is not important and outflows are very strong. When {dot}m> ∼10^–3, cooling becomes important and outflows are significantly weak. In the range 10^–4< {dot}m< 10^–3, the HAFs transients from a strong outflow phase to a very weak outflow phase with increase of {dot}m. The properties of the HAF around a NS are also compared with those of the HAF around a BH. We find that with a similar {dot}m, the dynamical properties of the HAF around a NS are quite similar as those of the HAF around a BH. However, the emitted spectrum of a HAF around a NS can be quite different from that of a HAF around a BH due to the presence of a thermal soft X-ray component coming from the surface of the NS.