Hot accretion flow around neutron stars

Abstract

We perform as the first time hydrodynamic simulations to study the properties of hot accretion flow (HAF) around a neutron star (NS). The energy carried by the HAF will eventually be radiated out at the surface of the NS. The emitted photons can propagate inside the HAF and cool the HAF via Comptonization. We find that the Compton cooling can affect the properties of HAF around a NS significantly. We define the Eddington accretion rate as ${\dot{M}}_{\mathrm{Edd}}=10L_{\mathrm{Edd}}/c^2$, with $L_{\mathrm{Edd}}$ and $c$ being the Eddington luminosity and the speed of light, respectively. We define $\dot{m}$ as the mass accretion rate at the NS surface in unit of ${\dot{M}}_{\mathrm{Edd}}$. When $\dot{m}>10^{-4}$, Compton cooling can effectively cool the HAF and suppress wind. Therefore, the mass accretion rate is almost a constant with radius. The density profile is $\rho \propto r^{-1.4}$. When $\dot{m}<10^{-4}$, the Compton cooling effects become weaker, wind becomes stronger, accretion rate is proportional to $r^{0.3-0.5}$. Consequently, the density profile becomes flatter, $\rho \propto r^{-1\sim -0.8}$. When $\dot{m}<10^{-6}$, the Compton cooling effects can be neglected. We find that with a same accretion rate, the temperature of HAF around a NS is significantly lower than that of HAF around a black hole (BH). Also, the Compton $y-$parameter of HAF around a NS is significantly smaller than that of HAF around a BH. This result predicts that HAF around a NS will produce a softer spectrum compared to HAF around a BH, which is consistent with observations.

11 pages, 5 figures, accepted by ApJ

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Cited by in corpus (2)

• A systematic study of the advection-dominated accretion flow for the origin of the X-ray emission in weakly magnetized low-level accreting neutron star
• Two-temperature radiative hot accretion flow around neutron stars