AC1 - Spectral and Temporal properties of Black Holes and neutron stars and the theoretical models |
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Speaker |
Bhattacharjee, Ayan |
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Coauthors |
Chakrabarti, Sandip K. |
| Talk Title |
Formation of Two-Component Advective Flows around Neutron Stars |
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Abstract |
We use the Smoothed Particle Hydrodynamics method to simulate the behaviour of both inviscid and viscous matter accreting on a neutron star. The fundamental difference between accretion onto black holes and neutron stars is the presence of a hard surface for the latter. We show that for an advective flow with nominal viscosity and angular momentum, the solution allows two shocks in the flow. The outer one, forms due to a strong centrifugal barrier and is called CENtrifugal pressure dominated Boundary Layer or CENBOL, which is a common feature for both neutron stars and black holes. The inner shock or Normal Boundary Layer (NBOL) forms very close to the surface of a neutron star, due to the presence of the physical boundary. In presence of strong cooling (blackbody emission from the optically thick region), a disk is formed along the equatorial plane. The two-components, disk, and halo are disaggregated out of the halo component and remains steadily oscillating. Our results capture both the low and high-frequency quasi-periodic oscillations. We also compute the spectra and compare with a few observed cases. This indicates that the TCAF is the most general flow configuration for a neutron star when the magnetic field is weak. |
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