2024/08/05 by Monu Singh, Singh, Monu, Santabrata Das +1 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE)
paper · pdf · doi:10.48550/arxiv.2408.02256
openalex publication_date 2024/08/05 · openalex created_date 2024/10/14 · openalex updated_date 2026/07/28
We investigate the properties of low angular momentum, relativistic, viscous, advective accretion flows around rotating black holes that include shock waves in the presence of thermal conduction. We self-consistently solve the governing fluid equations to obtain the global transonic accretion solutions for a set of model parameters, namely energy (E), angular momentum (λ), viscosity (α), conduction parameter (Φ\rm s) and cooling parameter (f\rm c). We observe that depending on the model parameters, accretion flow experiences centrifugally supported shock transition and the present study, for the first time, focuses on examining the shock properties, such as shock radius (r\rm s), compression ratio (R) and shock strength (Ψ) regulated by the dissipation parameters (Φ\rm s,~f\rm c). We show that shock-induced global accretion solutions persist for wide range of model parameters and identify the boundary of the parameter space in energy-angular momentum plane that admits standing shocks for different dissipation parameters (Φ\rm s,~f\rm c). Finally, we compute the critical conduction parameter (Φ\rm s\rm cri), beyond which shock ceases to exist. We find that Φ\rm s\rm cri directly depends on the black hole spin (a\rm k) with Φ\rm s\rm cri ∼ 0.029 and ∼ 0.04 for weakly (a\rm k→ 0) and rapidly (a\rm k→ 1) rotating black hole. Furthermore, we observe that Φ\rm s\rm cri decreases with increasing viscosity (α), and shocked accretion solutions continue to exist for α\lesssim 0.065 (a\rm k → 0) and \lesssim 0.104 (a\rm k → 1), respectively.