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19982022
most citedTwo temperature accretion around rotating black holes: Description of general advective flow paradigm in presence of various cooling processes to explain low to high luminous sources

55 citations · 169 across the 8 of their papers we have counts for

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astro-ph.HE2022

Understanding spectral states of sub-Keplerian accretion discs around compact objects as transitions between steady states

Arunima Ajay, S R Rajesh, Nishant K. Singh

We present here a simple hydrodynamic model based on a sequence of steady states of the inner sub-Keplerian accretion disc to model its spectral states. Correlations between differ…

astro-ph.HE2013

Time variability of viscosity parameter in differentially rotating discs

S. R. Rajesh, Nishant K. Singh

We propose a mechanism to produce fluctuations in the viscosity parameter () in differetially rotating discs. We carried out a nonlinear analysis of a general accretion flow, wh…

astro-ph.HE2009★ 13 cited

Transition from radiatively inefficient to cooling dominated phase in two temperature accretion discs around black holes

Monika Sinha, S. R. Rajesh, Banibrata Mukhopadhyay

We investigate the transition of a radiatively inefficient phase of a viscous two temperature accreting flow to a cooling dominated phase and vice versa around black holes. Based o…

astro-ph.HE2009★ 55 cited

Two temperature accretion around rotating black holes: Description of general advective flow paradigm in presence of various cooling processes to explain low to high luminous sources

S. R. Rajesh, Banibrata Mukhopadhyay

We investigate the viscous two temperature accretion discs around rotating black holes. We describe the global solution of accretion flows with a sub-Keplerian angular momentum pro…

astro-ph.HE2009★ 10 cited

Two temperature viscous accretion flows around rotating black holes: Description of under-fed systems to ultra-luminous X-ray sources

S. R. Rajesh, Banibrata Mukhopadhyay

We discuss two temperature accretion disk flows around rotating black holes. As we know that to explain observed hard X-rays the choice of Keplerian angular momentum profile is not…