Estimation of mass outflow rates from dissipative accretion disc around rotating black holes

Abstract

We study the properties of the dissipative accretion flow around rotating black holes in presence of mass loss. We obtain the complete set of global inflow-outflow solutions in the steady state by solving the underlying conservation equations selfconsistently. We observe that global inflow-outflow solutions are not the isolated solution, instead such solutions are possible for wide range of inflow parameters. Accordingly, we identify the boundary of the parameter space for outflows, spanned by the angular momentum (λ in ) and the energy (E in ) at the inner sonic point (x in ), as function of the dissipation parameters and find that parameter space gradually shrinks with the increase of dissipation rates. Further, we examine the properties of the outflow rate Rṁ (defined as the ratio of outflow to inflow mass flux) and ascertain that dissipative processes play the decisive role in determining the outflow rates. We calculate the limits on the maximum outflow rate (R maẋ m ) in terms of viscosity parameter (α) as well as black hole spin (a k ) and obtain the limiting range as 3% R maẋ m 19%. Moreover, we calculate the viable range of α that admits the coupled inflow-outflow solutions and find that α 0.25 for Rṁ = 0. Finally, we discuss the observational implication of our formalism to infer the spin of the black holes. Towards this, considering the highest observed QPO frequency of black hole source GRO J1655-40 (∼ 450 Hz), we constrain the spin value of the source as a k 0.57.

Low angular momentum relativistic hot accretion flow around Kerr black holes with variable adiabatic index

“…We find that HFQPO at νQP O = 450 Hz can be explained in GRO J1655 − 40 provided it spins very rapidly with a k ≥ 0.85. This result is consistent with some of the earlier findings (Šrámková et al 2015;Aktar et al 2017).…”

Accretion-ejection in rotating black holes: a model for ‘outliers’ track of radio-X-ray correlation in X-ray binaries

“…We calculate A j by knowing the radius of two boundary surfaces, namely centrifugal barrier (CB) and funnel wall (FW) (Molteni et al 1996). The radius of CB is obtained using pressure maximum surface i.e., (dΦ eff i /dx) rCB = 0 and the radius of FW is defined as the pressure minimum surface, i.e., Φ eff i | rFW = 0 (Molteni et al 1996;Aktar et al 2015Aktar et al , 2017. We also consider the projection factor 1 + (dx j /dy j ) 2 for calculating jet area function Aktar et al 2017).…”

Point-wise Self-similar Solution for Spiral Shocks in Accretion Disk with Mass Outflow in Binary

“…This model has been used to explain the observational spectral states and quasiperiodic oscillations of compact objects (Chakrabarti & Titarchuk 1995;Molteni et al 1996). The mass ejection (jets or outflows from disks) due to the shock compression has also been extensively investigated with this model in recent years (Chattopadhyay & Das 2007;Das & Chattopadhyay 2008;Kumar & Chattopadhyay 2013;Aktar et al 2015Aktar et al , 2017Aktar et al , 2019.…”

“…This makes the territory of self-similarity shrink to pointwise regions, and the solution becomes point-wise valid. Meanwhile, we also consider the mass outflow due to the compression of spiral shock according to the similar analyses in Aktar et al (2015Aktar et al ( , 2017Aktar et al ( , 2019. Therefore, our model is an analytical accretion-ejection model for the interactive binary, which includes the effects characterized by the parameters of binary and might be used in further studies of binary evolution (Wang 2018).…”