Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8038
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dc.contributor.authorDas, Santabrata-
dc.contributor.authorNandi, Anuj-
dc.contributor.authorStalin, C. S-
dc.contributor.authorRakshit, Suvendu-
dc.contributor.authorDihingia, Indu Kalpa-
dc.contributor.authorSingh, Swapnil-
dc.contributor.authorAktar, Ramiz-
dc.contributor.authorMitra, Samik-
dc.date.accessioned2022-09-02T05:29:53Z-
dc.date.available2022-09-02T05:29:53Z-
dc.date.issued2022-08-
dc.identifier.citationMonthly Notice of Royal Astronomical Society, Vol. 514, No. 2, pp. 1940–1951en_US
dc.identifier.issn1365-2966-
dc.identifier.urihttp://hdl.handle.net/2248/8038-
dc.descriptionRestricted Accessen_US
dc.description.abstractWe study the relativistic, inviscid, advective accretion flow around the black holes and investigate a key feature of the accretion flow, namely the shock waves. We observe that the shock-induced accretion solutions are prevalent and such solutions are commonly obtained for a wide range of the flow parameters, such as energy (E) and angular momentum (λ), around the black holes of spin value 0 ≤ ak < 1. When the shock is dissipative in nature, a part of the accretion energy is released through the upper and lower surfaces of the disc at the location of the shock transition. We find that the maximum accretion energies that can be extracted at the dissipative shock (Emax) are ∼ 1 per cent and ∼ 4.4 per cent for Schwarzschild black holes (ak → 0) and Kerr black holes (ak → 1), respectively. Using Emax, we compute the loss of kinetic power (equivalently shock luminosity, Lshock) that is enabled to comply with the energy budget for generating jets/outflows from the jet base (i.e. post-shock flow). We compare Lshock with the observed core radio luminosity (LR) of black hole sources for a wide mass range spanning 10 orders of magnitude with sub-Eddington accretion rate and perceive that the present formalism seems to be potentially viable to account LR of 16 Galactic black hole X-ray binaries (BH-XRBs) and 2176 active galactic nuclei. We further aim to address the core radio luminosity of intermediate-mass black hole (IMBH) sources and indicate that the present model formalism perhaps adequate to explain core radio emission of IMBH sources in the sub-Eddington accretion limit.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of Royal Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.1093/mnras/stac1398-
dc.rights© Royal Astronomical Society-
dc.subjectAccretion, accretion discen_US
dc.subjectBlack hole physicsen_US
dc.subjectGalaxies: activeen_US
dc.subjectRadio continuum: generalen_US
dc.subjectX-rays: binariesen_US
dc.titleOn the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flowen_US
dc.typeArticleen_US
Appears in Collections:IIAP Publications



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