A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

Lee, Jason P.; Becker, Peter A.

doi:10.1093/mnras/stz3287

Cited by 7 publications

(2 citation statements)

References 70 publications

(93 reference statements)

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“…Hence, the outflows/jets are expected to carry a fraction of the available energy (equivalently core emission) at the PSC, which in general considered as the base of the outflows/jets (Chakrabarti 1999;Chattopadhyay & Das 2007;Das & Chattopadhyay 2008;Singh & Chakrabarti 2011;Sarkar & Das 2016). Becker and his collaborators showed that the energy extracted from the accretion flow via isothermal shock can be utilized to power the relativistic particles emanating from the disc (Le & Becker 2005;Becker, Das, & Le 2008;Das, Becker, & Le 2009;Lee & Becker 2020). Moreover, magnetohydrodynamical study of the accretion flows around the black holes also accounts for possible role of shock as the source of high energy radiation (Nishikawa et al 2005;Takahashi et al 2006;Hardee, Mizuno, & Nishikawa 2007;Takahashi & Takahashi 2010).…”

Section: Introductionmentioning

confidence: 99%

On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow

Das,

Nandi,

Stalin

et al. 2022

Preprint

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We 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 ≤ a k < 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 (∆E max ) are ∼ 1% and ∼ 4.4% for Schwarzschild black holes (a k → 0) and Kerr black holes (a k → 1), respectively. Using ∆E max , we compute the loss of kinetic power (equivalently shock luminosity, L shock ) that is enabled to comply with the energy budget for generating jets/outflows from the jet base (i.e., post-shock flow). We compare L shock with the observed core radio luminosity (L R ) 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 L R of 16 Galactic black hole X-ray binaries (BH-XRBs) and 2176 active galactic nuclei (AGNs). 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.

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Section: Introductionmentioning

confidence: 99%

On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow

Das,

Nandi,

Stalin

et al. 2022

Preprint

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“…The sub-Keplerian flow can give many types of the advective solutions depend on the variation of the AM distributions in the flow. Two types of the advective solutions for the hot accretion flow are very popular in the literature, one, the shocked accretion flow (Fukue 1987;Chakrabarti 1989;Molteni et al 1996;Lanzafame et al 1998;Mukhopadhyay 2003;Becker et al 2008;Das & Czerny 2012;Giri & Chakrabarti 2013;Das et al 2014;Lee et al 2016;Kumar & Chattopadhyay 2017;Dihingia et al 2019;Lee & Becker 2020;Garain et al 2020) and the other, a special kind of the smooth solution known as the Advection-Dominated Accretion Flow (ADAF) solution (Ichimaru 1977;Narayan & Yi 1994;Honma 1996; Narayan et al 1997;Lu et al 1999;Kato et al 2008;Narayan et al 2012;Yuan & Narayan 2014;Kumar & Gu 2018. Interestingly, both the advective disk solutions/models can be generated from the same set of the fluid differential equations and assumptions, but both (shock and ADAF) solutions have basic difference of AM distribution.…”

Section: Introductionmentioning

confidence: 99%

Review the possible advective disk structures around a black hole with two-type gas inflows

Kumar,

Yuan

2021

Preprint

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We studied the general advective accretion solutions around the Kerr black hole (BH) with investigating two types of inflow gases at the outer accretion boundary (AB). We classified these two types of gases as a cold-mode and a hot-mode inflow gas at the outer AB on the basis of their temperatures and solutions. We found that the hot-mode gas is more efficient for angular momentum transportation around the outer AB than the cold-mode gas. The hot-mode gas can give global multiple (popular as shock solution Chakrabarti 1989) or single sonic point solutions and the cold-mode can give smooth global solution (popular as ADAF Narayan & Yi 1994) or two sonic point solutions. These solutions also represented on a plane of energy and angular momentum (B ob − L 0 ) parameter space. Theoretically for the first time, we explored the relation between the nature of accretion solutions with the nature of initial accreting gas at the AB with detail computational and possible physical analysis. We also found that the surface density of the flow is highly affected with changing of the temperature at the AB, which can alter the radiative emissivities of the flow. The flow variables of various advective solutions also compared. On the basis of those results, we plotted some inner disk structures around the BHs. Doing so, we conjectured about the persistent/transient nature of spectral states, soft-excess and time scales of variabilities around the black hole X− ray binaries (BXBs) and active galactic nuclei (AGNs).

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Development of a platform for experimental and computational studies of magnetic and radiative effects on astrophysically relevant jets at OMEGA

Rigon,

Stoeckl,

Johnson

et al. 2024

Physics of Plasmas

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Accurate modeling of astrophysical jets is critical for understanding accretion systems and their impact on the interstellar medium. While astronomical observations can validate models, they have limitations. Controlled laboratory experiments offer a complementary approach for qualitative and quantitative demonstration. Laser experiments offer a complementary approach. This article introduces a new platform on the OMEGA laser facility for high-velocity (1500 kms−1), high-aspect-ratio (∼36) jet creation with strong cylindrical symmetry. This platform's capabilities bridge observational gaps, enabling controlled initial conditions and direct measurements of plasma characteristics, crucial for refining astrophysical jet dynamics and improving the models accuracy.

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A two-fluid model for black-hole accretion flows: Particle acceleration, outflows, and TeV emission

Cited by 7 publications

References 70 publications

On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow

On the origin of core radio emissions from black hole sources in the realm of relativistic shocked accretion flow

Review the possible advective disk structures around a black hole with two-type gas inflows

Development of a platform for experimental and computational studies of magnetic and radiative effects on astrophysically relevant jets at OMEGA

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