Radiatively driven rotating pair-plasma jets from two-component accretion flows

Abstract

Centrifugal pressure of matter spiralling on to black holes has long been known to produce standing or oscillating shocks. The post‐shock disc puffs up in the form of a torus, which intercepts soft photons from the outer Keplerian disc and inverse‐Comptonizes them to produce hard photons. The post‐shock region also produces jets. We study the interaction of both hard photons and soft photons, with rotating electron–positron jets. We show that hard photons from the post‐shock torus are instrumental in acceleration of jets, while soft photons from the Keplerian disc is a better collimating agent. We also show that if the jets are launched closer to the black hole, relativistic and collimated jets are produced; if they are launched at larger distances both collimation and acceleration are less. We also show that if the shock location is at relatively larger distances from the black hole, collimation is better.

Radiatively driven relativistic jets with variable adiabatic index equation of state

“…The funnel like surface of the PSD is the region from where the jet is supposed to originate, the shape itself will arrest the lateral spread of the outflowing matter. Moreover, such shape causes the r component of radiative flux directed towards the axis (Chattopadhyay 2005) which would also reduce the lateral spreading even with high jet-base temperature. However, one can justify our assumption only if we solve the jet equations since we need some estimate of the pressure.…”

“…Beyond few tens of r g the general relativistic effect may be ignored, but special relativistic effects cannot be. But close to the horizon, if only special relativistic effects are considered then the I ps gets unnecessarily jacked up (Chattopadhyay 2005). In order to address this, we estimate the fraction of radiation that will not be absorbed by the black hole and escape.…”

“…Infact it was shown that, contrary to expectation, pairplasma is thermally the least relativistic, and to make a flow more relativistic one needs baryons in addition to electrons or positrons, and the fluid with proton number density around 27% of that of electrons is thermally the most relativistic. Now radiation force is imparted mainly onto the electrons and positrons which should make the lighter jet to move faster due to inertia, as is shown for cold jets (Chattopadhyay et al 2004;Chattopadhyay 2005). On the contrary, the thermodynamics of the jet will make the fluid with 27% proton content to be more relativistic.…”

“…If however, one considers the gas pressure (p) to be negligible compared to the radiation pressure (P ij ), then even in the fully relativistic limit, the net radiative term is only proportional to the number density of the flow. Therefore, the physics of interaction of disc radiation with a fluid jet in the relativistic regime is qualitatively and quantitatively different than that between radiation and jet in the non-relativistic domain (Chattopadhyay & Chakrabarti 2002;, or relativistic jets in the domain where P ij ≫ pδ ij (Chattopadhyay et al 2004;Chattopadhyay 2005). In this paper, we would like to investigate this phenomenon in details.…”

“…Interaction of radiations with the outflowing jet from PSD was studied by Chattopadhyay & Chakrabarti (2000a,b, 2002. The investigation of outflowing jet (Chattopadhyay et al 2004;Chattopadhyay 2005) was further elaborated for the radiation field of the Chakrabarti-Titarchuk type hybrid disc (Chakrabarti & Titarchuk 1995). Generally most of the papers which investigate the interaction of jet with disc photons do not consider the issue of the launch mechanism of jets in terms of the accretion properties.…”