Observed jet power and radiative efficiency of black hole candidates in Kerr + PFDM model

TL;DR

This study investigates black hole jet power and radiative efficiency within the Kerr+PFDM spacetime model, demonstrating its ability to explain observations in X-ray binaries and constraining spacetime parameters, while highlighting limitations similar to Kerr spacetime.

Contribution

It introduces the Kerr+PFDM model to explain black hole emissions and provides combined analysis constraints on spacetime parameters based on observational data.

Findings

Kerr+PFDM can explain radiative efficiency via continuum fitting method.

Kerr+PFDM can replicate observed jet power using Blandford-Znajeck mechanism.

The model cannot simultaneously account for jet power and radiative efficiency of GRS 1915+105.

Abstract

In this research, we explore the electromagnetic energy emitted by astrophysical black holes within the Kerr+PFDM spacetime, a model encompassing rotating black holes surrounded by dark matter. Our investigation focuses on black holes within X-ray binary systems, namely GRS 1915+105, GRO J1655-40, XTE J1550-564, A0620-00, H1743-322, and GRS 1124-683. Our findings indicate that the Kerr+PFDM spacetime can account for the radiative efficiency of these sources as determined through the continuum fitting method (CFM). Additionally, employing the Blandford-Znajeck mechanism, we demonstrate the ability to replicate the observed jet power. By combining the outcomes of both analyses for the selected objects, we establish more rigorous constraints on the spacetime parameters. Notably, our results reveal that similar to the Kerr spacetime, the Kerr+PFDM spacetime cannot simultaneously account for the observed jet power and radiative efficiency of GRS 1915+105.