Jets and spectral states with three-components of accretion flow around a black hole

TL;DR

This paper proposes a three-component accretion flow model around black holes to better explain spectral states, transitions, and jet behaviors observed in X-ray binaries, improving upon previous two-component models.

Contribution

It introduces a third hot accretion flow component that accounts for all spectral states and transitions, and offers a new scenario for jet formation and evolution.

Findings

The three-component model explains the entire hardness-intensity diagram.

A new jet kinetic power expression is derived from the model.

The model aligns with recent theoretical and observational insights.

Abstract

It is generally believed that high energy radiation (power-law components) can be mostly produced by a hot corona gas in the accreting black holes. There is a very popular hybrid disk radial coupling model that the inner part of cool Keplerian disk (or Shakura-Sunyaev disk) can produce advection-dominated accretion flow or corona-like structure, which can also generate outflows/jets. Here we argue that this simple coupling model cannot explain the whole hardness-intensity diagram of the spectral states and their transitions, and associated jets of a $X-$ray binary. Based on recent theoretical works on advective disk structures around a black hole, as well as many observational behaviors of a source, we conclude that there should be a third component of hot accretion flow with the radial coupling model, which can successfully explain all the spectral states and transitions. Interestingly, this model also provides a new scenario for the jet generation, launching, and evolution during the states with help of created barrier of the inner flow. We have also find out the jet kinetic power expression with our new jet generation scenario.