A Model for Spectral States and Their Transition in Cyg X-1

TL;DR

This paper proposes a new accretion model for Cyg X-1, explaining its spectral states and transitions through the dynamics of a small, co-spatial two-component inner disk influenced by wind-fed accretion.

Contribution

It introduces a novel accretion framework for wind-fed black hole binaries, emphasizing the role of a small, variable inner disk in spectral state changes.

Findings

Inner disk expansion and recession drive state transitions.

Wind-fed systems lack large outbursts due to absence of extensive outer disks.

Presence of a weak cool disk explains relativistically broadened Fe K lines.

Abstract

A new accretion picture based on a small disk surrounding a black hole is developed for the wind-fed source Cyg X-1. The hard and soft spectral states of Cyg X-1 are interpreted in terms of co-spatial two component flows for the innermost region of an accretion disk. The state transitions result from the outward expansion and inward recession of this inner disk for the hard to soft and soft to hard transition respectively. The theoretical framework for state transitions in black hole X-ray binaries with high mass companions involving a change in the inner disk size, thus, differs from systems with low mass companions involving the change in the outer disk size. This fundamental difference stems from the fact that matter captured and supplied to the black hole in wind-fed systems has low specific angular momentum and is hot essentially heated in the bow and spiral shocks, whereas it has high specific angular momentum and is cool in Roche lobe overflow systems. The existence of a weak cool disk around the ISCO region in the hard state allows for the presence of a relativistically broadened Fe K line. The small disk fed by gas condensation forms without an extensive outer disk, precluding thermal instabilities and large outbursts, resulting in the lack of large amplitude outbursts and hysteresis effects in the light curve of high mass black hole X-ray binaries. Their relatively persistent X-ray emission is attributed to their wind-fed nature.