Relativistic Accretion

TL;DR

This paper reviews the properties of astrophysical black holes, focusing on different accretion modes, the role of mass loss and winds, and the influence of black hole spin on jet formation and emission characteristics.

Contribution

It provides a comprehensive overview of accretion processes onto black holes, highlighting the significance of mass loss, winds, and spin effects in astrophysical phenomena.

Findings

Accretion rates vary from below to above the Eddington limit.

Mass loss through winds is crucial when radiation cannot carry away all infalling material.

Black hole spin influences jet formation and emission types.

Abstract

A brief summary of the properties of astrophysical black holes is presented. Various modes of accretion are distinguished, corresponding to accretion at rates from well below to well above the Eddington rate. The importance of mass loss is emphasized when the accreting gas cannot radiate and it is asserted that a strong wind is likely to be necessary to carry off mass, angular momentum and energy from the accreting gas. The possible importance of the black hole spin in the formation of jets and in dictating the relative importance of non-thermal emission over thermal radiation is discussed.