On the role of the magnetic field on jet emission in X-ray binaries

TL;DR

This paper proposes that variations in the magnetic field strength of jets in X-ray binaries explain the scatter in radio/X-ray correlations, challenging the assumption that radio flux directly measures jet power.

Contribution

It introduces a model where the magnetic field strength variability accounts for differences in jet emission, providing a new perspective on radio/X-ray correlations in black hole binaries.

Findings

Jet magnetic field strength influences the spectral energy distribution.

Stronger magnetic fields lead to lower radio emission due to radiative losses.

Variable magnetic fields can explain spectral state transitions.

Abstract

Radio and X-ray fluxes of accreting black holes in their hard state are known to correlate over several orders of magnitude. This correlation however shows a large scatter: black hole candidates with very similar X-ray luminosity, spectral energy distribution and variability, show rather different radio luminosities. This challenges theoretical models that aim at describing both the radio and the X-ray fluxes in terms of radiative emission from a relativistic jet. More generally, it opens important questions on how similar accretion flows can produce substantially different outflows. Here we present a possible explanation for this phenomenon, based on the strong dependency of the jet spectral energy distribution on the magnetic field strength, and on the idea that the strength of the jet magnetic field varies from source to source. Because of the effect of radiative losses, sources with stronger jet magnetic field values would have lower radio emission. We discuss the implications of this scenario, the main one being that the radio flux does not necessarily provide a direct measure of the jet power. We further discuss how a variable jet magnetic field, reaching a critical value, can qualitatively explain the observed spectral transition out of the hard state.