# Relativistic Turbulence with Strong Synchrotron and Synchrotron-Self-Compton Cooling

## TL;DR

This paper studies the thermodynamic and radiative properties of relativistically hot, turbulent plasmas in high-energy astrophysics, revealing a universal electron temperature and the spectral characteristics of synchrotron and inverse-Compton emissions.

## Contribution

It introduces a universal electron temperature in turbulent, radiatively cooled plasmas and analyzes the resulting broadband emission spectrum, including synchrotron and SSC components.

## Key findings

- Electron temperature scales as 1/√τ_T, independent of turbulence strength.
- Synchrotron and SSC emissions are comparable and well separated in energy.
- The number of IC peaks depends logarithmically on optical depth and magnetic field.

## Abstract

Many relativistic plasma environments in high-energy astrophysics, including pulsar wind nebulae, hot accretion flows onto black holes, relativistic jets in active galactic nuclei and gamma-ray bursts, and giant radio lobes, are naturally turbulent. The plasma in these environments is often so hot that synchrotron and inverse-Compton (IC) radiative cooling becomes important. In this paper we investigate the general thermodynamic and radiative properties (and hence the observational appearance) of an optically thin relativistically hot plasma stirred by driven magnetohydrodynamic (MHD) turbulence and cooled by radiation. We find that if the system reaches a statistical equilibrium where turbulent heating is balanced by radiative cooling, the effective electron temperature tends to attain a universal value $\theta = kT_e/m_e c^2 \sim 1/\sqrt{\tau_T}$, where $\tau_T=n_e\sigma_T L \ll 1$ is the system's Thomson optical depth, essentially independent of the strength of turbulent driving or magnetic field. This is because both MHD turbulent dissipation and synchrotron cooling are proportional to the magnetic energy density. We also find that synchrotron self-Compton (SSC) cooling and perhaps a few higher-order IC components are automatically comparable to synchrotron in this regime. The overall broadband radiation spectrum then consists of several distinct components (synchrotron, SSC, etc.), well separated in photon energy (by a factor $\sim \tau_T^{-1}$) and roughly equal in power. The number of IC peaks is checked by Klein-Nishina effects and depends logarithmically on $\tau_T$ and the magnetic field. We also examine the limitations due to synchrotron self-absorption, explore applications to Crab PWN and blazar jets, and discuss links to radiative magnetic reconnection.