Observational Constraints on Direct Electron Heating in the Hot Accretion Flows in Sgr A* and M87*

TL;DR

This paper uses recent Event Horizon Telescope data and theoretical models to constrain the fraction of energy directly heating electrons in hot accretion flows around black holes, focusing on Sgr A* and M87*.

Contribution

It provides observational constraints on the electron heating parameter  in hot accretion flows by combining EHT data with MAD model predictions.

Findings

Sgr A* requires   0.3, likely around 0.5

Constraints on  for M87* are inconclusive due to uncertainties

Method links observational data with theoretical accretion models

Abstract

An important parameter in the theory of hot accretion flows around black holes is $\delta$, which describes the fraction of ``viscously'' dissipated energy in the accretion flow that goes directly into heating electrons. For a given mass accretion rate, the radiative efficiency of a hot accretion flow is determined by $\delta$. Unfortunately, the value of $\delta$ is hard to determine from first principles. The recent Event Horizon Telescope Collaboration (EHTC) results on M87* and Sgr A* provide us with a different way of constraining $\delta$. By combining the mass accretion rates in M87* and Sgr A* estimated by the EHTC with the measured bolometric luminosities of the two sources, we derive good constraints on the radiative efficiencies of the respective accretion flows. In parallel, we use a theoretical model of hot magnetically arrested disks (MAD) to calculate the expected radiative efficiency as a function of $\delta$ (and accretion rate). By comparing the EHTC-derived radiative efficiencies with the theoretical results from MAD models, we find that Sgr A* requires $\delta \ga 0.3$. %with the most likely value being $\delta \sim 0.5$. A similar comparison in the case of M87* gives inconclusive results as there is still a large uncertainty in the accretion rate in this source.