BLACK HOLE SPIN AND THE RADIO LOUD/QUIET DICHOTOMY OF ACTIVE GALACTIC NUCLEI

TLDR

Radio loud active galactic nuclei (AGNs) are on average 1000 times brighter in the radio band compared to radio quiet AGNs. The study investigates whether the radio loud/quiet dichotomy of AGNs can be explained by differences in black hole spin and discusses other physical effects that might contribute. The authors use general relativistic magnetohydrodynamic simulations to build steady‑state axisymmetric models across a broad spin range and jet geometries, assuming constant magnetic flux through the horizon, and derive an analytic solution with a fitting formula that reproduces the steeper jet power scaling. For thin disks the jet power scales roughly as ΩH², limiting spin‑induced power variations to a few tens, whereas for thick disks the scaling steepens to ΩH⁴ or ΩH⁶, allowing up to 1000‑fold variations in power across realistic spin distributions, as confirmed by an analytic solution and fitting formula.

Abstract

Radio loud active galactic nuclei (AGNs) are on average 1000 times brighter in the radio band compared to radio quiet AGNs. We investigate whether this radio loud/quiet dichotomy can be due to differences in the spin of the central black holes (BHs) that power the radio-emitting jets. Using general relativistic magnetohydrodynamic simulations, we construct steady state axisymmetric numerical models for a wide range of BH spins (dimensionless spin parameter 0.1 ⩽ a ⩽ 0.9999) and a variety of jet geometries. We assume that the total magnetic flux through the BH horizon at radius rH(a) is held constant. If the BH is surrounded by a thin accretion disk, we find that the total BH power output depends approximately quadratically on the angular frequency of the hole, P ∝ Ω2H ∝ (a/rH)2. We conclude that, in this scenario, differences in the BH spin can produce power variations of only a few tens at most. However, if the disk is thick such that the jet subtends a narrow solid angle around the polar axis, then the power dependence becomes much steeper, P ∝ Ω4H or even ∝Ω6H. Power variations of 1000 are then possible for realistic BH spin distributions. We derive an analytic solution that accurately reproduces the steeper scaling of jet power with ΩH and we provide a numerical fitting formula that reproduces all our simulation results. We discuss other physical effects that might contribute to the observed radio loud/quiet dichotomy of AGNs.