# Winds and feedback from supermassive black holes accreting at low rates: Hydrodynamical treatment

## TL;DR

This study uses hydrodynamical simulations to investigate winds from low-accretion-rate supermassive black holes, revealing powerful, thermally-driven outflows that align with observed properties in low-luminosity active galactic nuclei.

## Contribution

It provides the first detailed hydrodynamical modeling of winds in low-luminosity AGNs, exploring diverse initial conditions and long-term evolution.

## Key findings

- Winds reach velocities up to 0.01c.
- Winds carry 0.1-1% of inflow energy.
- Outflows can heat ambient gas and suppress star formation.

## Abstract

Outflows produced by a supermassive black hole (SMBH) can have important feedback effects in its host galaxy. An unresolved question is the nature and properties of winds from SMBHs accreting at low rates in low-luminosity active galactic nuclei (LLAGNs). We performed two-dimensional numerical, hydrodynamical simulations of radiatively inefficient accretion flows onto non spinning black holes. We explored a diversity of initial conditions in terms of rotation curves and viscous shear stress prescriptions, and evolved our models for very long durations of up to $8 \times 10^5 GM/c^3$. Our models resulted in powerful subrelativistic, thermally-driven winds originated from the corona of the accretion flow at distances $10-100 GM/c^2$ from the SMBH. The winds reached velocities of up to $0.01 c$ with kinetic powers corresponding to 0.1-1% of the rest-mass energy associated with inflowing gas at large distances, in good agreement with models of the "radio mode" of AGN feedback. The properties of our simulated outflows are in broad agreement with observations of winds in quiescent galaxies that host LLAGNs, which are capable of heating ambient gas and suppressing star formation.