Hydrodynamic Simulations of Large-scale AGN-driven Outflows

talk (id. 1258) presented at the European Astronomical Society (EAS) Annual Meeting, Symposium S6: Properties and impact of large-scale multiphase AGN outflows, Valencia, Spain, June 27, 2022
https://doi.org/10.6084/m9.figshare.26156374

1. Hydrodynamic Simulations of Hydrodynamic Simulations of
Large-scale AGN-driven OutflowsLarge-scale AGN-driven Outflows
Ash Danehkar
Eureka Scientific, Oakland, CA 94602, USA
[email protected]
Collaborators: Sally Oey, and Will Gray (Starburst-driven Outflows)
EAS Annual Meeting, Symposium S6: Properties and impact of large-scale multiphase AGN outflows. 27 June 2022
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Outline

Motivation for AGN Wind Simulations

Galactic Wind Theory
–Starburst Winds vs. AGN Outflows

Hydrodynamic Simulation Setup
–Radiative Cooling

Galactic Wind Modes
–Energy-driven Outflows vs. Momentum-driven Outflows

Photoionization Calculations
–Collisional Ionization (CIE) vs. Non-equilibrium Ionization (NEI)

Future Plans
–Radiative Transfer: Radiation-driven Outflows

Summary

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Motivation for AGN Wind Simulations
Tombesi + 2013

Warm Absorbers (WA)

Ultra-fast outflows (UFO)
Tombesi + 2013
NGC 4051
Pounds & King 2013
IRAS F11119+3257
Tombesi + 2015
Correlation between outflow kinematics and physical conditions

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Motivation for AGN Wind Simulations
Pounds & King 2015
Zubovas & King 2014
Multi-phase of AGN Winds

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Galactic Wind Theory
Different Wind Regions, as defined by Weaver+ 1977

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Galactic Wind Theory

Adiabatic Winds
–Chevalier & Clegg 1985

Radiative Cooling Winds

Radiative cooling in AGN-driven winds
(see e.g. Richings & Faucher-Giguere 2018)
Silich + 2004

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Starburst Winds versus AGN Outflows

Starburst-driven Outflows
–Slow Winds: 250-1000 km/s → triggering star formation
–Ambient Densities: 1-10,000 cm
-3
–Lower Ionizing Luminosities < 10
43
erg/s
→ stronger radiative cooling
–Metallicities: 0.1 – 0.5 Z☉
–Inconsiderable Gravitational Forces

AGN-driven Ouflows (see e.g. Richings & Faucher-Giguere 2018)
–Fast Winds: 1000-40,000 km/s → quenching star formation
–Ambient Densities: 1-10,000 cm
-3
–Higher lonizing Luminosities ~ 10
44
– 10
47
erg/s
→ weaker radiative cooling
–Metallicities: 0.1 – 3 Z☉
–Considerable Gravitational Forces near SMBH
–Relativistic Effects in Compact Ultra-fast Outflows
Starburst-driven Outflows (Romero+ 2018, Strickland+ 2003)
AGN-driven Outflows (Richings & Faucher-Giguere 20183)

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Hydrodynamic Simulation Setup

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Hydrodynamic Simulations: Ionizing Field
Ionizing SED ( )
Photo-Heating Rate:
Photoionization Rate:
PG 1211+143
Danehkar + 2018
log Lion = 45.2 erg/s
AGN Ionizing SED Starburst Ionizing SED
Starburst99
Danehkar + 2021
log Lion = 42.6 erg/s

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Hydrodynamics + Radiative Functions
Radiative Cooling Function (Λ) and Photo-Heating Function (Γ):
Atomic Chemistry and Cooling Package MAIHEM: Gray + 2019
 Cooling Efficiencies (Λ
i
): Gnat & Ferland 2012
 Heating Efficiencies (Γ
i
) made with photoionization cross-section:
Verner & Yakovlev 1995, & Verner, Ferland, et al. 1996

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Simulations of Galactic-scale Outflows
Danehkar, Oey, Gray, ApJ 921, 91 (2021)
Hydrodynamic Simulations of Galactic Winds

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Radiative Cooling in Galactic Winds

Adiabatic Bubble (AB)

Catastrophic Cooling Bubble (CB)

Catastrophic Cooling (CC)
Danehkar + 2021 (JPhCS 2028, 012013)

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Radiative Cooling in Galactic Winds

Adiabatic Bubble (AB), Adiabatic Pressure-Confined (AP)

Catastrophic Cooling (CC), Catastrophic Cooling Bubble (CB)
Temperature discrepancy factor (fT = Tw / Tadi)
Danehkar, Oey, Gray, 2021

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Galactic Wind Modes
(Danehkar, Oey, Gray, 2021, ApJ 921, 91)
Danehkar, Oey, Gray, 2021
Energy-driven Outflows:
Adiabatic Wind (AW),
Adiabatic Bubble (AB)
Pressure-Confined (AP)
Catastrophic Cooling (CC)
Catastrophic Cooling Bubble (CB)
Cooling, Pressure-Confined (CP)
No Expanding Wind (NW)
Momentum-driven Outflows:
Momentum-Conserving (MC)

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Galactic Wind Modes
Pounds & King 2015

Momentum-driven Outflows

Energy-driven Outflows

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Photoionization Calculations (steady state)
Photoionization
+ Collisional Ionization
Danehkar, Oey, Gray, 2021 (ApJ 921, 91)

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Photoionization Calculations (steady state)
Danehkar, Oey, Gray, 2021 (ApJ 921, 91)
PIE (Pure Photoionization), CIE+PIE=CPI (Photoionization + Collisional Ionization)

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Photoionization Calculations (time-dependent)

Collisional Ionization

Non-equilibrium Ionization
Danehkar, Oey, Gray, 2022 (ApJ 937, 68)

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Photoionization Calculations (time-dependent)
PIE (Pure Photoionization),CIE+PIE (Collisional Ionization+Photoionization),
NEI+PIE (Non-equilibrium Photoionization), Danehkar + 2022

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Future Plans: Radiative Transfer
Implementation of a Radiative Transfer (RT) unit
Improvement of radiative cooling and photo-heating
Stellar flux at a given distance (e.g. Klassen + 2014)
Inclusion of radiation pressure (radiation driving)
Simulations hosted on https://galacticwinds.github.io/superwinds/
Included in MAIHEM RT unit
Optical Depth:

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Summary

Galactic Starburst-driven and AGN-driven Winds
–Adiabatic Winds without Radiative Cooling (thermally driven winds; Chevalier & Clegg 85)
–Radiative Cooling Winds

Hydrodynamic Simulations of Galactic Winds
–MAIHEM Cooling Package: Radiative Cooling + Photo-Heating (Gray + 2019)
–Radiative Cooling in Starburst-driven Outflows (Danehkar, Oey, Gray, 2021, ApJ 921, 91)

Colliosinal Ionization vs. Non-equilibrium Ionization
–CIE (steady state), Danehkar et al. 2021, ApJ 921, 91 (radiatitve cooling in starburst-driven outflows)
–NEI (time-dependent) → C IV & O VI, Danehkar, et al. 2022, ApJ 937, 68 https://galacticwinds.github.io/superwinds/

Future Plans
–Hydrodynamic Simulations of AGN-driven Outflows (NGC 4051; Danehkar+ in preparation)
•Fast Winds 500-40,000 km/s higher than 250-1000 km/s in starburst-driven winds
•lonizing Luminosities ~ 10
44
– 10
47
erg/s higher than < 10
43
erg/s in starburst galaxies
–Implementation of a Radiative Transfer (RT) unit
•Improving photoionization calculations + including radiative pressures (radiation-driven winds)

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Thank you for your attention
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