e-Talk presented at IAU Symposium 373 (IAUS373): Resolving the Rise and Fall of Star Formation in Galaxies, Busan, Korea, August 2022 Danehkar, Ashkbiz (2024). Conditions for Cool Superwinds in Massive Star-forming Regions. figshare. Presentation. https://doi.org/10.6084/m9.figshare.25029482

1. Conditions for Cool Superwinds
Conditions for Cool Superwinds
in Massive Star-forming Regions
in Massive Star-forming Regions
Ash Danehkar
Eureka Scientific, Inc., Oakland, CA 94602, USA
danehkar@eurekasci.com
Collaborators: Sally Oey, and Will Gray
IAU Symposium 373: Resolving the Rise and Fall of Star Formation in Galaxies. 9{11 August 2022
Image
Credit:
Hui
Yang,
Illinois
&
NASA/ESA

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Outline

Superwinds and Superbubbles
– Evidence for Cool Superwinds (ALMA and VLA observations)

Superwind Theory
– Radiative Cooling Functions

Hydrodynamic Simulations

Superwind Modes
– Typical H II Regions
– Ultra-compact H II Regions (UC-HII)

Photoionization Models
– Collisional Ionization (CIE) vs. Non-equilibrium Ionization (NEI)

Future Plans
– Radiative Transfer Implementation

Summary

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Superwinds and Superbubbles
Superwind and Superbubble in NGC 3079
(Credit: X-ray:NASA/CXC/UMich/J-T Li;Optical:NASA/STScI)

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Evidence for Cool Superwinds
Turner + 2017

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Superwinds and Superbubbles
Superwind and Superbubble (Strickland + 2002)

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Superwind Theory

Adiabatic Winds
– Chevalier & Clegg 1985

Radiative Cooling Winds
Silich + 2004

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

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Hydrodynamic Simulations

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

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

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Superwind Modes: Typical H II Regions

Adiabatic Bubble (AB)

Catastrophic Cooling Bubble (CB)

Catastrophic Cooling (CC)
Danehkar + 2021 (JPhCS 2028, 012013)

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Superwind Modes: Typical H II Regions

Adiabatic Bubble (AB), Adiabatic Pressure-Confined (AP)

Catastrophic Cooling (CC), Catastrophic Cooling Bubble (CB)
Temperature discrepancy factor (fT = Tw / Tadi)
Danehkar, Oey, Gray, 2021 (ApJ 921, 91)

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Superwind Modes: Typical H II Regions
(Danehkar, Oey, Gray, 2021, ApJ 921, 91)
Danehkar, Oey, Gray, 2021 (ApJ 921, 91)
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-Conserving (MC)

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Superwind Modes: Ultra-compact H II Regions
(Danehkar, in preparation)

Typical H II regions
– Cluster radius ⪎ 1 pc
– Ambient density ⪍ 103
cm{3

Compact H II regions
– Cluster radius ~ 0.1 pc
– Ambient density ~ 103
cm{3

Ultra-compact H II regions
– Cluster radius ~ 0.01 pc
– Ambient density ~ 104
cm{3

Hyper-compact H II regions
– Cluster radius ~ 0.001 pc
– Ambient density ~ 105
cm{3
Olivier + 2021
Compact &
Ultra-compact
H II Regions
Evolved
H II Regions

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Superwind Modes: Ultra-compact H II Regions
(Danehkar, in preparation)
Danehkar 2022, in preparation
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-Conserving (MC)

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

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Collisional Ionization + Photoionization
(steady state photoionization)
Danehkar, Oey, Gray, 2021 (ApJ 921, 91)
PI (Pure Photoionization), CPI (Collisional Ionization+Photoionization)

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Non-equilibrium Photoionization
(time-dependent photoionization; see my talk in IAUS370)

Collisional Ionization

Non-equilibrium Ionization
Danehkar, Oey, Gray, 2022 (submitted)

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Non-equilibrium Photoionization
(time-dependent photoionization; see my talk in IAUS370)
PIE (Pure Photoionization),CIE+PIE (Collisional Ionization+Photoionization),
NEI+PIE (Non-equilibrium Photoionization), Danehkar + 2022

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UV Diagnostics Diagrams
(see my poster in FM4)
NEI+PIE (Solid colors; Danehkar + 2022 submitted) ,
CIE+PIE (shaded colors; Danehkar + 2021, ApJ 921:91),

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

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Summary

Superwind Theory
– Adiabatic Model without radiative cooling (fluid solutions by Chevalier & Clegg 85)
– Radiative Cooling Model (semi-analytic solutions by Silich+ 2004)

Hydrodynamic Simulations
– MAIHEM Cooling & Chemistry Package: Radiative Cooling + Photo-Heating (Gray + 2019)
– Radiative Cooling in H II regions (Danehkar, Oey, Gray, 2021, ApJ 921, 91)

Colliosinal Ionization (CIE) vs. Non-equilibrium Ionization (NEI)
– CIE (steady state), Danehkar et al. 2021, ApJ 921, 91
– NEI (time-dependent) → C IV & O VI enhancements, Danehkar, et al. 2022 submitted

Future Plans
– Hydrodynamic Simulations of Ultra-compact H II regions (Danehkar+ in preparation)
• Ambient density ~ 103
{105
cm{3
higher than 1-103
cm{3
in typical H II regions
• Cluster radius ~ 0.02–0.2 pc smaller than ~ 1 pc in typical H II regions
– Implementation of a Radiative Transfer unit
• Improving photoionization calculations + radiative pressures

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Image
Credit:
Hui
Yang,
Illinois
&
NASA/ESA
Thank you for your attention