Hydrodynamic Simulations of Starburst-driven Superwinds

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Talk presented at Challenges and Innovations in Computational Astrophysics - III (ChaICA-III; Virtual), 21 June 2021, https://doi.org/10.6084/m9.figshare.14820438

Science

Ashkbiz Danehkar
Department of Astronomy, University of Michigan
danehkar@umich.edu
In Collaborations with: Sally Oey, and Will Gray
Challenges and Innovations in Computational Astrophysics - III, June 21, 2021
Hydrodynamic Simulations of
Starburst-driven Superwinds
Superbubble
in
NGC
3079
(Credit:
X-ray:NASA/CXC/UMich/J-T
Li;Optical:NASA/STScI)

21/06/2021 ChaICA-III
2
Outline

Superwinds & Superbubbles
– Superwind Theory: Adiabatic Solution
– Superbubble & Superwind Theory

Catastrophic Cooling
– Superwind Theory: Radiative Solution

Hydrodynamic Simulations

Photoionization Modeling
– Diagnostic Diagrams

Hydrodynamic and Photoionization Results

Summary & Future Directions

21/06/2021 ChaICA-III
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Superwinds & Superbubbles
Superwind and Superbubble in NGC 3079
(Credit: X-ray:NASA/CXC/UMich/J-T Li;Optical:NASA/STScI)

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Superwinds & Superbubbles
Superwind and Superbubble (Romero+ 2018, Strickland+ 2003)

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Superwind Theory: Adiabatic
Adiabatic Solutions
– Adiabatic Wind (γ=5/3)
– Chevalier & Clegg 1985
Chevalier & Clegg 1985

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Superwind Theory: Adiabatic
Adiabatic Bubble Solutions
– Castor+ 1975
– Weaver+ 1977
Weaver+ 1977
Weaver+ 1977

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Superwind Theory
Gray, Oey, Silich + 2019

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Catastrophic Cooling
NGC 2366
Green Pea analog!
[O II], [O III] and Continuum (Oey+ 2017)
Mrk 71
Oey + 2017

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Catastrophic Cooling
Super Star Cluster NGC 5253 (Turner et al. 2017)

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Superwind Theory: Radiative

Radiative Solutions
– Silich et al. 2004
– With Radiative Cooling
Silich + 2004

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Superwind Theory: Radiative
Radiative Cooling
Silich + 2004
Silich + 2004

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Hydrodynamic Simulations
Danehkar, Oey, Gray, 2021

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Hydrodynamic Simulations
Danehkar, Oey, Gray, 2021

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Hydrodynamic Simulations
MAIHEM Package built on FLASH code (Will + 2015)
Temperature Density
Danehkar, Oey, Gray, 2021

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Hydrodynamic Simulations
Radiative Cooling

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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Danehkar, Oey, Gray, 2021
Hydrodynamic Simulations

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Photoionization Modeling
Danehkar, Oey, Gray, 2021
Photoionization
+ Hydro Collisional Ionization

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Photoionization Modeling
Danehkar, Oey, Gray, 2021
PI (Pure Photoionization), CPI (Photoionization + Hydro Collisional Ionization)

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Diagnostic Diagrams
Emission Lines of Superwinds
Danehkar, Oey, Gray, 2021
Gray, Oey, Silich + 2019

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BPT Diagnostic Diagrams
Danehkar, Oey, Gray, 2021
Optical Emission Lines (radiation-bounded)

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UV Diagnostic Diagrams
Danehkar, Oey, Gray, 2021
UV Emission Lines (radiation-bounded)

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UV Diagnostic Diagrams
UV Emission Lines (radiation-bounded)
Danehkar, Oey, Gray, 2021

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Model Results
Danehkar, Oey, Gray, 2021

Hydrodynamics & Photoionization Results
https://superwinds.astro.lsa.umich.edu/

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Summary

Superwind Theory
– Adiabatic Solution (Chevalier & Clegg 85)
– Radiative Solution (Silich + 2004)

Hydrodynamic Simulations
– Catastrophic Cooling (Gray, Oey, Silich, 2019)
– Radiative Cooling increases with (Danehkar, Oey, Gray, 2021):
• higher mass-loading, lower outflow velocity, higher metallicity

Photoionization Modeling (Photoionization + Hydro Collisional Ionization)
– Emission lines predicted for adiabatic and cooling outflows
– BPT & UV Diagnotic Diagrams

Future Directions
– Non-equilibrium Photoionization (Photoionization + NEI; next work)
– 2-D simulations: Instability-induced gas clumping

21/06/2021 ChaICA-III
25
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