Non-equilibrium Photoionization and Hydrodynamic Simulations of Starburst-driven Outflows

Talk presented at 4th Workshop on Numerical Modeling in MHD and Plasma Physics (MHD-PP; Virtual), 13 October 2021

Transcript

1. Non-equilibrium Photoionization
   Non-equilibrium Photoionization
   and Hydrodynamic Simulations
   and Hydrodynamic Simulations
   of Starburst-driven Outflows
   of Starburst-driven Outflows
   Starburst-driven Outflow (Romero+ 2018, Strickland+ 2003)
   Ashkbiz Danehkar
   Department of Astronomy, University of Michigan
   danehkar@umich.edu
   In Collaborations with: Sally Oey, and Will Gray
   Fourth Virtual Workshop on Numerical Modeling in MHD and Plasma Physics (MHD-PP), October 13, 2021
   

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   Starburst-driven Outflows
   Starburst-driven Outflows and Bubbles in NGC 3079
   (Credit: X-ray:NASA/CXC/UMich/J-T Li;Optical:NASA/STScI)
   

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   Starburst-driven Outflows
   Starburst-driven Outflows (Romero+ 2018, Strickland+ 2003)
   

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   Outline
    Background: Starburst-driven Outflows
   – Adiabatic Wind and Bubble Formation Solutions
   – Radiative Semi-analytic Wind Solutions
    Hydrodynamic Setup: NEI Radiative Cooling in FLASH
   – Radiative Cooling Rates + Photo-Heating Rates
    Emissivity Calculations: CLOUDY Photoionization Modeling
   – CIE+PIE Implementation
   – NEI+PIE Implementation
    Applications: Star-forming galaxies
   – Optical BPT and UV Diagnostic Diagrams
    Future Plans: Detailed Radiative Transfer, 2D Simulations
   

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

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   Strong Cooling & Suppressed Winds
   Super Star Cluster NGC 5253 (Turner et al. 2017)
   

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

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   Wind Formation: Adiabatic Theory
   Different Wind Regions, as defined by Weaver+ 1977
   

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   Wind Formation: Radiative Solution
   
   Radiative Semi-analytic Solutions
   – Silich + 2004
   – With Radiative Cooling
   Silich + 2004
   

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    Wind Formation: Radiative Solution
    Radiative Cooling
    Silich + 2004
    Silich + 2004
    

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    Hydrodynamic Simulations
    Danehkar, Oey, Gray, 2021
    

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    Hydrodynamic Simulations
     Solve using a hybrid Riemann solver (Roe+HLLE) in FLASH
    – Unsplit Hydrodynamic Solver
    – 2nd-order MUSCL-Hancock Scheme
     Coupled with the Non-equilibrium Atomic Chemistry and Cooling
    Package MAIHEM (Gray + 2019)
    – Radiative Cooling Function (Λ)
    – Photo-Heating Function (Γ)
    

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    Hydrodynamic Simulations
     Boundary Conditions:
     Initial Conditions:
     Radiative Cooling Function (Λ) and Photo-Heating Function (Γ):
    Included in the Atomic Chemistry and Cooling Package MAIHEM (Gray + 2019)
    

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    Hydrodynamic Simulations
    Cooling Function (Λ) and Photo-Heating Function (Γ):
     Included in the Atomic Chemistry and Cooling Package MAIHEM (Gray + 2019):
    
    Cooling Efficiencies from (Λ
    i
    ) calculated using ion-by-ion efficiencies
    from Gnat & Ferland 2012.
    
    Heating Efficiencies from (Γ
    i
    ) calculated using photoionization cross sections
    from Verner & Yakovlev 1995, and Verner, Ferland, et al. 1996.
    

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    Hydrodynamic Simulations
    Model Grids: https://superwinds.astro.lsa.umich.edu/
    Temperature Density
    Danehkar, Oey, Gray, 2021
    

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    Hydrodynamic Simulations
    
    Adiabatic Bubble (AB)
    
    Catastrophic Cooling Bubble (CB)
    
    Catastrophic Cooling (CC)
    Danehkar, Oey, Gray, 2021
    

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    Hydrodynamic Simulations
    
    Adiabatic Bubble (AB), Catastrophic Cooling Bubble (CB)
    
    Catastrophic Cooling (CC), momentum-conserving (MC)
    Temperature discrepancy factor (fT = Tw / Tadi)
    Danehkar, Oey, Gray, 2021
    

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    Hydrodynamic Simulations
    
    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
    (Danehkar, Oey, Gray, 2021)
    

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    Photoionization Modeling (CIE+PIE=CPI)
    Danehkar, Oey, Gray, 2021
    Photoionization
    + Collisional Ionization
    

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    Photoionization Modeling (CIE+PIE=CPI)
    Danehkar, Oey, Gray, 2021
    PIE (Pure Photoionization), CIE+PIE=CPI (Photoionization + Collisional Ionization)
    

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    Photoionization Modeling (NEI+PIE=NPI)
    Danehkar, Oey, Gray, 2021
    Photoionization
    + Non-equilibrium Ionization
    

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    Photoionization Modeling (NEI+PIE=NPI)
    PIE (Pure Photoionization), CIE+PIE=CPI (Photoionization + Collisional Ionization),
    NEI+PIE=NPI (Photoionization + Non-equilibrium Ionization), Danehkar, Oey, Gray, 2021
    

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    Optical & UV Diagnostic Diagrams
    Emission Lines of Superwinds
    Danehkar, Oey, Gray, 2021
    

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    Optical BPT 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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    Future Plans: Extension to 2D
     Allow to Study Different Instabilities
     Rayleigh-Taylor instability, Richtmyer-Meshkov instability, Kelvin-Helmholtz instability
     Formation of Instability-induced Dense Clumps
    Lancaster, Ostriker, et al. 2021
    

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    Future Plans: Extension to 2D
     Allow to Study Different Instabilities
     Rayleigh-Taylor instability, Richtmyer-Meshkov instability, Kelvin-Helmholtz instability
     Formation of Instability-induced Dense Clumps
    Lancaster, Ostriker, et al. 2021
    

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    Future Plans: RT Implementation
     Implementation of detailed Radiative Transfer (RT) calculations
     Improvement of radiative cooling and photo-heating processes
     Stellar flux at a given distance (e.g. Klassen + 2014):
     Inclusion of radiation pressure:
    Included in MAIHEM Need RT calculations
    

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    Concluding Points
     Starburst-driven Outflows
    – Adiabatic Solution (Chevalier & Clegg 85)
    – Radiative Solution (Silich + 2004)
     Non-equilibrium Cooling Hydrodynamic Simulations
    – MAIHEM Cooling Package (Gray + 2019): Radiative Cooling + Photo-Heating
    – Parameter Space Investigation (Danehkar, Oey, Gray, 2021, ApJ, arXiv:2106.10854)
     Photoionizaion Modeling
    – CIE+PIE (Danehkar et al. ApJ, 2021; arXiv:2106.10854)
    – NEI+PIE (Danehkar, et al. in preparation)
     Future Plans
    – Detailed Radiative Transfer Implementation: Improved Radiative Solutions
    – 2-D Simulation: Instability-induced Clumps
    

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    Thank you for your attention
    Starburst-driven Outflow (Romero+ 2018, Strickland+ 2003)
    

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