Simulations of Superwind Suppression in Super Star Clusters

Talk at Galaxy Group Meeting, University of Michigan, MI, USA, November 2019

Transcript

1. Ashkbiz Danehkar
   Department of Astronomy, University of Michigan
   danehkar@umich.edu
   In Collaborations with: Sally Oey, Will Gray, Sergiy Silich, and et al.
   Galaxy Group Meeting, University of Michigan, November 25th, 2019
   Simulations of
   Superwind Suppression
   in Super Star Clusters
   Horsehead Nebula
   Horsehead Nebula
   

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   Outline
   
   Superwinds and Super bubbles
    Super bubble Observation
    Super bubble Thoery
    Superwind Theory
   
   Superwinds Suppression Cooling Conditions for Star Formation
   → →
   
   Starburst and Radiation Leakage
   
   Hydrodynamic Simulation of Superwinds
   
   Photoionization Modeling of Superwinds
   
   Diagnostic Diagrams
   

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   Superwinds and Super Bubbles
   Schematic View of Superwind and Super Bubble (Romero+ 2018, Strickland+ 2003)
   

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   Superwinds and Super Bubbles
   Rosette Nebula
   (Credit: Schmitz/PhotographingSpace)
   

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   Superwinds and Super Bubbles
   Rosette Nebula (Bruhweiler + 2010): 6 OB stars of NGC 2244
   

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   Superwinds and Super Bubbles
   
   O-type Stars:
   – Temperature: 30,000 – 50,000 K
   – Lumisoity: 104 - 106 L⊙
   – Mass: 20 – 60 M⊙
   
   Early B-type Stars:
   – Temperature: 15,000 – 25,000 K
   – Lumisoity: 103 - 104 L⊙
   – Mass: 10 – 20 M⊙
   

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   Superwinds and Super Bubbles
   
   O-type Stars:
   – Temperature: 30,000 – 50,000 K
   – Lumisoity: 104 - 106 L⊙
   – Mass: 20 – 60 M⊙
   
   Early B-type Stars:
   – Temperature: 15,000 – 25,000 K
   – Lumisoity: 103 - 104 L⊙
   – Mass: 10 – 20 M⊙
   

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   Infrared X-ray
   Optical Composite Colors
   NGC 1929, LMC N44 Superbubble
   Cool
   Hot
   Cool
   Hot
   Cool
   Hot
   Cool
   Hot
   

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   Superwinds and Super Bubbles
   Schematic View of Superwind and Super Bubble (Strickland+2003)
   

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    Superwinds and Super Bubbles
    Heckman et al. 1993
    
    Starburst SN explosions thermal-driven winds shock heat superwinds
    → → → →
    
    Snowplow Phase Blowout phase
    →
    

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    Superwind Theory
    Superbubble Theory
    ●
    Castor+ 1975
    ●
    Weaver+ 1977
    Weaver+ 1977
    Weaver+ 1977
    

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    Superwind Theory
    Supewind Theory: Starburst M82
    ●
    Adiabatic Wind (γ=5/3)
    ●
    Chevalier & Clegg 1985
    ●
    Without radiative cooling
    Chevalier & Clegg 1985
    

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    Superwind Theory
    Supewind Theory
    ●
    Silich et al. 2004
    ●
    With radiative cooling
    Silich + 2004
    

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    Hydrodynamic Simulation of Superwinds
    ●
    Radiative Cooling
    Silich + 2004
    Silich + 2004
    

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    Hydrodynamic Simulation of Superwinds
    ●
    MAIHEM Model in FLASH: Gray+2017
    ●
    Based on Turbulence Models with FLASH: Gray+2015, 2016, 2017
    Gray, Oey, Silich + 2019
    

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    Hydrodynamic Simulation of Superwinds
    ●
    MAIHEM Simulations in FLASH
    Temperature Density
    Danehkar, Oey, Gray +
    

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    Superwind Suppression
    E
    A1
    A
    C
    B1-1
    B
    F L
    Smith+ 2006
    500 pc
    

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

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    Superwind Suppression
    Super Star Cluster NGC 5253 (Turner et
    al. 2017)
    

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    Conditions for Star Formation
    
    Cold Gas (10-1000 K) → Molecular Gas (H
    2
    and CO)
    
    Cold Gas (10-1000 K) → Dense Clump
    http://abyss.uoregon.edu/~js/
    

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    Star Formation in Dark Nebulae
    Pillars of Creation
    Pillars of Creation
    Eagle Nebula
    Eagle Nebula
    Pillars of Creation
    Pillars of Creation
    

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    Conditions for Star Formation
    

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    Hydrodynamic Simulation of Superwinds
    ●
    MAIHEM Simulations in FLASH
    Temperature Density
    Danehkar, Oey, Gray +
    

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    Physical Conditions for Star Formation
    
    Cold Gas (10-1000 K) → Molecular Gas (H
    2
    and CO)
    
    Cold Gas (10-1000 K) → Dense Clump
    http://astrodoc.ca/b33/
    Larson 1985
    Omukai et al. 2005
    

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    Physical Conditions for Star Formation
    
    Cold Gas (10-1000 K) → Molecular Gas (H
    2
    and CO)
    
    Cold Gas (10-1000 K) → Dense Clump
    http://astrodoc.ca/b33/
    Larson 1985
    Omukai et al. 2005
    

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    Starburst and Radiation Leakage
    Heckman et al. 1993
    
    Snowplow Phase → Blowout phase
    
    Snowplow Phase: Superbubble
    
    Blowout phase: Radiation Leakage
    

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    Starburst and Radiation Leakage
    Adamo et al. 2010
    Haro 11
    Rivera-Thorsen et al. 2017: UV continuum: green, Ha: red, Lyα: blue
    

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    Starburst and Radiation Leakage
    Rivera-Thorsen et al. 2017: UV continuum: green, Ha: red, Lyα: blue
    Haro 11
    Dynlop 2013
    

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    Photoionization Modeling of Superwinds
    ●
    Emission Lines: C IV, O III], C III], He II
    GP-like galaxies J104557 & J141851 (Berg + 2019)
    

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    Diagnostic Diagrams
    
    BPT Diagram (Baldwin, Phillips & Terlevich 1981)
    Groves et al. 2006
    (Starburst)
    Kewley+ 2001, 2006
    

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    Diagnostic Diagrams
    ●
    Emission Lines of Superwinds
    BPT diagram of GP galaxies (Jaskot & Oey 2013)
    

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    Diagnostic Diagrams
    Amorin + 2017
    AGN: Feltre + 2016
    SF: Gutkin + 2016
    AGN SF
    AGN SF
    AGN SF
    AGN SF
    

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    Diagnostic Diagrams
    ●
    Emission Lines of Superwinds
    Danehkar, Oey, Gray +
    Radiation-bounded
    Density-bounded
    

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    Diagnostic Diagrams
    ●
    Emission Lines of Superwinds
    Zachrusson + 2013
    

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    Starburst and Radiation Leakage
    Adamo et al. 2010
    Rivera-Thorsen et al. 2017: UV continuum: green, Ha: red, Lyα: blue
    Haro 11
    

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    Thank you for your attention
    Thank you for your attention
    Horsehead Nebula
    Horsehead Nebula
    Superwind Suppression in Super Star Clusters
    

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    Superwinds and Super Bubbles
    Massive Globular Cluster M54 (NGC 6715; Siegel et al. 2007)
    

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