modelling photoionisation feedback with mcrt/mcrhdkuiper/... · overview method: mcrt/mcrhd bondi...
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Modelling photoionisationfeedback with MCRT/MCRHD
From massive star formation to diffuse ionised gas
Bert Vandenbroucke ([email protected])
Tübingen Spring Workshop 2020 on Modeling High-Mass Stellar Feedback
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Overview
Method: MCRT/MCRHD
Bondi accretionDiffuse Ionised Gas
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Method: MCRT/MCRHD
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CMacIonize
Regular (or AMR) grid
Voronoi grid
𝐼𝑖 = න𝜈𝑡
∞4𝜋𝐽𝑖 𝜈
ℎ𝜈𝜎 𝜈 d𝜈
≈𝑄
𝑊𝑡𝑉𝑖
𝑗
𝑤𝑗𝑙𝑖𝑗𝜎 𝜈𝑗
BV &Wood (2018)
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Iterative ionization state calculation
Iteratively repeat until convergence(takes approx. 10 iterations)
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Example output
Uniform HII region Turbulent HII region
based on Wood et al. (2013),BV & Sartorio (in prep.)
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Example output (2)
BV et al. (2018)
Hα emission in SILCC DR2
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Algorithmic improvements
2.0Domain-decomposed task-based MCRT
BV, in prep.
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Algorithmic improvements (2)
2.0
BV, in prep.
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MCRHD
Do hydro step
Convert quantities
Do MCRTUpdate
pressure
𝑇 = 𝑇𝑛𝑥𝐻 + 𝑇𝑖 1 − 𝑥𝐻
𝑇𝑛 = 500 K
𝑇𝑖 = 8,000 K
BV & Wood (2018)
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Bondi accretion
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1D Bondi accretion
Isothermal, steady-state accretiononto a point mass
𝑣 𝑟 =−𝐶𝑠 −𝑊−1 −𝜔 𝑟 , 𝑟 ≤ 𝑅𝐵
−𝐶𝑠 −𝑊0 −𝜔 𝑟 , 𝑟 > 𝑅𝐵
𝜔 𝑟 =𝑅𝐵𝑟
4
exp 3 −4𝑅𝐵𝑟
𝜌 𝑟 = −𝜌𝐵𝑅𝐵
2𝐶𝑠𝑟2𝑣 𝑟
Bondi (1952), BV et al. (2019)
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Trapped HII regions
Two-temperature isothermal steady-state accretion
Mestel (1954), Keto (2002,2003), BV et al. (2019)
A similar, closed-form analyticexpression is available
𝑑𝑃
𝑑𝑟< −
𝐺𝑀
𝑟2
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However…
See Lund et al. (2019), BV et al. (2019) for details
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Instability/numerical issue?Slide 21 of 29
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3D accretion: D-type expansion in disk
Sartorio et al. (2019)
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3D accretion: trapped HII regions
Sartorio et al. (2019)
Non-spherical trapped and semi-trappedHII regions also possible
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Critical luminosity
Sartorio et al. (2019)
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Diffuse Ionised Gas
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Diffuse Ionised Gas (DIG)
WHAM survey (2003)Dettmar (1990)
Milky Way: WIMNGC 891
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Modelling DIG
Girichidis et al. (2016) BV et al. (2018)
UV radiationfrom O/B stars
SILCC DR2 DIG model
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RHD modelsIonising luminosity per source
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Discussion
MCRT/MCRHD as a method
not so slow as one might think
1D Bondi: instability vs numerical issue
can someone try this with another method?
The DIG as a constraint for feedback
need discs that have a diffuse gas layer to ionize
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