Reverse construction of initial conditions: from supernovae to - - PowerPoint PPT Presentation

Reverse construction of initial conditions: from supernovae to progenitors Yudai Suwa

Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Key observables characterizing supernovae

Explosion energy: ~1051 erg Ni mass: ~0.1M⦿ Ejecta mass: ~M⦿ NS mass: ~1 - 2 M⦿

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measured by fjtting SN light curves measured by binary systems

fjnal goal of fjrst-principle (ab initio) simulations

related

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Supernova simulation is an initial value problem

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stellar evolutionary calculations ρ(r), T(r), Ye(r), vr(r) supernova explosions

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Uncertainties in stellar evolutionary calculations

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zoning and time step criteria on the final core compactness in two different regions—A:17.1–17.5 and B

NB) all MZAMS=15M⊙

• Nomoto & Hashimoto (1988)

Woosley & Weaver (1995) Woosley, Heger, Weaver (2002) Limongi & Chieffj (2006) Woosley & Heger (2007)

ξM = M/M rM/1000 km Suwa+, ApJ (2016) Sukhbold & Woosley (2014) difgerent spacial resolution difgerent time resolution “Compactness parameter” O’Connor & Ott (2011) Difgerent codes lead to difgerent structure Even with the same code, difgerent (time or space) resolutions lead to difgerent structure

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Asteroseismology

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Constantino+ 2015 Constantino+ 2016 core helium burning (CHeB) stars

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

A possibility

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“key parameter” diagnostic explosion energy (erg) 1049 1050 1051

current stellar evolutionary model ??? what we want!

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Problem reduction

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Takiwaki+ 2016 http://2sn.org/stellarevolution/explain.gif

stellar evolution supernova explosion

time

traditional way new approach stellar structure supernova explosion stellar evolution

• Q1. what is the better initial condition for explosion?
• Q2. Is it possible to produce such structure?

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Parametric initial conditions

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M

M1 M2 M3 M4 M5 Sc S1 S2 S5 Yec Ye3 Ye4 S,Ye

M1: the edge of the fjnal convection in the radiative core M2: the inner edge of the convection zone in the iron core M3: the NSE core M4: the iron core mass M5: the base of the silicon/oxygen shell [Suwa & E. Müller, MNRAS, 460, 2664 (2016)]

• riginal idea is given by Baron & Cooperstein (1990)

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Parametric initial conditions

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105 106 107 108 109 1010 1011 Density [g cm-3] s11.2 WHW02-s11.2-g0.99 WHW02-s11.2-g0.975 WHW02-s11.2-g0.95 0.5 1.0 1.5 2.0 0.0 0.5 1.0 1.5 Ratio to s11.2 Mass [M]

[Suwa & E. Müller, MNRAS, 460, 2664 (2016)] s(Mr) Ye(Mr)

dP dMr = −GMr 4πr4 P(ρ, s, Ye) dMr dr = 4πr2ρ

+

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Parametric initial conditions

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[Suwa & E. Müller, MNRAS, 460, 2664 (2016)]

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Hydrodynamics simulations

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[Suwa & E. Müller, MNRAS, 460, 2664 (2016)]

0.25 0.3 0.35 0.4 0.45 0.5 0.2 0.4 0.6 0.8 1 1.2 1.4 Mass [M] Ye

• 4
• 3
• 2
• 1

Velocity [104 km s-1] 1 2 3 4 5 Temperature [MeV] 5 6 7 8 9 10 11 12 13 14 15 Log(Density [g cm-3]) s11.2 WHW02-s11.2-g0.99 WHW02-s11.2-g0.975 WHW02-s11.2-g0.95 ρc=1011 ρc=1014

50 100 150 200 250 0.1 0.2 0.3 0.4 0.5 Shock radius [km] Time after bounce [s] s11.2 WHW02-s11.2-g0.99 WHW02-s11.2-g0.975 WHW02-s11.2-g0.95 1010 1011 1012 1013 1014 1015

• 0.4
• 0.3
• 0.2
• 0.1

Central density [g cm-3] Time after bounce [s] s11.2 WHW02-s11.2-g0.99 WHW02-s11.2-g0.975 WHW02-s11.2-g0.95 0 0.2 0.4 0.6 0.8 1

Agile-IDSA: 1D/GR/neutrino-radiation hydro code, publicly available

https://physik.unibas.ch/~liebend/download/

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Parameter regime beyond evolution models

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Model Sc S1 S2 S5 Yec Ye3 ρc [kB/baryon] [1010 g cm−3] BC01 0.5 0.63 1.6 4.0 0.415 0.46 2.0 BC02 0.4 0.63 1.6 4.0 0.415 0.46 2.0 BC03 0.6 0.63 1.6 4.0 0.415 0.46 2.0 BC04 0.5 0.53 1.6 4.0 0.415 0.46 2.0 BC05 0.5 0.73 1.6 4.0 0.415 0.46 2.0 BC06 0.5 0.63 1.5 4.0 0.415 0.46 2.0 BC07 0.5 0.63 1.7 4.0 0.415 0.46 2.0 BC08 0.5 0.63 1.6 3.0 0.415 0.46 2.0 BC09 0.5 0.63 1.6 6.0 0.415 0.46 2.0 BC10 0.5 0.63 1.6 4.0 0.411 0.46 2.0 BC11 0.5 0.63 1.6 4.0 0.425 0.46 2.0 BC12 0.5 0.63 1.6 4.0 0.415 0.452 2.0 BC13 0.5 0.63 1.6 4.0 0.415 0.47 2.0 BC14 0.5 0.63 1.6 4.0 0.415 0.46 1.0 BC15 0.5 0.63 1.6 4.0 0.415 0.46 3.0 BC16 0.4 0.73 1.6 4.0 0.415 0.46 2.0 BC17 0.4 0.63 1.7 4.0 0.415 0.46 2.0 BC18 0.4 0.63 1.6 6.0 0.415 0.46 2.0 BC19 0.4 0.63 1.6 4.0 0.425 0.46 2.0 BC20 0.4 0.63 1.6 4.0 0.415 0.47 2.0 BC21 0.4 0.63 1.6 4.0 0.415 0.46 1.0 BC22 0.4 0.63 1.6 4.0 0.415 0.46 3.0

[Suwa & E. Müller, MNRAS, 460, 2664 (2016)]

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Explosions in 1D

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0.1 0.2 0.3 0.4 0.5 0.1 0.2 Diagnostic Energy [1051 erg] Time after bounce [s]

[Suwa & E. Müller, MNRAS, 460, 2664 (2016)]

1 2 3 4 5 1 1.1 1.2 1.3 1.4 Temperature (1010K) Mass (M⊙) Maximum temperature

4.7x1051 erg/s

T9=9 T9=5

mass cut 0.071M⊙ 0.083M⊙

Yudai Suwa @ Many Riddles About Core-Collapse Supernovae /15 27/6/2016

Summary

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Question: How can we produce strong (Eexp~1051 erg) explosion? Possible Answer: Change initial conditions. By starting from specifjc initial conditions, strong explosions are obtained without any change of simulation codes. Next Question: Which kind of stellar evolutionary calculations can produce these perforable presupernova structure?