Reverse construction of initial conditions: from supernovae to progenitors Yudai Suwa Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University
Key observables characterizing supernovae Explosion energy: ~10 51 erg measured by fj tting Ni mass: ~0.1M ⦿ SN light curves Ejecta mass: ~ M ⦿ related measured by NS mass: ~1 - 2 M ⦿ binary systems fj nal goal of fj rst-principle ( ab initio ) simulations 2 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Supernova simulation is an initial value problem stellar evolutionary calculations ρ (r), T(r), Y e (r), v r (r) supernova explosions 3 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Uncertainties in stellar evolutionary calculations Suwa+, ApJ (2016) Sukhbold & Woosley (2014) Nomoto & Hashimoto (1988) Woosley & Weaver (1995) Woosley, Heger, Weaver (2002) Limongi & Chie ffj (2006) Woosley & Heger (2007) NB) all M ZAMS =15M ⊙ di fg erent spacial resolution Di fg erent codes lead to di fg erent structure di fg erent time resolution Even with the same code, di fg erent (time or space) resolutions lead to di fg erent structure zoning and time step criteria on the final core compactness in two different regions—A:17.1–17.5 and B M/M � “Compactness parameter” ξ M = r M / 1000 km O’Connor & Ott (2011) 4 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15 �
Asteroseismology Constantino+ 2015 Constantino+ 2016 core helium burning (CHeB) stars 5 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
A possibility what we want! diagnostic explosion energy (erg) 10 51 10 50 current stellar evolutionary model ??? 10 49 “key parameter” 6 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Problem reduction new approach traditional way supernova explosion supernova explosion Q1. what is the better initial condition for explosion? stellar structure time Takiwaki+ 2016 http://2sn.org/stellarevolution/explain.gif Q2. Is it possible to produce such structure? stellar evolution stellar evolution 7 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Parametric initial conditions [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] S,Y e original idea is given by Baron & Cooperstein (1990) Y e4 S 5 Y e3 S 2 Y ec S 1 S c M M 1 M 2 M 3 M 4 M 5 M 1 : the edge of the fj nal convection in the radiative core M 2 : the inner edge of the convection zone in the iron core M 3 : the NSE core M 4 : the iron core mass M 5 : the base of the silicon/oxygen shell 8 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Parametric initial conditions [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] s ( M r ) Y e ( M r ) 10 11 P ( ρ , s, Y e ) 10 10 Density [g cm -3 ] dP = − GM r 10 9 4 π r 4 dM r 10 8 + 10 7 s11.2 dM r WHW02-s11.2-g0.99 10 6 = 4 π r 2 ρ WHW02-s11.2-g0.975 dr 10 5 WHW02-s11.2-g0.95 2.0 Ratio to s11.2 1.5 1.0 0.5 0.0 0.5 1.0 1.5 Mass [M � ] 9 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Parametric initial conditions [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] 10 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Hydrodynamics simulations [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] https://physik.unibas.ch/~liebend/download/ Agile-IDSA: 1D/GR/neutrino-radiation hydro code, publicly available 10 15 15 s11.2 ρ c =10 11 14 WHW02-s11.2-g0.99 ρ c =10 14 Log(Density [g cm -3 ]) 13 WHW02-s11.2-g0.975 10 14 12 Central density [g cm -3 ] WHW02-s11.2-g0.95 11 10 9 s11.2 10 13 8 WHW02-s11.2-g0.99 7 WHW02-s11.2-g0.975 6 WHW02-s11.2-g0.95 10 12 5 5 Temperature [MeV] 4 10 11 3 2 10 10 -0.4 -0.3 -0.2 -0.1 0 0.2 0.4 0.6 0.8 1 0 1 Time after bounce [s] 0 250 Velocity [10 4 km s -1 ] s11.2 -1 WHW02-s11.2-g0.99 WHW02-s11.2-g0.975 -2 WHW02-s11.2-g0.95 200 Shock radius [km] -3 -4 150 0.5 0.45 0.4 100 Y e 0.35 0.3 50 0.25 0 0.1 0.2 0.3 0.4 0.5 0 0.2 0.4 0.6 0.8 1 1.2 1.4 Time after bounce [s] Mass [M � ] 11 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Parameter regime beyond evolution models [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] Model S c S 1 S 2 S 5 Y ec Y e 3 ρ c [10 10 g cm − 3 ] [ k B / baryon] BC01 0.5 0.63 1.6 4.0 0.415 0.46 2.0 BC02 0.63 1.6 4.0 0.415 0.46 2.0 0.4 BC03 0.63 1.6 4.0 0.415 0.46 2.0 0.6 BC04 0.5 1.6 4.0 0.415 0.46 2.0 0.53 BC05 0.5 1.6 4.0 0.415 0.46 2.0 0.73 BC06 0.5 0.63 4.0 0.415 0.46 2.0 1.5 BC07 0.5 0.63 4.0 0.415 0.46 2.0 1.7 BC08 0.5 0.63 1.6 0.415 0.46 2.0 3.0 BC09 0.5 0.63 1.6 0.415 0.46 2.0 6.0 BC10 0.5 0.63 1.6 4.0 0.46 2.0 0.411 BC11 0.5 0.63 1.6 4.0 0.46 2.0 0.425 BC12 0.5 0.63 1.6 4.0 0.415 2.0 0.452 BC13 0.5 0.63 1.6 4.0 0.415 2.0 0.47 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 1.6 4.0 0.415 0.46 2.0 0.4 0.73 BC17 0.63 4.0 0.415 0.46 2.0 0.4 1.7 BC18 0.63 1.6 0.415 0.46 2.0 0.4 6.0 BC19 0.63 1.6 4.0 0.46 2.0 0.4 0.425 BC20 0.63 1.6 4.0 0.415 2.0 0.4 0.47 BC21 0.63 1.6 4.0 0.415 0.46 0.4 1.0 BC22 0.63 1.6 4.0 0.415 0.46 0.4 3.0 12 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Explosions in 1D [Suwa & E. Müller, MNRAS, 460 , 2664 (2016)] 5 0.5 mass cut Maximum temperature Diagnostic Energy [10 51 erg] 4 0.4 Temperature (10 10 K) 4.7x10 51 erg/s 3 0.3 2 0.2 0.071M ⊙ T 9 =9 1 0.1 T 9 =5 0.083M ⊙ 0 0 1 1.1 1.2 1.3 1.4 0 0.1 0.2 Mass (M ⊙ ) Time after bounce [s] 13 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
Summary Question: How can we produce strong (E exp ~10 51 erg) explosion? Possible Answer: Change initial conditions. By starting from speci fj c 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? 15 Yudai Suwa @ Many Riddles About Core-Collapse Supernovae 27/6/2016 /15
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