Asymmetric explosion of core-collapse supernovae
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1 Asymmetric explosion of core-collapse supernovae Rémi Kazeroni (CEA) Thierry Foglizzo (CEA), Jérôme Guilet (MPA Garching) Journées des doctorants - IRFU 01/07/2015
2 About me Rémi Kazeroni (IRFU/SAp) Advisor: Thierry Foglizzo. Collaborator: Jérôme Guilet (MPA). Curriculum: ENSTA ParisTech + Master M2S (Modélisation et Simulation) Master numerical simulations of the Standing Accretion Shock Instability (SASI). 2
3 PhD thesis Asymmetric explosion of core-collapse supernova Massive stars at the end of their lives explode in supernova. A supernova starts with the collapse of the iron core of the star. The supernova remnant is a neutron star or a black hole. massive star (M > 8-10 Msun) NASA, Hubble Space Telescope SN 1987A 3
4 PhD thesis Asymmetric explosion of core-collapse supernova Hydrodynamic instabilities in the inner region generate large scale asymmetries and impact both the explosion and the properties of the remnant. X spin Guitar 1600km/s Grefenstete+14 blue: Titanium green: Silicon red: Iron nucleosynthesis Palomar Observatory kick 4
5 Outline Standing Accretion Shock Instability & neutron star spin Modeling & numerical simulations Our results Towards more realistic models 5
6 Theoretical framework neutrino-driven explosion (Bethe & Wilson 85) 1D fails (Liebendörfer+ 01) Multi-D hydro instabilities: Neutrino-driven convection SASI ν+n e+p e+p ν+n Foglizzo, RK+ 15 Janka+ 07 6
7 Standing Accretion Shock Instability SASI (Blondin+ 03) Entropyvorticity wave Iron Shock Neutron star Foglizzo+ 07 Iron Acoustic wave Hanke+ 13 Large scale shock oscillations Advective-acoustic cycle Some consequences of SASI Induces a global asymmetry Help successful explosions Unstable modes: l ~ 1-2 Pulsar kick Sloshing modes and spiral modes Pulsar spin 7
8 SASI spiral modes and neutron star (NS) spins Gas dynamics in the supernova core: x bigger and 100 x faster see Foglizzo+ 12 Spin-up of a NS born from a non-rotating progenitor Spin-down a NS born from a rotating progenitor? Counter-rotating NS? Blondin & Mezzacappa 07 8
9 SASI spiral modes and neutron star (NS) spins key issues: Flow pattern: spiral mode or sloshing mode? Only spiral modes can redistribute angular momentum efficiently. spiral mode sloshing mode Fernández 15 What is the timescale to obtain a robust spiral mode? In order to affect the NS spin, a spiral wave must form before the explosion sets in. Blondin & Mezzacappa 07 9
10 Modeling: 2D framework Aim: simplified setup to characterize the hydrodynamics supersonic flow neutron star shock Physics Perfect gas equation of state (γ=4/3) Approximation of the cooling (Blondin & Mezzacappa 06, Fernandez & Thompson 09) No neutrino heating Newtonian potential of a point mass Constant accretion rate subsonic flow 2D cylindrical domain 10
11 Numerical simulations Numerics Simulations with RAMSES: MHD code using Godunov type method. New version: DUMSES-Hybrid running on GPUs r* rsh Parametric study: R=rsh / r* ε = (A2p A2-p)/(A2p + A2-p) Ap: mode amplitude entropy perturbation 11
12 Spiral domination threshold R=3 early spiral mode R=1.67 a sloshing mode dominates: no NS spin-up! Spiral modes dominate only if R=rsh / r* > 2 12
13 Timescale to obtain a spiral mode (Tsp) Tsp decreases with R For R=2.22, Tsp 1s Direction of rotation unpredictable if ε<<1 stochasticity Unexpected direction of rotation 13
14 Non-linear dynamics: reversal of the direction of rotation 14
15 Pulsar spin estimates from analytical calculations and numerical simulations results similar to Fernández 10, Guilet & Fernández 14 paper to be submitted soon: RK, J. Guilet & T. Foglizzo 15 Minimal period: 50ms P 1s Guilet & Fernández 14 SASI may spin-up the NS if R 2.5 SASI may not impact the spin if R <
16 Ongoing work: role of the initial rotation Importance of the rotation Reduces the critical neutrino luminosity required for explosion (Nakamura+14, Iwakami+ 14) A spiral mode may spin-down a NS up to the point of reversing its direction of rotation (Blondin & Mezzacappa 07) Our study Effect on the saturation amplitude? Angular momentum accreted by the PNS? L = βx1016 (cm2/s) β = 0.1 P 6ms Maximal rotational energy available to match with pulsar spin observations? in prep: RK, T. Foglizzo, J. Guilet et al 16
17 Future work: neutrino heating Including neutrino heating (convection) Characterizing convection with rotation in 3D, CPU hours on Occigen (CINES) Imprint on the kick-spin angle? (Mis)alignment related to the hydrodynamics? spin kick Noutsos+ 13 Wongwathanarat
18 Conclusion Spiral vs sloshing mode Reversal of the direction of rotation SASI has the potential to spin-up the NS for an identified set of parameters Impact of the rotation on: - the saturation amplitude of SASI - the NS spin at birth Next step: - convection & rotation in 3D: kick-spin alignment issue. Thanks for your attention! 18
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