ニュートリノ駆動型 超新星爆発シミュレーション ３Ｄと２Ｄの比較
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1 2014/7/8 Joint Meeting among Explosion Mechanism of Core-collapse Supernovae Tomoya Takiwaki (NAOJ->RIKEN)
2 Press Release in April There are two press release on supernovae in last April One: Lensed extremely luminous type Ia supernova. The other: 3D explosion of type II supernova found in K- computer.
3 Why is CC SN interesting? Last time of massive stars Birth of neutron star Mother of supernova remnant One of the most luminous object in the universe Target of Multi-messenger astrophysics Source of heavy elements in galaxies 4 kinds of force affects the explosion mechanism
4 Ni mass~ E_exp Various Kinds of CC supernovae Nomoto+2006 Initial Mass of Progenitor Fate of the star differs from the properties of the progenitor: 1. Mass 2. Metallicity 3. Rotation 4. Magnetic Field
5 Two class of CC SNe Neutrino Mechanism Rotation We focus on this Magnetic Mechanism Magnetic Fields Rotation BH magnetar pulsar Mass Mass
6 Neutrino Mechanism I ll explain one by one 1. Initial setup 2. Key aspects of neutrino mechanism 3. Simulations 4. Effect of Rotation
7
8 Neutrino Mechanism I ll explain one by one 1. Initial setup 2. Key aspects of neutrino mechanism 3. Simulations 4. Effect of Rotation
9 Key aspects of Neutrino Mechanism Radial Velocity Entropy~T^3/ρ Proto Neutron Star Post Shock Postshocked n,p Pressure Heated by neutrino Shock Preshocked Fe Ram Pressure Radius Fe=>n, p cooled by photodissociation The shock is stalling. Pressure inside and ram pressure out side balances. RHS is determined by stellar structure(density profile). LHS is determined by two ingredients. (1) Photodissociation (2) Neutrino Heating
10 A example of the failed supernovae Non-Explosion Is observed Entropy is visualized Spherical symmetric simulations
11 Key aspects of Neutrino Mechanism Entropy~T^3/ρ Proto Neutron Star Heated by neutrino Heated by convection Fe=>n, p cooled by photodissociation Radius Negative entropy gradient leads Rayleigh-Taylor instability (Cold heavy matter is put over Hot light matter) Rayleigh-Taylor convection transfer energy outward. Cooler than the initial state but ν heat is active Hotter than the initial state
12 Neutrino Mechanism I ll explain one by one 1. Initial setup 2. Key aspects of neutrino mechanism 3. Simulations 4. Effect of Rotation
13 s11.2(light Progenitor) Ω=0rad/s Explode! Convection Dominant EoS:LS-K220 resolution: 384(r)x128(θ)x256(φ) The finest grid Neutrino Trasport: Ray-by-Ray:IDSA +Leakage Hydro: HLLE, 2 nd order
14 Shape of the explosion? Many hot bubble is observed. That is evidence of strong convection.
15 s27(heavey Progenitor) Ω=0rad/s Failed (or need long-term sim.) EoS:LS-K220 resolution: 384(r)x64(θ)x128(φ) Neutrino Transport: Ray-by-Ray:IDSA +Leakage Hydro: HLLE, 2 nd order
16 Neutrino Luminosity Mass accretion vs neutrino heating explode 11.2 GR effect? 27.0 fail Mass accretion rate Heavier progenitor results high mass accretion rate and high ram pressure. That spoils the explosion. GR effects(or update of microphysics) can change the situation.
17 Nakamura+14.
18 slide from suwa Nakamura+ 14.
19 Nakamura+ 14.
20 Nakamura+ 14
21 Neutrino Mechanism I ll explain one by one 1. Initial setup 2. Key aspects of neutrino mechanism 3. Simulations 4. Effect of Rotation
22 Bar mode instability Rapid Rotation => spiral instability In the rigid ball, Rotational energy(t)/gravtational energy(w)=14% In Sne case, criteria becomes smaller. Called low-t/w instability
23 Neutrino + rotation Spiral wave transfer the energy to the outer regon. Finally explosion is found!
24 Shape of the explosion? Strong expansion is found at equatorial plane
25 The mass of the progenitor and rotation make various type of Explosion(or Non Explosion).
26 Does rotation affect the shock revival? Rapid rotation s11.2 N13 s27.0 Rapid rotation 1D=> no shock revival s11.2 : No N13 : Yes s27 : Yes
27 How energetic is that? s11.2 Rapid rotation Rapid rotation N13 s27.0 Rapid rotation Observe ^51erg! It s close to 10^51 erg!
28 Message Although CC SNe are not completely understood, we are close to solve the problem. (It s might be semi-final match or final match?) Quite nice model (close to the real one) can be obtained. When should we start the collaboration on astronomy with realistic supernovae model? Now s the time!
29 超新星シミュレーションの新問題 多次元モデルは物理のインプットに敏感で手法によって爆発したりしなかったりする 2 次元モデル ( 複数親星に対して ) Bruenn+12: 全部爆発 Mueller+13: おおよそ爆発 Dolence+14: 一つも爆発しない Nakamura+14: 全部爆発 Suwa in prep: 半分ほど爆発 Hanke in prep: おおよそ爆発 3 次元モデル ( 複数親星に対して ) Hanke in prep: 一つも爆発しない Takiwaki in prep: 半分ほど爆発 1D 2D 爆発する 3D インプットのエラーの範囲 爆発しない
30 超新星シミュレーションの新問題 多次元モデルは爆発するにせよしないにせよ非常にぎりぎり 定量的な評価を確定するためには相当手法に凝る必要がある! Ott+12 今後は数値計算の信頼性がとにかく大事!
31 ロードマップ とにかくすべてのインプットをアップデートせよ! Most realistic model の変遷 Hanke+13 Kuroda in prep フル GR Non Ray-by-Ray 6 次元ボルツマン Takiwaki+14 ニュートリノ反応現象論的 GR ペタスケール エクサスケール ~2020 Kuroda 論文での結論と 6 次元ボルツマンでの計算に今後は注目! 2020 年ぐらいまでにはかなりの決着を見るのでは?
32 ニュートリノ + 磁場 磁気回転不安定性で対流安定な場所でも乱流的になる それがニュートリノ加熱に効くかもしれない 高解像度計算が必要すぐに完全な計算はできない徐々に調べる 現在 政田くんと研究中 澤井くんも同様のことを指摘
33 ニュートリノ +SASI 爆発 Advective-acoustic cycle Pressure Wave Foglizzo s slides Vorticity Wave Standing Accretion Shock Instability(SASI) 渦が落ちる時間スケールで成長が律速 上から物がどんどん降ってくるとき成長しやすい Scheck+ 2008
34 SASI 爆発は起こるか? 2D 3D Takiwaki+2012 Iwakami+14 CC 的に爆発しにくいところでドミナントになる この不安定性で爆発に転じるのは今のところ難しい見通し
ニュートリノ駆動型 超新星爆発シミュレーション ３Ｄと２Ｄの比較
2016/01/05 宇宙の歴史をひもとく地下素粒子原子核研究 第二回超新星ニュートリノ研究会 ニュートリノ観測による超新星爆発メカニズムの探求 滝脇知也 ( 理化学研究所 ) 1 2 Three phases of supernovae Presupernova phase Burst phase Accretion phase Cooling phase Kato+2015 吉田敬さん石徹白さん
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