A03: Explosive Astrophysical Phenomena and Nucleosynthesis based on Quark Dynamics and Nuclear Structure
2011.12.3 @ Shima
Hideyuki Suzuki (Tokyo Univ. of Science)Core Members

Collaborators

PDGrant

Hideyuki Suzuki (TUS)
Masaru Shibata (Kyoto, Numerical Relativity)
Toshitaka Kajino (NAO, Nuclear Astrophysics)
Kohsuke Sumiyoshi (Numazu, Supernova Simulation)
Hideyuki Umeda (Tokyo, Stellar Evolution, Nucleosynthesis)
Akira Ohnishi (Kyoto), Shoichi Yamada (Waseda),
Kohji Uryu (Ryukyu), Satoshi Chiba (JAEA),
Nobuyuki Iwamoto (JAEA), Takashi Yoshida (Tokyo)
Kazuhiro Oyamatsu (Aichi Shukutoku), Masatoshi Takano (Waseda)
Ko Nakamura (NAO), Takashi Yoshida (Tokyo),
Chikako Ishizuka (TUS)
Tomoyuki Hanawa (Chiba), Ken-ichi Nomoto (IPMU),
Shigehiro Nagataki (Kyoto), Hajime Sotani (NAO)

He

H

ONeMg

COFeSi

Main Sequence

BinaryCollapse
M>8M

Mass Loss
GRB,HN

SN II
SNIb

WD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NSν ,GW,Nuclei

SN Iamerge• Yoshida: Stellar Evolution of SN Progenitors and of Rotating Stars• Umeda: Progenitors of ONeMg SNe• Furusawa, Yamada: NSE EOS with multi species of nuclei• Togashi, Yamamuro, Takano, Suzuki: SN EOS using the cluster variational
method(collaboration with A02, A04)
• Ishizuka: towards an EOS database

HeH

ONeMg

COFeSi

Main Sequence

BinaryCollapse
M>8M

Mass Loss
GRB,HNSN II
SNIbWD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BHNS

ν ,GW,Nuclei

SN Iamerge• Sekiguchi: Numerical Relativity with nuclear EOS + ν(simulations of mergerand collapsar models)• Takiwaki, Suwa, Kotake: 2D/3D SN simulations• Ohkita: aspherical explosion of massive CO stars

HeH

ONeMg

COFeSi

Main Sequence

BinaryCollapse
M>8M

Mass Loss
GRB,HNSN IISNIbWDCompanion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NS

ν ,GW,Nuclei

SN Iamerge• Nakazato, Sumiyoshi, Ishizuka, Ohnishi, Yamada, Suzuki: Hyperon interaction (EOS) - 1D BH formation• Izutani, Kikuchi: Systematic study of SN nucleosynthesis (1D models)• Nakamura: Explosion energy with nuclear reactions

HeH

ONeMg

COFeSi

Main Sequence

BinaryCollapseM>8M

Mass Loss
GRB,HN

SN II
SNIb

WD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NS

ν ,GW,Nuclei

SN Iamerge• Kajino: SN,GRB nucleosynthesis with ν oscillations• Wanajo, Nomoto: r-process at SN and NS merger

HeH

ONeMg

COFeSi

Main Sequence

BinaryCollapse
M>8M

Mass Loss
GRB,HN

SN II
SNIb

WD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NS

ν ,GW,Nuclei

SN Iamerge• Kiuchi: Magnetized NS merger• Kyutoku: GW from BH-NS merger - EOS• Hotokezaka: GW from NS-NS merger - EOS• Nagataki: explosiove nucleosynthesis at GRB and HN• Mizuta; thermal radiation from GRB jets (A04)

HeH

ONeMg

COFeSi

Main Sequence

BinaryCollapse
M>8M

Mass Loss
GRB,HN

SN II
SNIb

WD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NS

ν ,GW,Nuclei

SN Iamerge• Sotani: EOS - NS normal oscillations• Nagakura, Sumiyoshi, Yamada: multi-D ν transfer (collaboration with A04)
• Hanawa: A numerical method to solve transfer equations using moments

Hyperon Matter and Black Hole Formation in Failed Supernovae(Nakazato et al., 2011)

Fig. 2.— Time profiles of the central baryon mass density. Thick solid, thin solid, thickdashed, thin dashed, thick dot-dashed and thin dot-dashed lines correspond to the resultsfor EOS’s R, RP, A, AP, N and NP, respectively.

Fig. 4.— Profiles of the particle fractions at bounce (left), 500 msec after bounce (center)and 2 msec before black hole formation (right). The upper and lower panels show results for
EOS’s R and A, respectively.

Ishizuka EOS = Shen EOS + hyperons
Upper: EOS R UΣ = +30MeV,Lower: EOS A UΣ = −30MeV

Evolution of Fluorine Abundances with the ν-ProcessC. Kobayashi et al., 2011

15N(α, γ)19 F in convective Heshell of AGB
20Fig. 1.— Evolution of the [F/O] ratio against [O/H] for the solar
neighbourhood with SNe II, HNe, and SNe Ia only (short-dashedlines), with AGB stars (long-dashed lines), with the ν-process ofSNe II and HNe (solid line and dot-dashed line for Eν = 3 ×1053 and 9 × 1053 erg, respectively). The dotted line is for themodel for globular clusters. The observational data sources are:open circles, Cunha et al. (2003), open squares, Cunha & Smith(2005) for the solar neighbourhood stars; filled circles, Cunha et al.
(2008) for bulge stars. For the stars in globular clusters, crosses,
Yong et al. (2008), NGC 6712; plus, Smith et al. (2005), M4; stars,Cunha et al. (2003), ω Cen; asterisks, Alves-Brito et al. (2011, inpreparation), M22.

Ne(ν, ν 0 p)19 F at Type II SNeNeutrino induced reactions related to the ν-process nucleosynthesis of 92 Nb and98TcM-K.Cheoun et al., 2011
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erg / s]
53LMHerg / s] Lν [10(a)1.0erg / s] Lν [10530.1
7.0 (b)
6.0
5.0
4.0
3.0
2.0
1.0
10 (c)

53

50-50510152025t - tmerge [ms]FIG. 1 (color online). (a) Maximum rest-mass density,(b) maximum matter temperature, and (c) total neutrino luminosity as functions of time for three models. The dashed verticalline shows the time at which a BH is formed for model H.

Lν [10Lν [1053erg/s]

Tmax [10 MeV] ρmax [1015 g/cm3]

Gravitational Waves and Neutrino Emission from the Merger of Binary NeutronStars (Sekiguchi et al., 2011 PRL107, 051102)
2 (a) L1νeνeνx03 (b) M
2105 (c) H
43210-5101
100
10-1
10-20510158 9 10 11 12 13 14 15 162025t - tmerge [ms]FIG. 3 (color online). Neutrino luminosities for three flavors
for three models. (a) L, (b) M, and (c) H. The inset of (c) focuseson the luminosities in the BH formation. The meaning of thedashed line is the same as in Fig. 1.

L: 1.35-1.35MM: 1.5-1.5M
Hypermassive NSτ  τdyn
H: 1.6-1.6M(BH in τdyn )FIG. 2 (color online). Color maps of rest-mass density (with velocity fields), temperature, and total neutrino luminosity at t ( 15 ms
after the merger for model M. The upper and lower panels show the configuration in the x-y and x-z planes, respectively.

Eﬀects of hyperons in binary neutron star mergers (Sekiguchi et al., 2011)

2.0
1.0
0.0
5.0
4.0
3.0
2.0
1.0
0.0aνeνe
νx05101520aνeνeaνe46x-202S16νx053.2νx

ν νe

νe

810(H)

(S)

aνe

1015

2.4
2.2

1.824681012-21

10S15H15S165

tret - tmerge [ms]1016FIG. 5: fGW (t) in the HMNS phase, smoothed by a weightedspline, for H135 (solid red), S135 (dashed green), and S16(dashed-dotted blue).

S135
H135

014

tret - tmerge [ms]heff (D = 100 Mpc)

h+ [10-22] (D = 100Mpc)

2.620FIG. 3: Neutrino luminosities for H135 and S135 (top), H15and S15 (middle), and S16 (bottom). The dotted verticallines show the time at which a BH is formed. The solid anddashed curves correspond to the result with the Hyp-EOS andShen-EOS, respectively.

(a)

2.8

2t - tmerge [ms]210-1-22
10-1-22
10-1-2-5

H135
S135
S16

3

fGW [kHz]

erg/s]

H15 / S15

3.053

H135 / S135

Lν [102.0
1.5
1.0
0.5
0.0

15

S16
S135
S15
H135
H15LCGTbLIGO

10-22

10-23

1(b)

2345678

frequency [kHz]FIG. 4: (a) GWs observed along the axis perpendicular to the orbital plane for the hypothetical distance to the source
D = 100 Mpc. (b) The effective amplitude of GWs defined by 0.4f |h(f )| as a function of frequency for D = 100 Mpc. The
noise amplitudes of a broadband configuration of Advanced Laser Interferometer Gravitational wave Observatories (bLIGO),and Large-scale Cryogenic Gravitational wave Telescope (LCGT) are shown together.

H: Shen EOS with Λ
S: Shen EOS without
hyperons
135: 1.35-1.35M
15: 1.5-1.5M
16: 1.6-1.6M

Three-dimensional Hydrodynamic Core-Collapse Supernova Simulations for an
11.2M Star with Spectral Neutrino Transport
Takiwaki et al., 2011

multigroup ν transfer with IDSA
(Isotropic Diﬀusion Source Approx.)
10000
S11.2-3D

Shock radius [km]Radius [km]

1.40
1000
1.30

100

10-100-50050

100150200

Time after bounce [ms]250300

2000
1800
1600
1400
1200
1000
800
600
400
200
02D
3D
3D low

050

100
150200Time after bounce [ms]250300Fig. 7.— Time evolution of the 3D model, visualized by mass shell trajectories in thin graylines (left panel). Thick red lines show the position of shock waves, noting that the maximum(top), average (middle), and the minimum (bottom) shock position are shown, respectively.
The green line represents the shock position of the 1D model. ”1.30” and ”1.40” indicatesthe mass in unit of M⊙ enclosed inside the mass-shell. Right panel shows the evolution ofaverage shock radii for the 2D (green line), and 3D (red line) models. The ”3D low” (pinkline) corresponds to the low resolution 3D model, in which the mesh numbers are taken tobe half of the standard model (see Section 2).

Fig. 1.— Three dimensional plots of entropy per baryon (left panels) and logarithmic density(right panels, in unit of g/cm3 ) for three snapshots (top; t = 15 ms, middle; t = 65 ms, andbottom; t = 125 ms measured after bounce (t ≡ 0)) of our 3D model. In the right panels,velocities are indicated by arrows. The contours on the cross sections in the x = 0 (back京都大学基礎物理学研究所研究会「超新星爆発と数値シミュレーション」
2011 年 12 月 26 日 (月)-28 日 (水)京都大学基礎物理学研究所 湯川記念館パナソニックホール
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次世代スーパーコンピューター戦略プログラム：分野５「物質と宇宙の起源と構造」
科研費基盤研究（S）「超新星の爆発機構とガンマ線バースト源エンジンの統一的解明」（代表 佐藤勝彦）
新学術領域研究「素核宇宙融合による計算科学に基づいた重層的物質構造の解明」（領域代表者 青木慎也）共催