A03: Astrophysics Group
Explosive Astrophysical Phenomena and Nucleosynthesis based on
Quark Dynamics and Nuclear Structure
2012.12.13 @ Nara
Hideyuki Suzuki (Tokyo Univ. of Science)Core Members

Collaborators

Hideyuki Suzuki (TUS)
Masaru Shibata (Kyoto, Numerical Relativity)
Toshitaka Kajino (NAOJ, 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)

HHe

ONeMg

COFeSi

Main Sequence
Collapse
M>8M

Mass Loss

BinaryGRB,HNSN II
SNIbWD

Companion

SNIc
NS/BH
Nucleosynthesis

NS/BH
NSν ,GW,Nuclei

SN Ia
merge

A03 Astrophysics
Stellar Evolution
Umeda, Yoshida
Progenitor Model

Nucleosynthesis
Umeda, Kajino, Iwamoto, Chiba
Dynamics

Collapsar, Neutron Star Merger/Gravitational Waves
Shibata, Uryu
Supernova Explosion/Black Hole Formation/SN Neutrinos
Sumiyoshi, Yamada, Suzuki
Equation of States
Ohnishi, Takano, Oyamatsu
Neutrino Transfer
Interaction Rates
A02 Nuclear Physics
A04 Numerical Techniques

The grant was mainly used for the employment of PDs.
• Luca Baiotti (Kyoto, 2009.11-2010.1)• Kenta Kiuchi (Kyoto, 2010.2-2011.3)• Takashi Yoshida (Tokyo, 2009.4-)• Ko Nakamura (NAOJ, 2009.4-2012.9)• Chikako Ishizuka (TUS, 2011.4-2012.9)• Hirotada Okawa (Kyoto, 2012.4-2012.7)

Grants for related research (FY2009-2010,2011-2012)• T. Hanawa (Chiba): MHD wave
超新星爆発における磁気流体波の反射増幅効果の研究• K. Nomoto (Tokyo): r-processr プロセス元素の起源の超新星爆発シミュレーションに基づく解明• S. Nagataki (Kyoto): GRB/HN nucleosynthesis
ガンマ線バースト・極超新星に於ける爆発的元素合成• H. Sotani (NAOJ): NS matter - GW
重力波観測を用いた中性子星内部における物質構造への制限の可能性• Y. Sekiguchi (NAOJ): NS mergers/SGRB with numerical relativity
数値相対論で探る連星中性子星の合体とショートガンマ線バースト• N. Yasutake (NAOJ): QCD phase transition in PNS
超新星爆発後期の原始中性子星進化におけるＱＣＤ相転移の役割

Workshops• 1st Workshop(3rd Numazu Workshop on EOS)
2009.3.16-18, Numazu College of Technology
第３回沼津ワークショップ「クォーク力学・原子核構造に基づく爆発的天体現象と元素合成」• 2nd Workshop
2010.5.31-6.1, Tokyo University第 2 回「クォーク力学・原子核構造に基づく爆発的天体現象と元素合成」研究会• 3rd Workshop
2011.1.31-2.1, Ryukyu University
第 3 回「クォーク力学・原子核構造に基づく爆発的天体現象と元素合成」研究会• 4th Workshop with HPCI Field 5, Project-3
2011.12.26-28, Kyoto University
超新星爆発と数値シミュレーション
About 100 papers

Topics• Stellar Evolution of SN Progenitors (ONeMg or Fe cores) and of Rotating
Stars (talk by Yoshida, poster by Takahashi)• SN EOS using the cluster variational method(collaboration with A02, A04)
(talk by Togashi, poster by Takano)• NSE EOS with multi species of nuclei (poster by Furusawa)• hadron - quark phase transition (poster by Yasutake)• constructing EOS database• Numerical Relativity with nuclear EOS + ν(simulations of mergers andcollapsar models) (talks by Sekiguchi, Kiuchi)• 2D/3D SN simulations (talk by Suwa, poster by Nakamura)• Stellar collapse with nucleon/hyperon/quark EOSs (talk by Nakazato, Sumiyoshi)• SN,GRB nucleosynthesis with ν oscillations• r-process at SNe and NS mergers (talk by Wanajo)• EOS - GW connections (poster by Hotokezaka)• explosiove nucleosynthesis at GRB and HN (poster by Nagataki)• GRB jets (poster by Mizuta, A04)
• EOS - NS asteroseismology (poster by Sotani)• multi-D ν transfer (collaboration with A04) (talk by Sumiyoshi)

erg / s]
53

LM
Herg / 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

50-50

5

1015

2025t - 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]

toward 3D Numerical Relativity with realistic EOS and ν transfer
Gravitational Waves and Neutrino Emission from the Merger of Binary NeutronStars (Sekiguchi et al., 2011 PRL107, 051102)
2 (a) L1νeνeνx0
3 (b) M2105 (c) H
432
10-5

101
100
10-1
10-2

0510158 9 10 11 12 13 14 15 162025

L: 1.35-1.35M
M: 1.5-1.5M
Hypermassive NSτ  τdynt - 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.

H: 1.6-1.6M(BH in τdyn )polytropic EOS
no ν transfer↓
realistic EOS
ν transfer(leakage scheme)↓ 2012
moment scheme

FIG. 2 (color online). Color maps of rest-mass density (with velocity fields), temperature, and total neutrino luminosity at t ( 15 msafter the merger for model M. The upper and lower panels show the configuration in the x-y and x-z planes, respectively.

developement of 3D neutrino transfer (collaboration with A04)

Figure 35. Contour plots of the neutrino distributions on the meridian slice with φ = 0.436 radian (near zx-plane) for electron-type anti-neutrinos in the 3D deformed
supernova core. The density, radial, polar, and azimuthal components of the flux are displayed by color codes in the left top, right top, left bottom, and right bottom
panels, respectively. The densities are shown in the unit of fm−3 = 10−39 cm−3 and in log scale. The fluxes are shown in the unit of fm−2 s−1 .
(A color version of this figure is available in the online journal.)

polar and azimuthal flux from static deformed core
Sumiyoshi and Yamada, ApJS199 (2012) 17, Fig.35

Hyperon Matter and Black Hole Formation in Failed Supernovae (1D study)(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

Toward a new EOS of supernova matter
Collaboration with A02 group (Togashi and Takano)
EOS for uniform matter using the cluster variational method with AV18+UXI
potentials

0.12
0.1
0.08
0.06
0.04
0.02
00.1
0.08
0.06
0.04
0.02
00.1
0.08
0.06
0.04
0.02
00.1
0.08
0.06
0.04
0.02
0NeutronProton13.8

nB =10g/cm3, T=10MeV,Yp = 0.4
Z = 93, N = 228

13.7

nB =10g/cm3

Z = 67, N = 164
0.5

13.6

nB =103g/cm

Nucleus + Gas

0.4

Z = 50, N =120Gas

Matter

0.3

Ypn i (fm -3 )EOS for non-uniform matter (single nuclei + free nucleons) using ThomasFermi calculation (following a strategy of H. Shen EOS with RMF)

13.5

nB =10g/cm30.2

Z = 33, N = 790.1
0010203040 50r(fm)

60

70

80

T=10MeV
68nucleon distribution(T = 10MeV,YP = 0.4)
Yamamuro et al. in progress

101214log nB [ g/cm3 ]phase diagram (T = 10MeV)

from EOS with single representative nuclei to EOS with multicomponent in Nuclear Statistical Equilibrium

Figure 1. Mass fractions in log10 of nuclei in the (N, Z) plane for ρB = 1011 g cm−3 , T = 1 MeV, and Yp = 0.3. The cross indicates the representative nucleus for
the H. Shen EOS under the same condition.

Figure 5. Average mass number, Ā, of heavy nuclei with Z > 6 for our EOS (solid red lines) and Hempel’s EOS (dotted green lines) together with the mass numberof representative nucleus for H. Shen’s EOS (dashed blue liens) as a function of density for T = 1 MeV and Yp = 0.1, 0.3, 0.5. The insets are the close-ups of thehigh density regimes.

Figure 2. Mass fractions in log10 of nuclei in the (N, Z) plane for ρB = 1013.5 g cm−3 , T = 1 MeV, and Yp = 0.3. The cross indicates the representative nucleus for
the H. Shen EOS under the same condition.

√Figure 6. Square of mass numbers (top), the standard deviation of mass number, σA = A2 − Ā2 (middle), and the dispersion normalized by the average mass
number squared, σA2 /A2 (bottom), of heavy nuclei with Z > 6 for T = 1 MeV and Yp = 0.1 (left), 0.3 (middle), and 0.5 (right). In the top panels, the solid anddotted lines show the average mass number squared, A2 , and the square of average mass number, Ā2 , in our EOS, respectively, whereas the dashed lines display themass number squared of the representative nucleus for the H. Shen EOS.

neutrino coherent scattering off nuclei depends strongly on mass number A
Furusawa et al., ApJ 738 (2011) 178

electron capture rates in NSE should be compiled with NSE EOS
shell blocking + single nuclei scheme underestimates the e-cap. rate.

FFN

Sekiguchi et al. in progressNSEconstructing Nuclear EOS Database
70.0
H. Shen (2011)
M. Hempel (2010)T. Miyatsu (2012)
T. Niksic (2002)

746

60.0

50.0

Esym

40.0

30.0

20.0

10.0

0.0
0.0

0.1

0.1

0.2

0.2

0.2

0.3

RhoB

Figure 2: Figure made by the EOSDB, saved online as a eps file and downloaded. Symmetric energy ofrecent three Relativistic Mean Field models [10, 11, 12] and its constraint citeNiksic2002 shown in Fig.1.

Ishizuka NIC2012

Supernova Neutrino Database (various progenitors)(1D hydro simulation + protoneutron star cooling, connected by a parametercorresponding to the shock revival time)

Nakazato et al., arXiv:1210.0684

Stellar Evolution: Fe core or ONe core?
10Mlog Tc [K]9.5

M

99.82M
9.89M
10M
11M
12M

8.567893log ρc [g/cm ]Umeda, Yoshida and Takahashi, 20121011

neutrino-related nucleosynthesis
1.2
1

0.6

Neutrino induced reactions related tothe ν-process nucleosynthesis of 98 Tc M-

0.4

K.Cheoun et al., 201111N( Li)/N( B)

Normal0.8

7Inverted

0.2
0-5
1035

10-4-3102
sin 2 13

10-2

10-1

FIG. 1. Produced 7 Li=11 B abundance [15] as a function of
mixing angle for both a normal and inverted neutrino mass
hierarchy. This ratio varies in models with different neutrino
temperatures in the range indicated by the lower and upper solidlines. The width of the shaded region indicates the 21 confidence
limits to sin2 ð2)13 Þ from the Daya Bay result [7]. The top of theshaded region is the 21 upper limit on the observed -process
7 Li=11 B ratio as deduced here from the SiC X grains.

G. J. Mathews, T. Kajino, et al., PRD85 (2012),
10502389! "%$ 33

89! "#$!3:

41!
-'&()(* !+,!35! "%$41!
-'&*)(* !+,!33

41&'(()(* !+,3567.!/012+
3367

Summary• Systematic studies on EOSs and progenitor models with 1D simulations ofcore collapse and neutrino signal• Appreciable progress toward 3D simulations with GR + ν transfer(well connected to HPCI)• Good collaborations with A02 (Nuclear Physics) and A04 (ComputationalScience)
still in progress: new SN EOSs, electron capture rates
wish: hyperonic EOS from Lattice QCD in near future• Development of stellar evolution codes and databases (EOSs, SN neutrinospectra)• Nucleosynthesis (explosive process, r-process, ν-process)