The 4th DTA Symp. on Compact Stars and GW Astronomy
NAOJ Mitaka, May 13-14, 2016

Neutrinos and Element Genesis
as a probe of EOS andBinary Neutron Star Mergers
Taka KAJINO
National Astronomical Observatory of Japan
Department of Astronomy, The University of TokyoPurpose

Proto-neutron star

1. How to determine n-Mass Hierarchy
through MSW Effectn’s stream out.

■ Relic SN-n (in SK & HK)+ EOS of the Neutron Stars■ n-Nucleosynthesis & Cosmic Clock
Remarkably Sensitive to MSW EffectNucleosynthesis

2. How to approach Collective n–Oscillation■ Origin of r-Process
Core-Collapse Supernovae
vs. Binary Neutron Star Mergers ?

■ Origin of Life
Amino Acid on the Earth, all L-handed

Relic n travels in space.

Two Astronomical Motivations
G.J. Mathews, J. Hidaka, T. Kajino & J. Suzuki, ApJ 790(2014),115 ― SNR problem.
K. Nakazato, E. Mochida, Y, Niino, H. Suzuki, ApJ 804 (2015), 75 ― Metallicity Evol.

Supernova Rate Problem

Red Super-Giant Problem

failed-SNe with BH

Critical mass for failed-SNe ?

Horiuchi, Beacom et al., ApJ 738 (2011) 154.

Smartt, S.J. 2009, ARA&A 47, 63; 2015, PASA 32, e016

Simultaneous Solution ?
at BIRTH !

MC=25M

BH

50% missing?
at DEATH !

(16.5-18.0)+/- 1.5 M
Observed Mass of RSG (Init. Mass for SN)

Our Solution to SNR & RSG Problems vs. Init. Mass Function
Cosmic Star Formation Rate

Initial Mass Function

f0(M) ∝ M-2.35

Salpeter (1955)(16.5-18.0)M

MC=25M→ Neutrino Signal ?
→ EOS, n-Oscillation ?

failed SNe → Black Hole

Survey of Numerical SN-Simulations
Horiuchi, Nakamura, Takiwaki, Kotake, & Tanaka, MNRAS 445 (2014), L99
Woosley, Heger, Weaver, RMP 74 (2002), 1015.
Compactness parameter:compactnessfor Mb = 2.5
at core-bounce
parameter

Larger accretion & ram pressurethat the shock must overcome!
(large)2.5(small)r(Woosley, Heger & Weaver 2002)

Progenitors

Consistent with
MC =(16.5-18.0)M

failFailure

success
16.5

Successful explosion

Theoretical n-Spectra for Various Supernovae
Electron-capture SNe
Normal CC-SNe
Failed SNe(Faint Ne)(Neutron Star fromation) (Black Hole formation)

1.1

Pair-n heated SNe(BH + Acc. Disk)

1.5s

ONeMg SNe: Hudepohl, et al., PRL 104 (2010).

CC-SNe:Yoshida, et al., ApJ 686 (2008), 448;
Suzuki & Kajino, J. Phys. G40 (2013) 83101.

fSN (failed SNe): Sumiyoshi, et al., ApJ 688 (2008) 1176.
* Shen-EOS (stiff): Shen et al. Nucl. Phys. A637 (1998) 435.
* LS-EOS (soft, K=180): Lattimer & Swesty, Nucl. Phys. A535 (1991) 331.
GRBs: Nakamura, Kajino, Mathews, Sato & Harikae, Int. J. Mod. Phys. E22 (2013)
1330022; Kajino, Mathews & Hayakawa, J. Phys. G41 (2014) 044007.

Neutrino Signal
from failed SNeSumiyoshi, Yamada,& Suzuki
ApJ 688 (2008)1176.
Average Energy

En ∝ Tn

Tn x
Tn e
BH forms!

LS’sShen’sSoft EoS

Stiff EoS

Luminosity
Ln e
Ln e
Ln mt Ln mtTn e

Spectrum of Relic Supernova Neutrinos(RSNs)
Mathews et al. 2014; Totani et al. 1996, ApJ 460, 303; Lunadini 2009, PRL 102, 231101.
RedshiftedExpanding Universe

G.J. Mathews, J. Hidaka, T. Kajino& J. Suzuki, ApJ 790(2014),115.

101

SN Raten-Spectra
10010-1

Atmospheric-n10-2103

No n-oscillation
10-40102030
En (MeV)

405060Gd-loaded Water Cherenkov Detector
SK(22.5kton)

HK(1Mton)

Vagins and Beacom, PRL 93 (2004), 171101.

Present signal

New signal

COINCIDENCESRN Event Rate

0.8 – 5 events/year/22.5kton (SK)35 – 220 events/year/1Mton (HK)Coutesy of K. Inoue & M. Sakuda

Relic Supernova Neutrino(RSN) Spectrum
SAKUDA, Makoto : Mega-ton, Gd-loaded Water Cherenkov Detector at Super-K
Setting MC=(16.5-18.0) M to solve SN RATEPROBLEM and RSG PROBLEM simultaneously.

Hidaka, Kajino, Mathews, ApJ (2016),
submitted.

Normal Hierarchy

RSNs could be a good probe to test EOS and Mass Hierarchy!
MSW-HD Res. ＋ (Lne = Lne >> Ln m,t )Shen’s EOS ; D=1.5s

Reactor n’s

Inverted Hierarchy

Shen’s EOS ; D=1.5s

LS’s EOS ; D=0.5s

LS’s EOS ; D=0.5s
Atmospheric n’s

8n-Oscillation and Nucleosynthesis
p1 ne

p2 n ene ne

8ne neMSW Matter Effect:
p2 n x

p1 nx

n-Collective Oscillation

nmt

neNSThrough high-density resonanceat r ~ 103 g/cm3

nmt

ne Vacuum Oscillation

SiLayerR-process:Heavy Nuclei
np-process:
92Mo, 96Ru ?
Explo. Si-burn.: Fe-Co-Ni,60Co, 55Mn, 51V …

xelectrons

n-Detection
n-process:
6,7Li, 9Be, 10,11B …

n-process
92Nb, 98Tc, 180Ta, 138La …
c.f. SIEVERDING, Andre & WU, Meng-ru

Proto Neutron Star

Calculated n Flavor Oscillation
Energy spectra SWAP!

Pure nene

Sasaki, Kajino, Balantelin & Phelivan (2016)

nePure nmt

ne30 MeV

ne

Energy spectral swapping
occurs around 8 MeV!

Synchronizedoscillation

nmt

5 MeV

Bipolar oscillation

15 MeVnmt

Mean Field Approx. (single angle, 2 flavor) loses many symmetries!

★ Quest for solving many-body Hamiltonian EXACTLY !
Y. Pehlivan, A.B. Balantekin, T. Yoshida & T. Kajino, Phys. Rev. D84 (2011), 065008,
Y. Pehlivan, A.B. Balantekin & T. Kajino, Phys. Rev. D90 (2014), 065011.

How to predict Split Energy ES ?
Single angle approx. (Inverted)“INVARIANCE”

Swapped !

Hnn = Many-body Hamiltonian: similar to BCS or Spin-Lattice: holds the same “Symmetries”

Bethe ansatz (Homogenous matter)

ESMHD-Jet SN
235U

Proton Number Z

208Pb

184

Au56Fe

126
8250
20 28

Neutron Number N

Astrophysical site for the r-process ?
Core-Collapse Supernovae?
n-DW ?
MHD-JetLong-GRB

Binary Neutron-Star Mergers?

Woosley, et al., ApJ 433, 229 (1994). +Nishimura, et al., ApJ 642, 410 (2006).
Fujimoto, et al., ApJ 680, 1350 (2008).
Winteler, et al., ApJ 750, L22 (2012).
Nishimura et al., ApJ, 810, 109 (2015）.
Nakamura, et al, A&Ap 582 A34 (2015)

Goriely, et al., ApJ 738, L32 (2011).
Korobkin, et al., MNRAS 426, 1940 (2012).
Rosswog, et al., MNRAS 430, 2585 (2013).
Goriely, et al., PRL 111, 242502 (2013), (2015).
Piran, et al., MNRAS 430, 2121 (2013).
Wanajo, et al., ApJ 789, L39 (2014).

R-process cond. of high S/k & low Ye?
t =1-10My

Binary NSs arrive too late ?

Explosion Mechanism ?

Time Scale Problem ?

νννTakiwaki, Kotake, Suwa, ApJ 786 (2014), 83.

100My ≤tc ≤ 10TyννCredit-NASA

GW from Binary BH Merger is most likely
detected in 2015-16 !
A. Einstein predicted 100 yrs ago.

Black Hole Binaryat d=1.3 Gly(Horizon～47.0 Gly)Photon last scatter
4x105 year

Accelerating expansion
Due to Dark Energy

Dark AgeInflation

47.0 Gly

1.3 Gly
13.8 Gy
Quantumfluctuation

WMAP

1st star
4 million year
Birth of galaxies & stars

Time Scale Problem

Coalescence tc DELAY for too slow GW rad. !

Neutron Star Mergers (Theory)tc = 100 My

Extremely Metal-PoorStars (obs.)[Ba_r/Fe]Argast, Samland,
Thielemann & Qian,
A&A 416 (2004),
997.

Sun (obs.)

Dispersion Problem
BH Merger
at d=1.3 Gly

10 [Fe/H] = time/10Gy－4－3－2－10[Fe/H] ＝ log(NFe/NH) ー log(NFe/NH)

10My100My

After BB/Galaxy formed:

time ＝ 1My・・・

10Gy

Time Scale Problem

Coalescence tc DELAY for too slow GW rad. !

Lorimer, Living Rev. Rel. 11(2008), 80.8
0.6
0.4x

0.2
0.0

Orbital eccentricity

tc

Wanderman and Piran(2014), arXiv:1405.5878

tC = 4Gy
110100My 10Gy

100

10Ty

1000

Orbital period (hours)

SUPERCOMPUTING of Galactic Chemo-Dynamical
Evolution of Dwarf Spheroidal
N-Body/SPH Simulation of DM+GAS+Star Particles with GAS MIXING in star forming region.
SNe = Metals ; NSM(tc=100My)= r-process elements.

SPH code = ASURA (Saitoh et al., PASJ 60 (2008), 667; PASJ 61 (2009), 481)

Hirai et al., (COSNAP group), ApJ 814 (2015), 41.

Mtot = 7x108Msun, Ni = 5x105 particles, M★ = 100Msun
Gas Particles

Star Particles

SUPERCOMPUTING of Galactic Chemo-DynamicalEvolution of Dwarf Spheroidal
N-Body/SPH Simulation of DM+GAS+Star Particles with GAS MIXING in star forming region.
SNe = Metals ; NSM(tc=100My)= r-process elements.

Argast, Samland, Thielemann,Qian, A&A 416 (2004), 997.

Hirai, Ishimaru, Saitoh, Fujii, Hidaka
and Kajino, ApJ 814 (2015), 41.

Without GAS MIXINGWith GAS MIXING

tc = 100My

tc = 100My

NSMs have arrived
too late !

Universality

Dispersion Problem[Fe/H]Sun(obs.)

Galactic Time

SNe !

[Fe/H]

Galactic Time

Universality in Ultra-Faint Dwarf Galaxy, Ret. II
Alexander P. Ji, Anna Frebel, Anirudh Chiti, Joshua D. Simon, Nature 531 (2016), 610

UFDG Ret II

Universality
R-Process site:
SN (MHD-Jet) or NS-Merger ?
1. Event Rate ?
(2.6 +/- 0.2)x103 M~10 SNe[Eu/Fe]less than 0.01~0.28 NSM !
SN ? NSM ?

2. UFDG, very old with [Fe/H] = -3 ?
SN !

NSM ?

3. Ejecta stops in shallow grav. pot ?
SN !

[Fe/H]

NSM ?

10-2

10-3
NSM R-Process cal.:S. Wanajo et al.,ApJ. 789 (2014), L39.

10-4
10-5

No Production ofLight Elements A < 50!

10-6
10-7
10-8
050

100
150
Mass Number A

4. Extended
200
250 Universality ?
SN !

NSM ?

Ian U. Roederer et al., ApJ. 151 (2016), 82.

Extended Universality, found in
C Mg Ca ---Fe Ni Zn --- R-elements

Element (Z)Dispersion due to Turbulent Mixing
in individual SN Ejecta
Sr (weak-r) production region

Dependence of the r-element dispersion
on EOS in Metal-Poor Halo Stars

Ba (main-r) production region

Famaiano, Kajino, Aoki and Suda,
ApJ (2016), submitted.

EOS

Turbulent Mixing & Ejection
from Shallow Layer

Turbulent Mixing & Ejection
from Deep Layer

Solar System r-Process Abundance

Today !

Shibagaki, Kajino, Chiba, Mathews, Nishimura & Lorusso (2016), ApJ 816, 79.

n-Driven
Wind SN

Neutron Star Mergers

total SUM =n-DW(80%)+ MHDJet(15%)+ NSM(5%)

Magneto-Hydrodynam.
Jet Supernovae

Shibagaki, Kajino, Chiba, Mathews, Nishimura & Lorusso(2015), ), ApJ 816, 79. COSNAP + RIKEN Collab.

125,126,128,130Te

EMPs in the Early
Galaxy !

Without NSM

Only MHD-Jet SNe can satisfy UNIVERSALITY !

Astron. obs. cannot separate isotopes !

Atomic Number Z

ELEMENTAL !

Universality is in

Proton number (Z)ELEMENTAL (Z) Abundance

128Te

Z=50

128Pd

N=82

Neutron number (N)Relative Contributions (n-SNe : MHD Jets : NSMs) fromObserved Galactic event rates !

Ejected Mass [Msun] x Event Rate [/Galaxy/Century]nSN (Weak r) =7.4 x 10-4x(1.9±1.1) ax ((0.03±0.02) x (1.9±1.1)) b
Binary NSMs = (2±1) x 10-2 x (1-28)x10-3 c
MHD Jet SNe =0.6 x 10-2

Observations

a 1.9±1.1

Obs. Estimate

b 0.03±0.02 Winteler, et al., ApJ 750, L22 (2012).
c (1-28) x 10-3 Kalogera, et al., ApJ 614, L137 (2004).

Diehl, et al., Nature 439, 45 (2006).

NumberAstron. Observation, desirable !
SNefrom the early Galaxy- 4.0- 3.0

Binary Neutron-Star Mergers
in recent epoch- 2.0- 1.00.0[Fe/H] & time

SUMMARY
Relic Supernova Neutrinos- Failed-SNe can solve both SN RATE & RSG PROBLEMS simultaneously.

- RSN-n detection would indicate EOS of neutron stars n-MASS HIERARCHY.

Origin of R-Process Elements- Core-collapse (MHD Jet) SNe satisfy UNIVERSALITY from the early Galaxy.
- Time-Scale Problem:
Binary NSMs have arrived later at 100My < tc and the solar-system abundanceconsists of both SN & NSM r-process elements.

- Dispersion Problem:
Abundance Scatter/Dispersion arises from 1) Galactic stellar inhomogeneity forboth SNe and NSMs and 2) Turbulent Mixing in SN Ejecta.