Hirschegg 2017 “Neutron Star Mergers”

GCD-Evolution & the Originof R-Process Elements
Taka KAJINO
National Astronomical Observatory of JapanThe University of Tokyo
Beihang University, Int. Cent. Big-Bang Cosmology & Element Genesis

Last Photon Scatt.
3.8x105 y

Cosmic Evolution
Binary BH Merger

Dark Age

InflationGal. Evolution & Sites of R-Elements?
GW150914
13.8 Gy

1.3 Gly

Supernova

Quantum
Fluct. ofSpace-Time
Binary NS Merger

Galaxy formed in 0.1Gy,
then First Star formed in a few My.
Galactic Chemo-Dynamical Evolution

Purpose
How to identify Astro. Sites for R-Elements, SNe or NSMs.

Contribution(Solar Masses / Century)[１] Time-Scale Problem of NSMs in Galactic Chemical Evolution⇒ Galactic Chemo-Dynamical Evolution

Supernovae (n-Wind, MHDJ)
Solar-System AbundanceBinary Neutron Star Mergers

Early Galaxy
Cosmic Time[２]R-Process Abundances of EMP☆ and S.S. ⇒ UNIVERSALITY― Nuclear Physics― Astron. Obs. of EMP☆ + Cosmochem. Analys. of Pre-Solar Grains[３]n-Matter Interactions in Explosion Dynamics and Flavor Oscillation

Binary Neutron-Star Mergers
Lattimer & Schramm, ApJ 192, L145 (1974),

Goriely, et al., ApJ 738, L32 (2011),Korobkin, et al., MNRAS 426, 1940 (2012),

Bauswein, Goriely, & Janka, ApJ 773, 78 (2013),
Rosswog, et al., MNRAS 430, 2585 (2013),

Bauswein, et al., ApJ 773, 78 (2013),
Credit-NASA

Goriely, et al., PRL 111, 242502 (2013, 2015),

Piran, et al., MNRAS 430, 2121 (2013),

νWanajo, et al., ApJ 789, L39 (2014), ++Time Scale Problem ?
100My ≤tc ≤ 10Ty

Binary NS Mergers have arrived too late in cosmic history !

Gal. Chem. Evolution (not Dynamical Simul.)
Argast, et al., A&A 416 (2004), 997,
Wehmeyer et al., MNRAS, 452 (2015), 1970.

tc = 100 My

Time Scale Problem

Merging, too slow for GW rad.: 100My<tCtc

Merger R-Process (Theory)

xLorimer, Living Rev. Rel. 11(2008), 8

Orbital eccentricity[Ba_r/Fe]

0.8
0.6Sun(obs.)

EMP Stars

0.4
0.2
0.0－4

tlife (10-30M )1My－3－2[Fe/H]

10My 100My－10・・・ 10Gy

1

101001000
Orbital period (hours)

100My 10Gy

10Ty

Large Scale Structure Formation ― Hierarchical
N-Body Simulation

X. Zhao & G. Mathews (2014)

400y (kpc)

2000Mixing of r-elements between Neighboring UFDGs is limited-200[Fe/H] < -3.5 and only fractional 0.001-0.1%.
toKomiya & Shigeyama, ApJ 830, 10 (2016).
-400-400-2000200400x (kpc)SUPERCOMPUTING of Galactic Chemo-Dynamical Evolution
Dwarf Galaxies = Building Blocks of Milky Way Galaxy
N-Body/SPH Simulation of DM+GAS+Star Particles with GAS MIXING in star forming region.
SNe = Metals ; NSM(tC=100My)= r-process elements. (nH >100 cm-3 → ～10-100pc)
SPH code = ASURA (Saitoh et al., PASJ 60 (2008), 667; PASJ 61 (2009), 481)

Yutaka Hirai et al., ApJ 814 (2015), 41 & MNRAS (2017), in press.
Mtot = 7x108Msun, Ni = 5x105 particles, M★ = 100Msun
Star Particles

y [kpc]y [kpc]Gas Particles

x [kpc]x [kpc]Galactic Chemo-Dynamical (N-Body/SPH) Simulation
No need of introducing artificial parameters!
Hirai, Ishimaru, Saitoh, Fujii, Hidaka & Kajino, ApJ 814 (2016), 41; MNRAS (2017), in press.
Time-scale for STAR FORMATION ～ 1-2Gy(1000My)
Binary NSMs (100My<tC)can contribute from the epoch of INHOMOGENEOUS mixing !

Star Formation HistorySculptor

Time [Gy]Sculptor[Fe/H]

SUPERCOMPUTING of Galactic Chemo-Dynamical Evolution ofDwarf Galaxies
N-Body/SPH Simulation of DM+GAS+Star Particles with GAS MIXING in star forming region.
SNe = Metals ; NSM(tc=100My)= r-process elements. (nH >100 cm-3 → ～10-100pc)

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

Hirai, Ishimaru, Saitoh, Fujii, Hidaka and Kajino,
ApJ 814 (2015), 41; MNRAS (2017) in press.

Without GAS MIXINGWith GAS MIXING

tc = 100My

tc = 100My

NSM(r)SN II+SN Ia(Fe)Sun(obs.)Sun(obs.)

NSMs have arrived
still too late !

SNe[Fe/H]

Galactic Time

[Fe/H]

Galactic Time

Core-Collapse Supernovae
n-Driven Winds ⇒ Up to 1st R-Peak
Meyer, et al., ApJ, 399, 656 (1992),
Woosley, et al., ApJ 433, 229 (1994),
Qian & Woosley, ApJ, 471, 331 (1996),
Witti, et al., A&A, 286, 842 (1994),
Otsuki, Kajino, et al., ApJ 533, 424 (2000) ++Long-GRBs (Collapsar) ⇒ Peculiar R-Pattern
Credit Takiwaki (NAOJ)

νNakamura, Kajino, et al., A&A 584, A34 (2015).

MHD-JetNishimura, et al., ApJ 642, 410 (2006),
Fujimoto, et al., ApJ 680, 1350 (2008),
Winteler, et al., ApJ 750, L22 (2012),
Nishimura, Kajino, et al., ApJ, 810, 109 (2015) ++Explosion Condition, still unclear?
t =1-10My
Underproduction, off R-Peaks ?

MHD-Jet SN
235U

Proton Number Z

208Pb

184

56Fe

126
8250
20 28

Neutron Number N

UNIVERSALITY !

Early Galaxy !

Roederer et al., ApJ 747 (2012) L8.

Te(52)
Sn(50)

Without NSM

Nd(60)

UNIVERSALITY is explained by ONLY SN-MHD Jet !

Astron. Obs. Doesn’t separate ISOTOPES !

Atomic Number Z

ELEMENTAL (Z)Early Galaxy !

●Solar System r-Process AbundanceTe(52)
Nd(60)
Sn(50)

n-Driven
Wind SN

Magneto-Hydrodynam.
Jet Supernovae

Lorusso, Nishimura, Kajino et al. (2015),
PRL 114, 192501.

128,130Te(r)Sn(50)

Nd(60)

Many contributors

134 InLess abundant46

We don’t carein Elemental !

Abundant
128Pd

CCSN: Magneto-Hydrodynamic Jets
S. Nishimura, et al., ApJ , 642, 410 (2006) ; T. Takiwaki, K.Kotake and K. Sato, ApJ 691,1360 (2009); C. Winteler, et al., ApJ 750, L22 (2012).
FRDM

ETFSI model (Extended ThomasFermi + Strutinsky; Goriely 2003)

Mass A

Underproduction
PROBLEM !

Nucl. Phys. - Shell Quenching ?
orPossible Solutions
Another Site (NSM) !
S.S. abundance has no Time-Scale Problem.

RIKEN-RIBF : Decay Spectroscopy around A = 100-145
G. Lorusso et al., PRL 114 (2015), 192501.

A.Jungclaus, PRL99, (2007)

H. Watanabe et al., PRL111 (2013)

No clear evidence forshell quenching on N=82!
130Cd

130Cd

No clear evidence
for shell quenching on N=82 !
128Pd

128Pd is the progenitor parent of

the 2nd r-peak element 128Te
128Pd

126Pd82
126Pd (N=80)

128Pd (N=82)

82

MHD-Jet SNe vs. Binary Neutron Star Mergers
236U & others◎ Fission Recycling could operate!

Theory vs. Exp.

Fission Fragment Mass Distribution
M. Ohta et al., Proc. Int. Conf. on NDST, Nice, France, (2007)
S. Chiba et al., AIP Conf. Proc. 1016, 162 (2008).
Fission Region

Fission fragment mass A

Bimordial or Trimodal FFD:

MHD-Jet SNe &CC Supernovae

Neutron Star Mergers◎ Neutron capture (n,g) plays impotant roles !

Fluid-Dynamical Model for Neutron Star Merger
Binary Neutron Star Merger
Korobkin et al., MNRAS 426 (2012), 1940; Rosswog et al., MNRAS 430 (2013), 2585.

SPH Simulation: (Adiabatic Expansion)
Newtonian gravity, Neutrino Leakage scheme

Entropy, Ye, T, r Evolution: (Fission is a strong heat-source: S ～ q/T)

FissionRegionMass fraction

We solved thermodynamic evolution of each trajectory from the initial conditions.

Ye～0.03
Extremelyn-rich!

YeSolar System r-Process Abundance

Present t = 13.8Gy

Shibagaki, Kajino, Chiba, Mathews, Nishimura & Lorusso (2016), ApJ 816, 79.
●Solar System r-Process Abundance

Neutron Star Mergers(0.1 Gy = 100 My < t)n-Driven
Wind SN
Asymmetric Fission Recycling

Magneto-Hydrodynam.
Jet Supernovae
ISOTOPIC-MASS (A)Observed Galactic event rates !
Ejected Mass [Msun] x Event Rate [/Galaxy/Century]nSN (Weak r) =7.4 x 10-4x

MHD Jet SNe =0.6 x 10-2x ((0.03±0.02) x (1.9±1.1)) b

Binary NSMs

= (2±1) x 10-2 x

Observations

a 1.9±1.1(1.9±1.1) a(1-28)x10-3 cDiehl, et al., Nature 439, 45 (2006).

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

Galactic Evolution including Binary Evolution
Kajino, Mathews et al. (2017)

Strong Universality in Ultra-Faint Dwarf Ret. II
Ian U. Roederer et al., ApJ. 151 (2016), 82.
Alexander P. Ji, Anna Frebel, Anirudh Chiti, Joshua D. Simon, Nature 531 (2016), 610

UFDG Ret II

WhichStrong
is likely
r-process site,
Universality
MHD-Jet SN or Binary NSM?
Product. Yield ~ 10-2 M /event

1. Event Rate, too small?

(2.6 +/- 0.2)x103M[Eu/Fe]~10 SNe

Ret. II baryon mass
IMF~(0.01-0.3)x10 NSM/SN (0.1%)
MHDJ/SN (1-3%)
SN !
NSM !
2. Very old ?
SN !
NSM !
3. Extended Universality ?
Dust forms ?
SN !
NSM ?
4. Ejecta escape from shallow pot. ?
SN !
NSM ?
[Fe/H]

Ret. II should be very old !
INTEGRAL Mission (g-Ray Satellite) detects 511 keV Emission Line.
■ Does e+- come from DM-annihilation or Stellar Activity ?

Exposure map■ No significant detection except for Reticulum II⇒ e+- from recent stellar activity !
Courtesy from Roland Diehl:
Siergert et al., A&A(2016), submitted.

Ret. II

Micro-quasar !
links toMHDJ-SN or NSM ??

Extended Universality
Ultra-Faint warf Galaxy: Ret. II
Astron. Observation
Ian U. Roederer et al., ApJ. 151 (2016), 82.
Carbon Silicon
Wanajo et al., ApJ. 789 (2014), L39.
Shibagaki et al., ApJ. 816 (2016), 79; (2017)

Element (Z)
10-2

Goriely, et al., ApJ 738, L32(2011); Korobkin, et al.,MNRAS 426, 1940 (2012);
Bauswein, et al., ApJ 773, 78(2013); Rosswog, et al.,MNRAS 430, 2585 (2013);
Goriely, et al., PRL 111, 242502(2013), (2015): Piran, et al.,MNRAS 430, 2121 (2013).

Theor. Calculation

10-3
10-4
10-5

10-6

NSM cannot produce enough A < 50 !

10-710-8050

100
150
Mass Number A

200250Another DIFFICULTY for R-Process in Binary NSMs
Macronova (Kilonova)
Tanvir, Levan, Fruchter, et al., Nature 500, 547 (2013)

Dust is hard to form for deficient Carbon
and other lighter elements.
Figure 1 HST imaging of the location of SGRB 130603B. The host is well resolved

Takami, Nozawa & Ioka, ApJ 786, L5 (2014).

and displays a disturbed, late-type morphology. The position (coordinates RAJ2000 = 11
28 48.16, DecJ2000 = +17 04 18.2) at which the SGRB occurred (determined fromground-based imaging) is marked as a red circle, lying slightly off a tidally distorted
spiral arm. The left-hand panel shows the host and surrounding field from the higher
resolution optical image. The next panels show in sequence the first epoch and second
epoch imaging, and difference (upper row F606W/optical and lower row F160W/nIR).
The difference images have been smoothed with a Gaussian of width similar to the psf,
to enhance any point-source emission. Although the resolution of the nIR image isinferior to the optical, we clearly detect a transient point source, which is absent in theoptical.

Figure 2 Optical, near infrared (left axis) and X-ray (right axis) light curves ofSGRB 130603B. Upper limits are 2s and error bars 1s. The optical data (gri bands)

Dust formation becomes even more difficult when one includes
epoch 1 points are bold symbols. The optical afterglow decays
steeply afterthe firstmore
complete
opacity table for heavy actinide elements.
have been interpolated to the F606W band and the nIR data to the F160W band using anaverage spectral energy distribution at »0.6 days (see Supplementary Information). HST»0.3 days, and is modelled here as a smoothly broken power-law (dashed blue line). We
note that the complete absence of late-time optical emission also places a limit on any

Milky Way Halo Stars[Eu/Fe]>1

EXTENDED UNIVERSALITY
Honda, Aoki, Kajino, Beers, et al.,(SUBARU-HDS Collaboration),
ApJ 607 (2004), 474; ApJS 152 (2004) 113.
Extended UniversalityCarbonSilicon

Strong Universality

EuTh/EuBlue symbols: [Eu/Fe]>1Error bars cover Th detected starsTh

QUEST for Cosmo-Chemistry and Astronomy:
to find/confirm “EXTENDED UNIVERSALITY”◎ Supernova Grains e.g. Murchison Meteorite Courtesy of S. Amari
SiC X-grains- Enhanced 12C (12C/13C > Solar), Enhanced 28Si
- Deficient 14N (14N/15N < Solar)- Decay of 26Al (t1/2=7x105yr), 44Ti (t1/2=60yr)

Pre-solar X-grains condense and form in SN/NSM ejecta.

■ If SiC X-grain incl. much r-elements
NSM ? SN !
■ If extended Universality manifests in [r/C-Si-Fe]= 0SN !
■ If diversity in [r/C-Si-Fe]exists
SN !

◎ Spectr. Astron. Obs.
Direct detection ofC, Si & r-elements
simultaneously !

EMP

SN+indirect

SN-remnant

SUMMARY★ TIME-SCALE PROBLEM of NSMs remains.
Galactic Chemo-Dynamical Evolution can PARTIALLY resolve this problem.
★ UNIVERSALITY in EMP☆ is satisfied only by SNe(nDW+MHDJ).
★ S.S. r-elements need both SNe and NSMs.

Evolution of ISOTOPIC Abundances takes the key !
Pre-solar X-Grains (SiC+r nuclei) should be an evidence !

⇒ Quest for Astronomy, Astrophysics and Cosmology⇒ Quest for Nuclear Physics

SYNERGY among Astronomy, Cosmochemistry

and Nuclear Physics is highly desirable !