第1回 NOP/Φ研/KMI分野横断セミナー
2014年5月26日（月）、名古屋大学 ES総合館

超新星元素合成とニュートリノ振動の物理
梶野 敏貴 （Taka KAJINO）
National Astronomical Observatory
Department of Astronomy, The University of Tokyo

Challenge of the Century
Universal expansion is most likely accelerating and flat !
WB + WCDM + WL = 1
CMB – Planck 2013

- What is CDM (WCDM = 0.27) and DE (WL = 0.68) ?
CMB including n-mass- Is BARYON sector (WB = 0.05) well understood ?
SN Ia magnitude-redshift relation
1998

Big-Bang Nucleosynthesis
with Axions + SUSY to solve DM & Li Problems:
SUSY-DM ⇒ “beyond the Standard Model”⇒ mn ＝ 0 is the unique signal !

Key Particles

Neutrons (n’s) & Neutrinos (n’s).

Big-Bang Nucleosynthesis is now a Precise Science ～1%
Smith, Kawano & Malaney, ApJ S85(2003) 219;

Mathews, Kajino & Shima, PRD71 (2005) 21302 (R).

Neutron Life

New UCN Experiment
Serevlov et al., PL B605 (2005), 72.

4He

dtn/tn = -0.01

1% decrease!

7Li PROBLEM

by at least factor 3 !

Kirkman et al., ApJ S149 (2003) 1.

CKM
MatrixVud

CMB - WMAP

b-decay asym.

Cosmological Implication for 4He-6Li-7Li PROBLEM
New measurements using
Inverse-Compton g-rays !
Shima et al. PR C72 (2005) 44004
Naito et al. PR C73 (2006) 34003+ New Experiment (2008 ―)
4He(g

3
4
6
NT,n) He( He,p) Li

4He(g

3
4
6
NT,p) H( He,n) Li

Decaying DM (i.e. SUSY) BBN for
solving 6Li problem:
Kusakabe Kajino, Shima et al.,
PR D79 (2009) 123513.

Supernova n-Process-2.0
4He(n, n’), 4He(n , e- ), 4He(n , e+)eeKusakabe, Kajino, Yoshida, Shima, Nagai, and Kii (2007-2014).

Excluded by
Cosmic Background Radiation

Allowed by
All Light Elements D, 3Li , 4Li , 6Li , and 7Lid

BBN Constraint on Magnetic Moment of Massive Neutrinos
M. Kusakabe, A. B. Balantekin, T. Kajino & Y. Pehlivan, PR D87 (2013), 085045.

Cosmological:

nn’ + g non-therm

shorter t X

sterile (mn=0, mn=0) sterile/active

Current Constraints
Laboratory:
Astrophysical:
Magnetic Moment of massive neutrino X

10-17mB < mn < 10-12mB

Decoupling Temp. is Max[1MeV, mX/20]

shorter t X

What happens as neutrinos
flow through the SN outer layers ?
Neutrino induced nucleosynthesis toconstrain n-mass hierarchy.
Astrophysical sites for r-process including
SNe, GRBs and neutron star mergers..
Pulsar kick from n–baryon int. inmagnetized neutron stars.
Origin of life – chirality of amino acids.

What happens to neutrinos
once they leave the supernova?
Supernova Relic Neutrinos (SRNs) toprobe EoS of proto-neutron stars.

What happens as neutrinos
flow through the SN outer layers ?
Pulsar Kick from n–baryon int. in Magnetized
Neutron Star.

n–induced nucleosynthesis and Mass Hierarchy.
R-process nucleosynthesis in GRBs.

ν
ν

ν

ν
ν

Mass Hierarchy?

Δm212 = 7.9×10-5 eV2
2

-3

2

|Δm 23| = 2.4×10 eV= (0.05 eV)2

Normal:S mn ～ 0.05 eV !
Inverted:
S mn ～ 0.1 eV !

Total n-Mass, constrained from Nuclear Physics
and Cosmology● 0nbb in COUORE, NEMO3, EXO, KamLAND Zen< 0.05 eV→(→
0.05～0.1
eVin
inthe
thefuture)
future|∑U2ebmb | < 0.3 eV: COUORE, NEMO3, EXO, KamLAND Zen (2012)
Strongly constrains mass hierarchy!

● CMB Anisotropies + LSS→ 0.1 eV in the future

Neutrinoless bb∑ mn < 0.36 eV (95%C.L.): WMAP-7yr + HST + CMASS (Putter et al. arXiv:1201.1909)
CMB Anisotropies & Polarization including Cosmic Magnetic Field∑ mn < 0.2 eV (2s, Bl<2nG): with Magnetic Field; Ymazaki, Kajino, Mathews & Ichiki, Phys. Rep. 517(2012), 141; Phys. Rev. D81 (2010), 103519.

www.esa.int/Our_Activities/Space_Science/
Planck/Planck_reveals_an_almost_perfect_
Universe10mn ＝ 0 is the unique SIGNAL indicating a Modelbeyond the Standard Model !

Higgs(standard model)
produces Quark Masses.

Key Cosmology = beyond the standard model
What is Dark Matter, axion or SUSY ?
WB + WCDM + WL = 1 ?
Why is cosmic expansion accelerating ?

10-10

Why 10-10 ?

nm

nt

?

ν-Masses require a theory
beyond the standard model !

Generation

Key Physics = beyond the standard model
Unification of elementary forces ?
CP violation and Lepto- & Baryo-genesis ?

Why left-handed neutrinos, Majorana or Dirac ?
Explosion Mechanism of Supernovae ?

The “KNOWN” in Neutrino Oscillations
KAMIOKANDE, SK, KamLand (reactor ν), SNO determined⊿m122 and θ12 uniquely: SK (atmospheric ν) determined⊿m232 and θ23 uniquely.

23－mixing
sin22q23 = 1.0|Δm223| = 2.4×10-3 eV2
12－mixing
Cabibbo angle
sin22q12 = 0.816 (q12+qC=p/2)2-52
Δm 12 = 7.9×10 eV“4 UNKNOWN”
1

2

3

4

13-mixing, hierarchy, dCP, mass

● sin22q13 = 0.1±0.02
T2K, MINOS, RENO, Daya Bay, Double Chooz?

● ⊿m132 = ±2.4x10-3 eV2● δ＝CP violation phase● Absolute Mass
0nbb, cosmology
E(nm)=E(nt): Yokomakura et al., PLB544, 286.

Various Neutrino-Sources in Nature/Culture
1.9K

CMB
atmospheric neutrino

Cosmic Background

Neutrino Cosmology
verificationof particle modelne

ne, nm, nt

ne, nm, nt

ne or ne nm ne nm
Direct signal of
SN neutrinos in SN1987A
Kamiokande, IMB, Gdand Sassonene, nm, nt

ne, nm, nt

Event of the Century!

SN Neutrino Spectra
are unknown !
By courtesy of K. Inoue

T(ne), T(ne), T(nx) ?

Electron-capture SN
Normal CC-SNe(Faint SnNe)(Neutron Star fromation)

Failed Sne(Black Hole formation)

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

4.0

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

Solar System Abundance

Number Abundance (Si = 106）

Big-Bang Nucleosynthesis
Stellar Fusion

1,2H, 3,4He, 6,7Li, etc.

12C…56Fe-58Ni, etc.

(r-nuclei)(s-nuclei)

Core-Collapse SNe & AGB: 56Fe < A
Iron peak

Supernova n-processr-nuclei
232Th (14.05Gy)

7Li, 11B

p-nuclei
92Nb 98Tc

Cosmic Ray Spallation
Li-Be-B, F, Na, etc.

238U (4.47 Gy)

np-nuclei

138La

Mass Number A

180Ta

8
Various roles of n’s in SN-nucleosynthesis
8

MSW Matter Effect:
Through high-density resonanceat r ~ 103 g/cm3

n-Collective Oscillation
NS

nmt

ne

Si
Layer

R-process:Heavy Nuclei
np-process:
92Mo, 96Ru ?

Explo. Si-burn.
Fe-Co-Ni,
60Co, 55Mn, 51V …

n-process180Ta, 138La, 92Nb, 98Tc …

n-process:
6,7Li, 9Be, 10,11B …

92Nb also has SN-n Origin !
Hayakawa et al., ApJ 778 (2013) L1.
92Nb(

t

1/2=3.47x10

7 y):

Unique Chronometer of SN n-Process

Isotopic anomaly in meteoritic 92Zr/93Nb:
Δ = 1x106―3x107 y

Tne = Tne = 4 MeVTime duration after the last nearby Supernova to
the Solar-System (protosolar cloud) formation

92 Zr

96Mo

93 Nb

92 Nb

Tantalum（180,181Ta）
181Ta （stable）, 180Ta (unstable, t
180Tam（isomer, t
15gg
1/2 = 8h）,
1/2 > 10 y)

The rarest isotope on the Earth & Universe !

Origin of 180Ta was unknown since 1957.
S-process cannot explain both 180Ta & 138La !
SN n-process for overproduced 180Ta/138La ?

Solved by
Tne = 3.2 MeV,
Tne = 4 MeV !

We solved dynamical “explosive SN-nucleosynthesis” coupled with“quantum transitions” simultaneously.

p process(Hayakawa,
et al. 2010, PR C81, 052801®;
PR C82, 058801)

Burbidge2-Fowler-Hoyle, Rev. Mod. Phys.
29 (1957), 547-650.
“Element Genesis”

Neutral current
SN n-process(ne)r processW. Fowler
F. Hoyle
M. Burbidge
J. Burbidge

Galactic Chemical Evolution of 9Be & 10,11B
Livermore Model

Tnm,t = 8 MeV
Woosley -Weaver 1995, ApJS 101, 181.

s ∝ En2

Tnm,t = 6 MeV
Consistent with SN1987A
Yoshida, Kajino & Hartmann 2005,
PRL 94 (2005), 231101.

Consistent with SN1987A

Overproduction problem is resolved!

9Be:

16
17

－Galactic Cosmic Rays
OLD stars

SUN

10+11B + 11B:

－Galactic Cosmic Rays
－Supernova n-process
Yoshii, Kajino, Ryan, 1997, ApJ 486, 605.
Ryan, Kajino, Suzuki, 2001, ApJ549, 55.

SN1987A constraint
on En,tot & Grav. Energy

SN-Boron calculations andconstraints on SN- n
Woosley & Weaver
ApJS 101 (1995), 181.

Tn = 8 MeV

Yoshida, Kajino & Hartman,
Phys. Rev. Lett. 94 (2005),
231101.

Tn = 6 MeV

Consistent with SN
simulation (MPA
group) 2004-2013.

GCE constraints on 11B& meteoritic 11B/10B(n) / 

Mean n-temperatures are known!
・R-process Elements & 180Ta/138La

Tne = 3.2 MeV, Tne = 4 MeV

Tnm, = Tnt = 6 MeV・Astron. GCE of Light Elements & 11B

We can now study the “EOS”
and “Neutrino Oscillation” !

0.25

ne

0.2

T(ne) < T(ne) < T(nx)
3.2

0.15

4.0

6.0
MeV

ne

0.1

nm,t ,nm,t

0.05
0

0

10

20

30

40

n (MeV)50

60

Temperature

Temperature Hierarchy of Supernova- n
Neutrino diffusion process
Tnm,nt > Tne > Tne

Dxn2 = 2Dntn
Dn = lnc/3
ln = (nT sn)-1

Weak interactions
ne + n → p + e- (CC)ne + p → n + e+ (CC)radiusni + p,n → p,n + ni (NC)0

Dxnm ,nt

Dxne Dxne(i = e, m, t)∴ lne < lne < lnm,nt~ 10 km

Proto-Neutron Star

∴ Dxne2 < Dxne2 < Dxnm,nt 2

Supernova n-Process; 7Li,11B,92Nb,138La,180Ta|Δm213| = |Δm223| = 2.4×10-3 eV2[]Shell Model:
Yoshida, Suzuki, Chiba, Kajino, et al., ApJ 686 (2008), 448:
Suzuki and Kajino, J. Phys. G40 (2013), 083101:
QRPA:
MSW
high-density
resonanceis
Cheoun, et al., PRC81 (2010),
028501;
PRC82 (2010),
035504;locatedthe bottom
J. Phys. G37 (2010), 055101;
PRC 83at(2011),
028801of He/C

shell at r ~ 103－104 g/cm3.

A=7

A = 11

nx→ne

nx→ne

Role of Nucl. Phys. for n-Nucleus X-Sections
New Shell Model cal. with NEW Hamiltonian: n -12C, 4He
Suzuki, Chiba, Yoshida, Kajino & Otsuka, PR C74 (2006), 034307.
Suzuki, Fujimoto & Otsuka, PR C67, 044302 (2003)
12C: New Hamiltonian = Spin-isospin flip int. withtensor force to explain neutron-rich exotic nuclei.

- m-moments of p-shell nuclei- GT strength for 12C12N, 14C14N, etc. (GT)- DAR (n,n’), (n,e-) cross sections

QRPA cal.: n -180Ta, 138La, 98Tc, 92Nb, 42Ca, 12C, 4He…
Cheoun, et al., PRC81 (2010), 028501; PRC82 (2010), 035504:
J. Phys. G37 (2010), 055101; PRC 83 (2011), 028801

181Ta(n, n n’)180Ta

GT

12C(n ,e-)12Ne

Spin-Mutipole
12C(n ,e-)12N(gs,1+)eGTSpin-Multipole

Double b decay - n mass - Astro-Cosmology Connection
K. Yako et al., PRL 103 (2009) 012503.

Experiment(RCNP, Osaka)

Shell model (theory)larger effect !

Yoshida, Kajino, Yokomakura, Kimura,Takamura & Hartmann,
PRL 96 (2006) 09110; ApJ 649 (2006), 349.

Tne < Tne < Tnmt, nmt

Normalsmaller effect !

H-Resonance

mn

L

L

NormalMass Hierarchy

Ne

Invertedmn

Inverted

10-6
NO 13-mixing

10-4

10-2

H-ResonanceNeBayesian Analysis, including astrophysicalmodel dependence on SN progenitor masses,

SN progenitor Massn-temps. ( Tne ,Tne ,Tnmt, nmt ) and nuclear input data.

aa(a,g)12C

12C(a,g)16O

Murchison Meteorite
SiC X-grains- 12C/13C > Solar- 14N/15N < Solar- Enhanced 28Si
- Decay of 26Al (t1/2=7x105yr), 44Ti (t1/2=60yr)

SiC X-grains are made of cc-SN Dust !
Fujiya, Hoppe and Ott (2011, ApJ 730, L7)
discovered 11B and 7Li isotopes in 13 SiC X-grains.

By courtesy of S. Amari

MSW Effect & n Mass Hierarchy
1Mathews, Kajino, Aoki
& Fujiya, PR D85,
105023 (2012);

Normal Mass
Hierarchy

0.9

Suzuki and Kajino,
J. Phys. G40 (2013),
083101

7Li/11B-Ratio

0.8
0.7
0.6
Inverted Mass
Hierarchy

0.5

First
of
LongDetection
BaselineExp.
7Li/11B in SN-grains
in 2011:

0.4

・T2K (Kamioka)“Inverted Mass Hierarchy”
2
2q13 = 0.1
・MINOSis statistically moresin
preferred!
74% ー Inverted
Reactor Exp. in2012:
24% ー Normal
W. Fujiya, P. Hoppe, &

0.3

0.2

・Double CHOOZ

U. Ott, ApJ 730, L7
・Daya Bay(2011).

0.1

・RENO (KOREA)

10-6

10-5

10-4

10-3

10-2

10-1

What happens as neutrinos
flow through the SN outer layers ?
Neutrino induced nucleosynthesis toconstrain n-mass hierarchy.
Astrophysical sites for r-process including
SNe, GRBs and neutron star mergers..
Pulsar kick from n–baryon int. inmagnetized neutron stars.
Origin of life – chirality of amino acids.

What happens to neutrinos
once they leave the supernova?
Supernova Relic Neutrinos (SRNs) toprobe EoS of proto-neutron stars.

A New Method to constrain EOS & n-Oscllation
G.J. Mathews, J. Hidaka, T. Kajino & J. Suzuki, ApJ (2014), submitted.

Supernova Rate Problem/Discrepancy
SFR of Massive Stars at birth
SNR: Supernova Explosions at death !

50% Massive Stars, missing !

Expected Reasons:Half was evolved into too dark SNe
to detect!

1. Failed SNe (<25M BH formation)
2. Faint ONeMg-SNe (8-10 M )or the mass function changed!

Fate of Massive Star

A. Heger et al. (2003)

metalicity

Solar
Metal

Metal
Poor
Stars

１０Mｓ

25Mｓ

40Mｓ

32

Initial Stellar MassElectron-capture SNe
Normal CC-SNe(Faint SnNe)(Neutron Star fromation)

Failed SNe(Black Hole formation)

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

4.0

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: Shen et al. Nucl. Phys. A637 (1998) 435.
* LS-EOS:
Lattimer & Swesty, Nucl. Phys. A535 (1991) 331.
ONeMg SNe: Hudepohl, et al., PRL 104 (2010).

GRBs: Nakamura, Kajino, Mathews, Sato & Harikae, Int. J. Mod. Phys. E 22 (2013)
1330022; Kajino, Mathews & Hayakawa, J. Phys. G41 (2014) 044007.

Spectrum of Relic Supernova Neutrinos(RSNs)
for Hyper-Kamiokande (Mega-ton): Water Cherenkov

n-spectrum at Various SNe & GRB

SN Rate x Volume101

No n-oscillation
100

10-1

Atmospheric-n

10-2

103

10-4

0

10

20

30
40
En (MeV)50

60

Spectrum of Relic Supernova Neutrinos(RSNs)
for Hyper-Kamiokande (Mega-ton): Water Cherenkov

Recent SNe
z = 0～1

Cosmologically Old SNez = 4～5

Relic Supernova Neutrinos
Hyper-Kamiokande (Mega-ton, 10y), Gd-loaded Water Cherenkov Detector
G. J. Mathews, J. Hidaka, T. Kajino, and J. Suzuki, ApJ(2014), in press.

SN rate problem is resolved byassuming 2 x failed SNe for BH
formation!

No n-Oscillation

Same assumption as Horiuchi, Beacom(2011)

SN rate problem still remains.
No n-Oscillation

LS-EOS

failed SNe(BH formation)
Shen-EOS
LS-EOS
Shen-EOS

Reactor-n BG

Atmospheric-n BG

ONeMg SNe

Relic Supernova Neutrinos(RSNs)
Hyper-Kamiokande (Mega-ton, 10y), Gd-loaded Water Cherenkov Detector
G. J. Mathews, J. Hidaka, T. Kajino, and J. Suzuki, ApJ(2014), in press.

Assuming 2 x failed SNe for BH formation!
Non-Adiabatic MSW Oscillation
failed SNe(LS-EOS)No Oscillation

Adiabatic MSW Oscillation
failed SNe(Shen-EOS)

ONeMg SNefailed SNe
LS-EOS(LS-EOS) failed SNe
failedSNe(BH formation)(Shen-EOS)
Shen-EOS

ONeMg SNe
ONeMg SNeWhat happens as neutrinos flow
through the SN outer layers ?
Pulsar Kick from n–baryon int. in Magnetized
Neutron Star.

n–induced nucleosynthesis and Mass Hierarchy.
R-process nucleosynthesis in GRBs.

ν
ν

ν

ν
ν

Supernova Nucleosynthesis Simulation
T. Kajino & S. Chiba

235U

Proton Number Z

208Pb

184
56Fe

126
82

50
20 28

Neutron Number N

R-process Nucleosynthesis
Otsuki, Tagoshi, Kajino and Wanajo, ApJ 533(2000),424; Wanajo, Kajino, Mathews and Otsuki, ApJ 554(2001),578.

Neutron-rich condition for successful r-process: 0.1 < Ye < 0.5
ne ＋ n → p + en e ＋ p → n + e+
Theoretical Challenge:1)Astrophysical Sites ?
・n-wind SNe・MHD jet SNe
・NS mergers(short GRB)・long GRBs

n = 3.15 Tn

Tne = 3.2 MeV, Tne = 4 MeV

Sr-Y-Zr
I-Xe
Theoretical model

Ir-Pt
Pb

2)Neutrino effects ?
Ye > 0.5 ?

-1

Dy-Er

Roberts, Reddy and Shen
(PR C86, 065803, 2012)

pointed out

Ye < 0.5 !
for nucleon potential
and Pauli blocking
effects.

Observed
Solar r-abundanceALighter Mass End(10-13 M)of n-Driven SNe;not enough neutrons for the heaviest r-process nuclides.
 Heavy Mass (15-25 M)CCSNe, wanted !?
Only weak r-process?

S. Wanajo, ApJL, L22 (2013)

Sr Y Zr
Te Ba
Eu

Pt

Alternative Models for the r-Process
Nishimura, Nishimura, Kajino & Mathews (2012)

Ejection of neutronizedcore material in MHD jet:Moderate entropy: S>15,
Neutron rich: Ye ~ 0.2.

Neutron star mergers:
Low Entropy S ~ 1,
Extremely neutron rich: Ye ~ 0.02.

:- can contribute to the s.s. andrecent generations of stars.
:- cannot contribute to theearly generations of stars.

Freiburghaus et al (1999), Korobkin et al. (2012),
Shibagaki, Kajino (2014)

Is there another possibility?
Yes!
R-Process nucleosynthesis in collapsar jets:
Surman et al. 2008, Fujimoto et al. 2008, Ono et al. 2012, Nakamura et al. 2013.

- Model for long duration gammaray bursts (GRB).
- A failed supernova.
- Produces a black hole and a hightemperature accretion disk.
- MHD + neutrino heating produces
an energetic jet.
However, no fully successful numerical hydrodynamic model !
Woosley 1999, McFadyan & Woosley 2003

→ Harikae et al. 2009 - 2014Collapsar Modelfor Long Gamma-Ray Bursts

Neutrino-Pair HeatingnnBlack HoleHarikae et al., ApJ 704 (2009), 354; 713 (2010) 304.
Nakamura, Kajino, Mathews, Sato & Harikae, IJMP 22(2013), 1330022.
Accretion Disk

Y [cm]

20,000 tracer particles

Stages of a Collapsar
1. Initial Collapse of 25-40 M progenitors.
2. Accretion disk heats up and a funnel region
above the black hole is heated by neutrino pairannihilation and magnetic fields.
3. Causes launch of a relativistic jet; G～5.

Modeling R-Process

1208 trajectories with positiveenergy to be ejected outside.

1. Extend the jet beyond the MHD+neutrino pairannihilation heating using 2D hydo.
2. Attach tracer particles to evolve the flow ofmaterial into the accretion disk and out into jet.

Evolution of low-Ye neutron-rich material
Nakamura, Kajino, Mathews, Sato & Harikae, Int. J. Mod. Phys. 22(2013), 1330022.

y [107 cm]

Ye
10.0

0.5

8.0

0.4

6.0

0.3

4.0

0.2

2.0

0.1

2.0

4.0
7

x [10 cm]

Neutronized accretiondisk material

2.0

4.0
7

x [10 cm]

2.0

4.0
7

x [10 cm]

Flows into the jet

Neutrino-Pair HeatingnBlack Hole

Accretion Diskn

Collapsar Modelfor Long Gamma-Ray Bursts
Harikae et al., ApJ 704 (2009), 354; 713 (2010) 304.
Nakamura, Kajino, Mathews, Sato & Harikae, IJMP 22(2013), 1330022.

R-Process Nucleosynthesis in Gamma-Ray Bursts
Nakamura, Kajino, Mathews, Sato & Harikae, IJMP 22(2013), 1330022.

What happens as neutrinos flow
through the SN outer layers ?
Pulsar Kick from n–baryon int. in Magnetized
Neutron Star.

n–induced nucleosynthesis and Mass Hierarchy.
R-process nucleosynthesis in GRBs.

ν
ν

ν

ν
ν

Estimating Pulsar Kick Velocities
of Proto-Neutron Star

CasA

A.G.Lyne, D.R.Lomier, Nature 369, 127 (94)

Kick Velocity:
Average … 400km/s，Highest … 1500km/s
99% of Explosion Energy ~ 1053 erg
http://chandra.harvard.edu/photo/is taken by Neutrinos!
2004/casa/casa_xray.jpg
Even 1% Asymmetry is sufficient to explain the Pulsar Kick.
Lai & Qian, Astrophys.J. 495 (1998) L103.

Relativistic Mean Field Theory:
Maruyama, Kajino, Cheoun et al., PR D83, 081303(R), (2011); D86, 123003 (2012).

Estimating Kick Velocity of PNS with T = 20 MeV and B = 2× 1017G
p
Poloidal Magnetic Field 2‐3% Asymmetry vkick  z  600 [km/s]
M

49

The Cross-Section of ν-B (Mg. Field) in Rel. MFT

Fermi
Distribution
Deformed Distribution

Perturbative
Treatmentσ  σ 0 + Δσ
Non-Magnetic PartΔσ  B
Magnetic Part50

EOS of Proto Neutron-Star-Matter in RMF

51

N, L, s, , r

PM1-L1

gsL, BE  16 M eV,
M *N / M N  0.7,
K  200 M eV
at r 0  0.17 fm -3

2
gs ,
3

SU(3)

Initial Angle-Dependence

ki  n (neutrino chem. pot.), B  2 1017 G and qi  0

生命の起源？
地球上で発生？
爆発的（暴走？）な進化を遂げた多様な地球上生命

ＤＮＡは宇宙から？
生命が宇宙に起源を持つとすれば ・ ・ ・
太陽系外のアミノ酸も同じ構造を持っている筈。

生命の起源を解く鍵

地球上のアミノ酸はすべて左巻き（Ｌ型）
左巻きキラリティーは地球だけの偶然（地球・太陽系起源説）？
それとも宇宙に共通（宇宙起源説）？
光学異性体

左（Ｌ）型と右（Ｄ）型は互いに鏡像関係にあり、左型を回転させても右型には一致しない。

http://www.nao.ac.jp/releaselist/archive/20100406/index_j.html

円偏光をとらえたすばる望遠鏡観測装置
すばる望遠鏡、オリオン星雲中心部の星形成領域に円偏光モード観測！
黄色部分が光が左回り（反時計回り）、
赤色部分が右回りの円偏光の領域。

実験室の偏光実験で否定
地球（太陽系）起源説：
大規模な円偏光に原始太陽系が飲み込まれて誕生。
円偏光の照射で左巻きアミノ酸が選択され、その後隕石で地球に持ち込まれた。
第２、第３の地球では、左巻き、右巻き両方のアミノ酸が存在しえる。

マーチソン隕石:アミノ酸は人類と同じ左型！
ＮＡＳＡ発表（２００９年３月１６日）
http://tokyo.secret.jp/80s/come/amino-acid.html

はやぶさ、奇跡の生還！
小惑星イトカワからのサンプルリターンに成功。

はやぶさⅡに期待！

アミノ酸は全宇宙で左巻き＝宇宙起源説
ボイド・梶野・ファミアーノ・尾中 論文, Astrobiology 10 (2010), 561-568; Int. J. Mol. Sci. 12(2011) 3432; Astrobiology (2014), submitted.

強磁場を持つ超新星（原始中性子星）周辺でのニュートリノ・原子核相互作用★ 左右非対称が完全に破れた素粒子は宇宙でニュートリノだけ！
Mann and Primakoff, Origins of Life, 11 (1981), 255；
14Cのベータ崩壊！ ５７３０年の半減期は、あまりにゆっくり過ぎる！

★ 超新星から多量（~1058 個）のニュートリノが放射される。
銀河中心で起きたとすると、１０兆個/秒/cm2★ 生命元素（炭素、窒素、酸素など）は超新星爆発で合成される。
天の川で約５０年に一回の頻度で繰り返し起きる。

★ 原始中性子星/ブラックホールは強磁場（~1014 ガウス）を伴う。

5.14

スピン： ニュートリノ＝１/２、炭素・酸素＝０、窒素＝１。
3.95

14N lives !

0.06%

2mec2
14O

99.3%
νe + 14N → e- + 14O

2.31

磁場を帯びた中性子星

νe + 14N → e+ + 14C
14N dies !

0.16 100%
14C (5730y)

0.00
14N (1+)0.61%

強磁場を持つ超新星（原始中性子星）周辺でのニュートリノ・原子核相互作用
Boyd, Famiano, Kajino & Onaka 2014,
Astrobiology, submitted.

ダイポール磁場
中性子星
or ブラックホール

強い磁場を帯びた中心星（中性子星、ブラックホール）からどれくらいの距離まで、磁場による偏極を保てるか？

SUMMARY
Relic Supernova-n:
Future observation of Relic Supernova n’s in megaton Hyper-Kamiokande(i.e. Gd-loaded Water Cherenkov detector in 10y run) could solve the SN
rate problem and also discriminate EoS and neutrino oscillation pattern.

n-Mass hierarchy & Total Mass:
Supernova n-process nucleosynthesis could determine the mass
hierarchy Dm132 and sin2q13～0.1 simultaneously. Inverted hierarchy isstatistically more preferred. Total n-mass, if Smν< 0.1eV or 0.05eV,strongly constrain the mass hierarchy.

Origin of r-process:
GRB could be a viable site for r-process (+ CCSN, MHD-jet, NSM).

Origin of Chirality of Amino Acids on Earth:
Breaking Chirality of neutrinos may be the universal origin.

Origin of Pulsar Kick:
Parity violation in magnetized neutron star triggers asymmetric n-baryon
reactions to likely explain the observed pulsar kick.