Meeting on “Unification of Particle Physics, Nuclear Physics
and Astrophysics”, Ise-Shima, December 3-5, 2011

Nucleosynthesis in Supernovae andGRBs and Neutrino Oscillation
Taka KAJINO
National Astronomical Observatory (NAOJ)
Department of Astronomy, University of Tokyo (UT)
COSNAP-Collaboration
NAOJ: W. Aoki, K. Nakamura, J. Hidaka, T. Kuroda, T. Yamazaki,
Tokyo: T. Yoshida, W. Fujiya, S. Sato, K. Shaku, M. Kusakabe,T. Otsuka, K. Nomoto, H. Umeda, S. Kawagoe, N. Yasutake
JAEA: T. Hayakawa, S. Chiba, N. Iwamoto,
Nihon: T. Suzuki, T. Maruyama,
Nagoya: H. Yokomakura, K. Kimura, A. Takamura,
Visi. Profs.: K. Cheoun (Soongsil), Y. Pehlivan (Turky), G. Mathews(Notre Dame), A. Balantekin (Wisconsin), M. Famiano (W.Michigan)ニュートリノの質量
Neutrino Masses

1～

Quark& Lepton Masses ～他の素粒子の質量10,000,000,000

Why 10-10 ?

Quark & Lepton
MassesE = mc2

This could be a signature of new physics at 1010
times higher energy scale than the ordinary scale.

10-10νi + νie+ + e-2γ (Τ)

Key Physics suggested by FINITE mass neutrinos:νµ?

ντν Masses

Unification of elementary forces beyond thestandard model ?
CP violation and Lepto- & Baryo-genesis ?

Generation

Why left-handed neutrinos, Majorana or Dirac ?
Explosion Mechanism of cc-SNe & Neutron Stars ?

Neutrino Oscillations|⊿m232| and θ23⊿m122 and θ12

SK (atmospheric ν)
KAMIOKANDE, SK, KamLand (reactor ν), SNO“KNOWN”

23－mixing
sin22θ23 = 1.02-32|Δm 23| = 2.4×10 eV12－mixing
Cabibbo angle
sin22θ12 = 0.816 (θ12+θC=π/2)2-52Δm 12 = 7.9×10 eV“UNKNOWN”
13－mixing● sin22θ13 (< 0.1)
T2K, June 14, 2011

● ⊿m132 = ±2.4x10-3 eV2● δ＝CP-phase● Absolute Mass
E(νµ)=E(ντ): Kobayashi-Masukawa, PTP (1973)
Yokomakura et al., PL B (1986)

Various Neutrino-Sources in Nature
1.9K

CMB
Cosmic Background

Neutrino Cosmology
verificationof particle model

νe, νµ, ντνe, νµ, ντ

PURPOSE
Study SUPERNOVA-ν and CMB-Anisotropies:
1. to constrain the ν−oscillation parameters θ13 and ⊿m132.
2. to constrain the ν−total mass.


Various roles of ν’s in SN-nucleosynthesisνp-process:
92Mo, 96Ru ?

MSW high-density resonancethrough θ13 at ρ ~ 103 g/cm3

νeNS

νµτ

SiLayer

R-process:Heavy Nuclei
Explo. Si-burn.
Fe-Co-Ni,60Co, 55Mn, 51V …

ν-process180Ta, 138La, 92Nb, 98Tc …

ν-process:
6,7Li, 9Be, 10,11B …

Neutrino-driven relativistic jet (Harikae + ’09, ‘10Special relativistic MHD code (Takiwaki et al 2009) Neutrino heating is calculated by ray-tracing in flat timespace.
 Realistic EOS of Shen et al (1998) is implemented.
 Initial data is taken from 35OC model (Woosley&Heger 2006)
Supernova
Nucleosynthesis
Simulation
T. Kajino & S. Chiba
ν-Pair Heated Collapsar Model
K. Nakamura, et al. ApJ (2011).

Proton Number Z

235U
208Pb

184

56Fe

126
82
50

20 28

Neutron Number N

R-process in Pair ν-Heated Collapsar Model for GRB
K. Nakamura, S. Sato, S. Harikae, T. Kajino and G.J. Mathews (2011), submitted to ApJ.
Neutron-rich condition for successful r-process:0.1 < Ye < 0.5
Sr-Y-ZrTνe = 3.2 MeV < Tνe = 4 MeVI-XeIr-Pt
Pb

Collapsar model

Dy-Er

Observed
Solar r-abundance
107,109Agtν >> tdyn

197Au

Tantalum（180,181Ta）

138La

181Ta （stable）, 180Ta (unstable, τ180Tam（isomer, τ15gg
1/2 = 8h）,
1/2 > 10 y)

180Ta is the rarest isotope in the Solar-Systerm andeven in the Universe!
Where was 180Ta synthesized ?
p processBurbidge2–Fowler-Hoyle,
RMP 29 (1957), 547-650.
“Element Genesis”

Neutral current
W. Fowler
F. Hoyle
M. Burbidgein Supernovae
J. Burbidger process (１９９０)

180Ta-genesis needs Quantum Phys. + SN Hydro-dyn.

Solar-180Ta is all “ISOMER” with T1/2 > 1015 y!

Excitatoin Energy- Long lived 180Tam is excited in hot SN-photon bath.
- Intermediate states are depopulated to the ground state,
which decays in 8 hours.
We solved dynamical “explosive SN-nucleosynthesis” coupled with“quantum transitions” simultaneously. (Hayakawa, et al. 2010, PR C81,052801®; PR C82, 058801)

Photons

Intermediate
statesIntermediate States

Plan
PlanckianDistribution

Distribution

Intermediate
statesK=9
K9-= 9180180Tag
TaT > 10 yIsomer
180Tam : solar abundance
T1/2=8.15 hK = 1 Ground
K=1St.
01+

Photon Flux

1575.3 T
1/2 > 10 15y
1/2IsomerResult fromν-Nucleosynthesis

T. Hayakawa, T. Kajino, S. Chiba, andG.J. Mathews, Phys. Rev. C81 (2010), 052801®
About 40% 180Tam
survives in supernova
explosion.

7766
55

138La
138La Heger et al. PLB606, 258 (2005)
180Ta (Overproduction)
180Ta
180Ta isomerThen, both 138La and180Ta abundances
can be consistentlyreproduced by theCC-int. of νe and νe of180Ta (New result)

4433Tνe = 3.2 MeV,Tνe = 4 MeV.

221100solar
solar
solar
gamma
system only

nc
6MeV

cc
4MeVcc
6MeVcc8MeV

Consistent withthe r-process !

Oscillation
Supernova(MSW)
ν-ProcessEffectto
onestimate
SupernovaTνµ,ν-Processand TντSN II: Yoshida, Kajino & Hartman, Phys. Rev. Lett. 94 (2005), 231101.
SNIc + II: Nakamura, Yoshida, Shigeyama, Kajino, ApJL 718 (2010), L137.

Tνµ, = Tντ = 6 MeV

GCE of 11B & 11B/10B
Abundance XAνν-temperatures
are known!
ν0.25
0.20.15

νe T(νe) < T(νe) < T(νx)
3.2

4.0

νe

6.0MeV
~85%

0.1
0.05

νµ,τ ,νµ,τ

0MSW
resonance
0 high-density
10 20 30
40 50

νx→νe~15%εν (MeV)

60

Suzuki, Chiba, Yoshida,Kajino & Otsuka, PRC74(2006), 034307

Our Theoretical Prediction
7Li/11B-Ratio
Yoshida, Kajino et al . 2005, PRL94, 231101; 2006, PRL 96, 091101;
2006, ApJ 649, 319; 2008, ApJ 686, 448.

Astrophysics:

Mass Hierarchy⊿m132

Normal Mass
Hierarchy

13-Mixing Angle
θ13

7Li/11B

Long Baseline Exp:

・T2K (Kamioka)

Inverted

June 14, 2011

・MINOSJuly 29, 2011
No Mixing10-6

10-5

10-4 10-3
sin22θ13

・RENO (KOREA)

10-2

10-1

・Double CHOOZ・Daya Bay

22θ ?
the lowerlimit
What isWhat
the islowerlimit tosinto
13sin2(θ13)?

T2K

Compasrison between MINOS and T2K

M(Inverted)(Normal)Mass hierarchy is still unknown !

Our Theoretical Prediction
7Li/11B-Ratio
Yoshida, Kajino et al . 2005, PRL94, 231101; 2006, PRL 96, 091101;
2006, ApJ 649, 319; 2008, ApJ 686, 448.

Astrophysics:

Mass Hierarchy⊿m132

Normal MassHierarchy

13-Mixing Angle
θ13

7Li/11B

Excluded by T2K and MINOSLong Baseline Exp:Inverted

・T2K (Kamioka)
June 14, 2011

・MINOS
July 29, 2011
No Mixing

10-610-5

10-4 10-3
sin22θ13

10-2

10-1 ALLOWED !

Murchison SiC X-grains

SiC X grains exhibit- 12C/13C > Solar- 14N/15N < Solar- Enhanced 28Si
- Decay of 26Al (t1/2 = 7x105 yr)& 44Ti (t1/2 = 60 yr)
Origin in Core Collapse Supernovae

Mass Hierarchy, Normal or Inverted ?
Mathews, Kajino, Aoki and Fujiya, arXiv:1108.0725 (2011).

First Detection of 7Li/11B

Predicted 7Li/11B-Ratio

W. Fujiya, P. Hoppe, andU. Ott, ApJ 730, L7 (2011).

Normal Mass
Hierarchy

11B and 7Li were measuredin SiC presolar X-grains
which are known to bemade of Supernova dusts.

Excluded by T2K and MINOS

Excluded by
SiC X-Grains
Inverted“Inverted mass hierarchy”
is more preferred !

ν-Asymmetry under
the Strong Dipole(Poroidal) Magnetic
Field

Asymmetricν-scattering
Proto-neutronstars
andabsorption.
inc.c.
Supernovae

Fundamental Interactions amongHadrons (p, n, Λ, Σ …) and Lepton(e,ν…) at High-ρ and High-T in
Relativistic Field Theory and QCD
Maruyama, Kajino, Yasutake, Cheoun,& Ryu, PRD83 (2011), 081302 (R).

ΛNeutrino scattering and absorption
process inside the magnetized
Neutron star (1015G) is asymmetric.
⇒ ~ 2 % asymmetric ν-abs. (drift)⇒ Enough for Pulsar-Kick ~500km/s !
By D.Page

Magnetic Field and ν-interactions★ Poroidal  Pulsar Kick
★ Toroidal  Twist Mode  Spin down & growth of intsability

T. Kuroda, with Yasutake, Maruyama, Hidaka & Kajino
Initially dipole  Double Toroidals

Initially no dipole  Single Toroidal

Why Amino Acids on the Earth, All Left-Handed?
Chitrality, earth origin or universal ?
★ Neutrinos are all left-handed!
★ Supernovae with strongly magnetized neutron star
or BH emit intensive flux of neutrinos over 1010 yrs!
★ SN ejecta including 14N interact with neutrino understrong magnetic field!
★ Neutrino-14N coupling is asymmetric & chiral selective!
Boyd, Kajino, & Onaka suggested that the L-handed chirality of amino acids
is UNIVERSAL! (Astrobio. 10 (2010), 561-568; Int. J. Mol. Sci. 12 (2011), 3432)
Magnetized Supernovae

14N lives !

5.14
3.95

0.06%

2mec2
14O

99.3%
νe + 14N → e- + 14O

2.31
14N dies !

Mann and Primakoff (Origins of Life, 11 (1981), 255)
suggested β-decay of 14C, but it’s too SLOW!

νe + 14N → e+ + 14C
0.16 100%
14C (5730y)

0.00
14N (1+)

0.61%

CONCLUSION
We propose a new astrophysical method to determine
the unknown ν-oscillation parameters, θ13 and mass
hierarchy ∆m132, simultaneously in terms of the supernova
ν-process nucleosynthesis of 180Ta, 138La, 7Li and 11B
By taking account of the MSW effects.
Combining the recent detection of 7Li/11B isotopic ratio
in presolar X-grains and the T2K + MINOS results oflong-baseline neutrino oscillation experiments on θ13,
we can conclude that the “inverted mass hierarchy” ismore preferred.

Collaboration、highly desirable in Theory plus Exp/Obs.
as required/demoinstrated in SN-neutrino project!
Nucleosynthesis―c.c. SNe―ν―Magnetic Field―Life