Neutrino-Nucleus Reactions and Nucleosynthesis

Toshio Suzuki 　　Nihon University

Roles of ν-process in nucleosynthesis

核物理から見た宇宙New Era of Nuclear Physics in The CosmosRIKEN Sept. 25, 2008

Roles of ν-processes in nucleosynthesis

Production of elements: 7Li, 11B, 19F, 26Al … 51V Rare elements 138La, 180Ta Woosley et al, Astrophy.J 356 (1990) Heger et al., PL B606 (2005)

Haxton Heger et al.

Nucleosynthesis through neutrino-induced reactions

Qian, Haxton, Langanke, Vogel ， PR C55 (1997)

138 138

180 180

( , )

( , )

Ba e La

Hf e Ta

GT exp. RCNP (3He, t)More GT strength than RPA(Heger et al.) Byelikov et al., PRL 98 (2007)

・ Production of rare elements by ν- reactions

・ Role of νin r-process nucleosynthesis

N=82, 126 regionsWithν-induced n emission →solar abundances

Calculation by Heger et al.

Research subjects(1) Reaction rates: better evaluations ν-nucleus reaction cross sections BR to n, p, γ, αemission channnels(2) ν-oscillation effects(3) Find possible new processes ex. νp process Frohlich et al, PRL 96 (2006)

64Ge(n,p) → nucleosynthesis of A>64 nuclei 92,94Mo, 96,98Ru otherwise flow stops at 64Ge (beta halif life=64s)

e p n e

New evaluation of reaction rates in p-shell and fp-shell nuclei

• ν-12C, ν-4He reactions evaluated by new shell model Hamiltonians (SFO)

　 ・ Synthesis of 7Li, 11B in supernovae 　・ Oscillation effects• GT strength in 56Ni, 58Ni and Ni isotopes

evaluated by GXPF1 ・ ν-56Ni reaction and synthesis of 55Mn in Pop. III star ・ n emission from n-rich Ni isotopes

Light Element Abundances and Nucleosynthesis Processes

Inner O/C He/C He/H H

10 12 10

12 10

12 10

12 11 10

10 12 10 13 10

Be : C( , 'pp) Be,

C( ,e pn) Be,

C( ,e d) Be,

C( ,e p) Be( ,n) Be

B : C( , 'pn) B, C(p, ) B

9 12 3 9

12 9

12 12 9

6 12 6 9 6

Be : C( , ' He) Be,

C( , 'pd) Be,

C( ,e ) B(p, ) Be

Li : C( , ' x) Li, Be(p, ) Li

Supernovae νSpectra

σ∝ E2

<E> & tail part ]/exp[

/)(

TETE

NEf1

32

),(),( 08MeVT ),.( 3266 MeV

MeVE 25:,

:e MeVE 11),.(),( 053 MeVT

:e MeVE 16),(),( 05MeVT

Neutrino-induced Reactions

W

e

e p

n

0Z

N

N'

charged-current neutral-current

Spin-dependent excitations ● Gamow-Teller (1+): ● Spin-diole (0-, 1-, 2-):

SFO: good description of magneticmoments, GT inp-shell nuceleiSuzuki, Fujimoto,Otsuka, PRC (2003)

Cross sections for Supernova Neutrinos with temperature T　　　

p and n emissions BR: Hauser-Feshbach model

Cross sections for Supernova Neutrinos with temperature T S. Chiba

SFO

ν- 4He reaction cross sections

cf. Woosley-Haxton: Sussex potential by Elliott et al.

Abundances of 7Li and 11B produced in supernova explosion processes

　　 M=16.2 M☼ (SN 1987A)

MeVTMeVTMeVTee

0.6,0.5,2.3 ,

No oscillation case

Cf. Yoshida, Suzuki, Chiba et al., Astrophys. J (2008)

7Be, 11C abundance

SN Nucleosynthesis with Neutrino OscillationsSupernova nucleosynthesis (-process)

16.2 M star supernova model corresponding to SN 1987A

Increase by a factor of 2.5 and 1.4Increase in the rates of charged-current reactions4He(e,e-p)3He and 12C(e,e-p)11C in the He layer

Normal mass hierarchy, sin2213 = 0.01

10-9

10-8

10-7

10-6

10-5

2 3 4 5 6

Mas

s F

ract

ion

Mr / M

11B

11C

O-rich O/C He/C He/N

10-10

10-9

10-8

10-7

10-6

2 3 4 5 6

Mas

s F

ract

ion

Mr / M

7Be7Li

O-rich O/C He/C He/N

no mix no mix

mix

no mix

mix

mix

7Li/11B Dependence on Mass Hierarchy and 13

N(7Li)/N(11B) Good indicator for neutrino oscillation parameters

normal

inverted

no mix

(Te, Te, T, E) = (3.2, 5.0, 6.0, 3.0) , (3.2, 4.8, 5.8, 3.0) , (3.2, 5.0, 6.4, 2.4) , (3.2, 4.1, 5.0, 3.5) , (4.0, 4.0, 6.0, 3.0) , (4.0, 5.0, 6.0, 3.0) (MeV, MeV, MeV, ×1053ergs)

Including uncertainties in neutrino temperatures

N(7Li)/N(11B) > 0.8Normal mass hierarchy and sin2213 > 0.002

Possibility for constraining mass hierarchy and lower limit of the mixing angle 13.

Neutrino experiments Constraining upper limit of 13

Cf. Yoshida et al.,PRL 96 (2006)

8-12MeV8-13MeV

M1 strength (GXPF1J)

7-12MeV 7-12MeV

Honma

fp-shellB(GT) for 58Ni

Exp: Fujita et al.

Neutron emission from Ni isotopes (BR by Higashiyama)

Neutral current reaction on 56Ni

Synthesis of Mn in Population III Star

56 55

54 55

55 55 55

Ni( , 'p) Co

Fe(p, ) Co

Co(e , ) Fe(e , ) Mn

58 59 59 59Ni(p, ) Cu(e , ) Ni(e , ) Co

　　　　 [Mn/Fe]No ν -0.53HW02 -0.29

　　　 [Mn/Fe]GXPF1J -0.25GXPF1J×2 -0.17

No νWith ν(GXPF1J)With ν x2With ν(Woosley)

Yoshida, Umeda, Nomoto

Summary

• Successful description of spin modes in nuclei （ GT transitions, magnetic moments 、 and M1 transitions ） by new shell model Hamiltonians

• Enhancement of ν-nucleus reaction cross sections

• More n emission from n-rch Ni isotopes

• Enhancement of production yields of 7Li, 11B, and 55Mn in supernovae

Collaborators

T. Yoshidab, S. Chibac, M. Honmad, K. Higashiyamae, H. Umedaf, K. Nomotof, D.H. Hartmanng, T. Kajinob,f and T. Otsukah

bNational Astronomical Observatory of JapancJapan Atomic Energy AgencydUniversity of AizueChiba Institute of TechnologyFDepartment of Astronomy, University of TokyogDept. Of Physics and Astronomy, Clemson UniversityhDepartment of Physics and CNS, University of Tokyo

B(GT) values for 12C -> 12N

present = SFO Suzuki, Fujimoto, Otsuka, PR C67 (2003)

Magnetic moments of p-shell nuclei

KVIRCNP

Negret et al., PRL 97 (2006)

B(GT) values for 14N -> 14C

SFO

SFO*: gAeff/gA=0.95

B(GT: 12C)_cal = experiment

SFO

Exp: LSNDPR C64 (2001)

EXP

Allen et al.(1990)

ν-12C Exclusive 12C → 12N (1+)

●WBP: Warburton-Brown ●HT: Hayes-Towner, PR C62, 015501 (2000) p:Cohen-Kurath (8-16)2BME, sd: USD of Wildenthal, 　 pf: KB3, p-sd and others: Millener-Kurath●NCSM: Hayes-Navratil-Vary, PRL 91 (2003) 　 AV8’(2-body) + TM’(99) (3-body)●CRPA: Kolb-Langanke-Vogel, NP A652, 91 (1999)

●SFO*: gAeff/gA=0.95

Suzuki, Chiba, Yoshida, Kajino, 　　　 Otsuka, PR C74 (2006)