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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
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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.
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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.
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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
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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
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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
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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
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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-):
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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
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Cross sections for Supernova Neutrinos with temperature T S. Chiba
SFO
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ν- 4He reaction cross sections
cf. Woosley-Haxton: Sussex potential by Elliott et al.
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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)
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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
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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)
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8-12MeV8-13MeV
M1 strength (GXPF1J)
7-12MeV 7-12MeV
Honma
fp-shellB(GT) for 58Ni
Exp: Fujita et al.
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Neutron emission from Ni isotopes (BR by Higashiyama)
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Neutral current reaction on 56Ni
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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
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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
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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
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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
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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
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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)