neutrons at cern n_tof: a window to stellar evolution and nucleosynthesis
DESCRIPTION
Neutrons at CERN n_TOF: A window to stellar evolution and nucleosynthesis. ( Astro )Physics case for neutron cross section measurements Example of measurements performed so far at n_TOF The present experimental plan New opportunities with a second experimental beam-line. - PowerPoint PPT PresentationTRANSCRIPT
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Neutrons at CERN n_TOF: A window to stellar evolution andnucleosynthesis
• (Astro)Physics case for neutron cross section measurements• Example of measurements performed so far at n_TOF• The present experimental plan• New opportunities with a second experimental beam-line
The n_TOF Collaboration
A Mengoni, ENEA, Bologna – IAEA, Vienna
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Why neutrons in astrophysics?
e-charge : 0mass : 940 MeVhalf-life : 10 min
Now4.5 Gyr
solar-
system
formati
on
BANG!
The n_TOF Collaboration
GCE
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Abundances: Anders and Grevesse, 1989
Nucleosynthesis of the Elements
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Abundances: Anders and Grevesse, 1989
Nucleosynthesis of the Elements
Nuclear reactions:• energy generation• nucleosynthesis
condensation
ejec
tion,
exp
losi
on
interstellargas & dust
Mixing(abundance distribution)
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Abundances: Anders and Grevesse, 1989
Nucleosynthesis of the Elements
All chemical elements beyond Ironare synthesized by neutron interactionsin stars
~ ½ by the s-process (red giants)~ ½ by the r-process (explosive)
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Abundances: Anders and Grevesse, 1989
Nucleosynthesis of the Elements
56Fe 91.72
57Fe 2.2
58Fe 0.28
Fe
Co
60Ni 26.223
59Co100
59Fe 44.503 d
60Fe 1.5 106 a
60Co5.272 a
61Co1.65 h
61Ni 1.140
62Ni 3.634
Ni 63Ni 100 a
64Ni 0.926
58Co70.86 d
62Cu9.74 m
63Cu69.17
64Cu 12.7 h
61Fe 6 m
Cu
56Fe 91.72
57Fe 2.2
58Fe 0.28
Fe
Co
60Ni 26.223
59Co100
59Fe 44.503 d
60Fe 1.5 106 a
60Co5.272 a
61Co1.65 h
61Ni 1.140
62Ni 3.634
Ni 63Ni 100 a
64Ni 0.926
58Co70.86 d
62Cu9.74 m
63Cu69.17
64Cu 12.7 h
61Fe 6 m
Cu
The canonical s-process
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The n_TOF Collaboration
Neutron capture cross sections
reaction rate: NA Nn<sn,g(En)·v>kT
key quantity: sn,g(En)
canonical s-process: s · NA ~ const.
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The n_TOF Collaboration
Neutron capture cross sections
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The n_TOF Collaboration
Neutron capture cross sections
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The n_TOF Collaboration
Neutron capture cross sections
weak
main
A
i iA
AAAA
NfNN
56
1
00
56
0
11 11/11 ss
ss
from phenomenological…
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The n_TOF Collaboration
Neutron capture cross sections
C Arlandini, et al.: ApJ 525 (1999) 886
• M = 2 M• Z = 0.5 Z
… to detailed stellar modeling: TP-AGB
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Needed: cross sections with uncertainties between 1 and 5% for complete set of isotopes from 12C to 210Po,
including unstable samples
Status and requests
Source: F Käppeler (2009)
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wide energy range high neutron flux &
high energy resolution low repetition rate
of the proton driver
457
130
518718001280
2
1
2
1
mm.
/s/s.
LL
ff
comparison with GELINA (~ same average flux at 30m)
232Th(n,g)
10 100 1000 10000 10000010-1
100
101
102
Res
pons
e (c
ount
s / n
s)Neutron Energy / eV
n-TOF 232Th (0.0041 at/b) 208Pb
GELINA 232Th (0.0016 at/b) 208Pb
source: P Rullhusen (GELINA)
Basic characteristics of experiments at n_TOF
The n_TOF Collaboration
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Basic characteristics of experiments at n_TOF
wide energy range high neutron flux &
high energy resolution low repetition rate
of the proton driver low background conditions
U Abbondanno et al. (The n_TOF Collaboration)Phys. Rev. Lett. 93 (2004), 161103
&S Marrone et al. (The n_TOF Collaboration)
Phys. Rev. C 73 03604 (2006)151Sm(n,g)
The n_TOF Collaboration
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0.0E+00
5.0E-09
1.0E-08
1.5E-08
2.0E-08
2.5E-08
3.0E-08
0 1 2 3 4 5 6
Temperature T8 [K]
deca
y ra
te [1
/s]
ne = 1, 3, 10, 30×1026 cm-3
• The branching at 151Sm can be used to determine the temperature during the s process.
T = 350 ± 40 Million KelvinkT = 30 keV
Sm
Eu
Gd
150Sm
151Sm 93 a
152Sm
153Sm
154Sm
151Eu
152Eu
153Eu
154Eu
155Eu
156Eu
152Gd
153Gd
154Gd
155Gd
156Gd
157Gd
Sm
Gd151
150
152
Sm NσNσ
)(λλλ
fnβ
ββ
Example: Branching point at 151Sm
source: M Heil
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Measurements performedCapture151Sm204,206,207,208Pb, 209Bi232Th24,25,26Mg90,91,92,94,96Zr, 93Zr139La186,187,188Os233,234U237Np,240Pu,243Am
Fission233,234,235,236,238U232Th209Bi237Np241,243Am, 245Cm
The n_TOF Collaboration
s-process branching, temperature, densitytermination of the s-process, nucleosynthesis of Lead
neutron source for the s-process: 22Ne(a,n)25Mg
massive stars, pre-solar grains
nuclear cosmo-chronometer
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Capture measurementsMo, Ru, Pd stable isotopes
Fe, and Ni (all stable isotopes)
A≈150 (isotopes varii)
79Se, Se (stable isotopes)
r-process residuals calculationisotopic patterns in SiC grains
s-process nucleosynthesis in massive stars
s-process branching pointslong-lived fission products
s-process branching (T and r for the weak component)
Other measurements147Sm(n,a), 67Zn(n,a), 99Ru(n,a)58Ni(n,p), other (n,lcp)
p-process studies
n_TOF-Ph2
(*) Approved by the RB (P208/n_TOF13)
Planned measurements
The n_TOF Collaboration
>>
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n_TOF-Ph2
n_TOF target
NewExperimentalArea (EAR-2)
The second n_TOF beam line & EAR-2
EAR-1 (at 185 m)
~ 20 m
Flight-path length : ~20 mat 90° respect to p-beam directionexpected neutron flux enhancement: ~ 100drastic reduction of the t0 flash
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Improvements (ex: 151Sm case)
sample mass / 3 s/bkgd=1
use BaF2 TAC e x 10 use D2O F30 x 5 use 20 m flight path F30 x
100
consequences for sample mass
50 mg 5 mg 1 mg 10 mg
boosts sensitivity by a factor of 5000 !
problems of sample production and safety issues relaxed
EAR-2: Optimized sensitivity
The n_TOF Collaboration
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The n_TOF Collaboration
Possible measurements at EAR-2
• 79Se• 90Sr• 126Sn• 147Pm• 135Cs
all s-process branching points + they are important fission fragments
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The n_TOF Collaboration
ConclusionNeutron cross sections are key quantities for studying stellar evolution and nucleosynthesis. n_TOF offers the best conditions to obtain these nuclear physics quantities with the required accuracy
The n_TOF Collaboration is carrying on an extensive plan to measure cross sections relevant for nuclear astrophysics, in particular for s-process nucleosynthesis studies
Opportunities for obtaining new data for presently inaccessiblenuclei (using extremely low quantities of material) will be open with the implementation of a second beam-line and a new experimental area (EAR-2)
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The n_TOF Collaboration
The end
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n_TOF-Ph2
Motivations:
• Study of the weak s-process component (nucleosynthesis up to A ~ 90)
• Contribution of massive stars (core He-burning
phase) to the s-process nucleosynthesis.
• s-process efficiency due to bottleneck cross sections (Example: 62Ni)
In addition:
Fe and Ni are the most important structural materials for nuclear technologies. Results of previous measurements at n_TOF show that capture rates for light and intermediate-mass isotopes need to be revised.
Capture studies: Fe, Ni, Zn, and Se<<back
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n_TOF-Ph2
32
30
34
38 40 42 44 46 48 50
The 79Se case
• s-process branching: neutron density & temperature conditions for the weak component.
• t1/2 < 6.5 x 104 yr
Capture studies: Fe, Ni, Zn, and Se<<back
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Observational uncertainties
Cross section uncertainties
Bao et al. ADNDT 76 (2000)
• Stellar model • s-abundance calculation• r-abundance (CS22892-
052)
See:Tavaglio et al., APJ521 (1999)Arlandini et al., APJ525 (1999) s-only
isotopes
Need for more than one r-process or need for improved s- abundances and cross sections?
In general:
<<back
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Source: F Herwig
<<
AGB stars
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n_TOF experiments & publications
Capture151Sm204,206,207,208Pb, 209Bi232Th24,25,26Mg90,91,92,94,96Zr, 93Zr139La186,187,188Os233,234U237Np,240Pu,243Am
Fission233,234,235,236,238U232Th209Bi237Np241,243Am, 245Cm
In summary:
Facility & Experimental setup : 11 papersMeasurements : 10 papers
(1 PRL, 9 PRC)Conference Proceedings : 51Total number of documents on db : 150
The n_TOF Collaboration
All data (published) can be found in the EXFOR database >>
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151Sm
204,206,207,208Pb, 209Bi
24,25,26Mg
90,91,92,94,96Zr, 93Zr, 139La
186,187,188Os
Measurements performed so far
The n_TOF Collaboration www.cern.ch/n_TOF
s-process branching, temperature, density
termination of the s-process, nucleosynthesis of Lead
neutron source for the s-process: 22Ne(a,n)25Mg
massive stars, pre-solar grains
nuclear cosmo-chronometer