Nuclear Physics in Greece
RECFA, Athens-Greece, 10/11/2023
Nikolas Patronis
n_TOF Physics Coordinator
CERN & Univ. of Ioannina
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The Hellenic Nuclear Physics community
Institutes:
Our younger colleagues:
BSc: ~40; MSc: ~15; PhD: ~25; post-docs:~10
Faculty members, Researchers: 25
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National and Kapodistrian University of Athens
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NCSR “Demokritos”
AMS (U. Oxford, under installation)
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National Technical University of Athens
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University of Ioannina
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Aristotle University of Thessaloniki
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HCMR
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Distinctions and funding of the Hellenic Nuclear Physics Community
AMS (U. Oxford, under installation)
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The n_TOF facility
Is the “gluon” of the Greek Nuclear Physics Society:
Join forces for:
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The n_TOF facility
Motivation:
High precision neutron induced cross section measurements for:
140 researchers
40 research institutions/teams
20 PhD students/year
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The n_TOF facility: EAR1 + EAR2 + NEAR
NEAR
proton beam from the PS
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proton beam
N2 gas cooling to avoid Pb corrosion and contamination of the cooling circuit
R Esposito et al. Phys. Rev. Accel. Beams 24, 093001 (2021)
3rd generation target
The n_TOF facility
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The n_TOF facility
proton beam momentum | 20 GeV/c |
intensity (dedicated mode) | 8.5 x 1012 protons/pulse |
repetition frequency | 1 pulse/1.2s |
pulse width | 7 ns (rms) |
n/p | 300 |
lead target dimensions | 70x76x63 cm3 |
cooling & moderation material | N2 & H2O (borated) |
moderator thickness in the exit face | 5 cm |
neutron beam dimension in EAR-1 (capture mode) | 2 cm (FWHM) |
The n_TOF facility
Neutron physics data for 11 orders of magnitude of neutron energies
The n_TOF facility: Is a unique neutron facility
Neutron physics data for 11 orders of magnitude of neutron energies
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The n_TOF history in a nutshell
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The n_TOF (bright!) future
Short term
Mid term
Long term
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Conclusions
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Thank you so much for your attention!
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Extra Slides
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The NEAR station
The NEAR Station is the n_TOF facility’s new high-flux irradiation station.
Two regions of activities
We can make integrated reaction rate measurements by shaping the neutron spectrum to look as close as possible to the stellar one
Boron Carbide filters
Irradiation at NEAR
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ESA INTEGRAL mission detects 26Al γ-rays
Nuclear physics data are necessary in order to quantify the 26Al net yield: production – destruction:
26Al(n,p/a) reactions are responsible for the destruction rate
•26Al is a radioactive nucleus produced in massive stars
•The 26Al half-life time (=720 thousand years) is still very small with respect to the age of Universe (=14 billion years).
•Each 26Al nucleus decay produce one highly energetic γ-ray at 1.8 MeV. The interstellar medium is transparent to this ”light”
•By recording these γ-rays we have a ”snapshot” of on-going nucleosynthesis in our Galaxy. Accordingly, we can trace the dynamics of the Milky Way (rotational speed, expansion, chemical element production, etc)
•From the total production and destruction of 26Al, we can understand how the cosmos chemical element factories (=stars) are producing energy and matter
n_TOF: Understanding the 26Al galactic snapshot
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Detector tests
DDX:
Double-Differential Charged-Particle
detection setup for XS measurements from 20 to 200 MeV
n beam
n beam
X17 detection setup:
Resolution function – setup
M. Bacak | n_TOF EAR1 | n_TOF CM
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30.05.2022
4x C6D6 detectors