scholarly journals Few-body reactions investigated with the Trojan Horse Method

2020 ◽  
Author(s):  
Roberta Spartà ◽  
Giuseppe G. Rapisarda ◽  
Claudio Spitaleri ◽  
Marco La Cognata ◽  
Rosario G. Pizzone ◽  
...  
Keyword(s):  
Cross Sections ◽  
Power Plants ◽  
Indirect Method ◽  
Nuclear Astrophysics ◽  
Reaction Cross ◽  
Trojan Horse ◽  
Fusion Power ◽  
Trojan Horse Method ◽  
Reaction Cross Sections

The Trojan Horse Method is an indirect method to measure reaction cross sections at energies of interest for nuclear astrophysics, exploiting the nuclei clustering properties. Here it is presented with its general features and detailed for the case of the ^22H(d,p)^33H and ^22H(d,n)^33He measurements, where interesting results for astrophysics and energy fusion power plants have been obtained.

scholarly journals Unscreened cross-sections for nuclear astrophysics via the Trojan Horse Method

2014 ◽  
Vol 569 ◽  
pp. 012018
Author(s):  
A Tumino ◽  
C Spitaleri ◽  
M La Cognata ◽  
L Lamia ◽  
R G Pizzone ◽  
...  
Keyword(s):  
Cross Sections ◽  
Nuclear Astrophysics ◽  
Trojan Horse ◽  
Trojan Horse Method

scholarly journals Underground Measurements of Nuclear Reaction Cross-Sections Relevant to AGB Stars

Universe ◽  
2021 ◽  
Vol 8 (1) ◽  
pp. 4
Author(s):  
Chemseddine Ananna ◽  
Francesco Barile ◽  
Axel Boeltzig ◽  
Carlo Giulio Bruno ◽  
Francesca Cavanna ◽  
...  
Keyword(s):  
Nuclear Reaction ◽  
Chemical Evolution ◽  
Cross Sections ◽  
Nuclear Astrophysics ◽  
Reaction Cross ◽  
Agb Stars ◽  
The Cross ◽  
Reaction Cross Sections

Nuclear reaction cross sections are essential ingredients to predict the evolution of AGB stars and understand their impact on the chemical evolution of our Galaxy. Unfortunately, the cross sections of the reactions involved are often very small and challenging to measure in laboratories on Earth. In this context, major steps forward were made with the advent of underground nuclear astrophysics, pioneered by the Laboratory for Underground Nuclear Astrophysics (LUNA). The present paper reviews the contribution of LUNA to our understanding of the evolution of AGB stars and related nucleosynthesis.

Measurements of the 107Ag neutron capture cross sections with PHWT at the CSNS Back-n facility

2022 ◽  
Author(s):  
X. X. Li ◽  
L. X. Liu ◽  
W. Jiang ◽  
J. Ren ◽  
H. W. Wang ◽  
...  
Keyword(s):  
Cross Section ◽  
Cross Sections ◽  
Nuclear Power ◽  
Power Plants ◽  
Nuclear Astrophysics ◽  
Reaction Cross ◽  
Pressurized Water ◽  
Resonance Parameters ◽  
Control Rod ◽  
The Cross

Abstract Silver indium cadmium (Ag-In-Cd) control rod is widely used in pressurized water reactor nuclear power plants, and which is continuously consumed in a high neutron flux environment. The mass ratio of 107Ag in Ag-In-Cd control rod is 41.44%. To accurately calculate the consumption value of the control rod, a reliable neutron reaction cross section of the 107Ag is required. Meanwhile, 107Ag is also an important weak r nuclei. Thus, the cross sections for neutron induced interactions with 107Ag are very important both in nuclear energy and nuclear astrophysics. The (n, γ) cross section of 107Ag has been measured in the energy range of 1-60 eV using a back streaming white neutron beam line at China spallation neutron source. The resonance parameters are extracted by an R-matrix code. All the cross section of 107Ag and resonance parameters are given in this paper as datasets. The datasets are openly available at https://www.scidb.cn/s/aaUJbu.

Nuclear astrophysics: nucleosynthesis in the Universe

2012 ◽  
Vol 11 (4) ◽  
pp. 243-250 ◽  
Author(s):  
Alinka Lépine-Szily ◽  
Pierre Descouvemont
Keyword(s):  
Energy Range ◽  
Cross Sections ◽  
Nuclear Physics ◽  
Nuclear Astrophysics ◽  
Reaction Rates ◽  
Reaction Cross ◽  
Point Of View ◽  
Definition Of ◽  
The Universe ◽  
Reaction Cross Sections

AbstractNuclear astrophysics is a relatively young science; it is about half a century old. It is a multidisciplinary subject, since it combines nuclear physics with astrophysics and observations in astronomy. It also addresses fundamental issues in astrobiology through the formation of elements, in particular those required for a carbon-based life. In this paper, a rapid overview of nucleosynthesis is given, mainly from the point of view of nuclear physics. A short historical introduction is followed by the definition of the relevant nuclear parameters, such as nuclear reaction cross sections, astrophysical S-factors, the energy range defined by the Gamow peak and reaction rates. The different astrophysical scenarios that are the sites of nucleosynthesis, and different processes, cycles and chains that are responsible for the building of complex nuclei from the elementary hydrogen nuclei are then briefly described.

scholarly journals Experimental Investigation of radiative proton-capture reactions relevant to Nucleosynthesis

2019 ◽  
Vol 24 ◽  
pp. 168
Author(s):  
A. Khaliel ◽  
T. J. Mertzimekis ◽  
A. Psaltis ◽  
I. Psyrra ◽  
A. Kanellakopoulos ◽  
...  
Keyword(s):  
Cross Sections ◽  
Nuclear Reactions ◽  
Nuclear Astrophysics ◽  
Theoretical Models ◽  
Reaction Cross ◽  
Tandem Accelerator ◽  
Proton Capture ◽  
Isotopic Abundances ◽  
Vast Network ◽  
Reaction Cross Sections

One of the primary objectives of the field of Nuclear Astrophysics is the study of the elemental and isotopic abundances in our solar system. Although a lot of progress has been made regarding a large number of nuclides, there is still a number of neutron-deficient nuclei, ie the p nuclei, which cannot be created via the s and r processes. These processes are responsible for the production of the bulk of heavy nuclides. The pre-explosive or explosive phases of massive stars are considered potential loci for p nuclides production via various combinations of photodisintegrations and nucleon captures, along with β+ decays and electron captures. For the study of the vast network of nuclear reactions (over 20'000) that are responsible for observed isotopic abundances, the statistical model of Hauser-Feshbach is employed. The model requires the knowledge of nuclear reaction cross sections, quantities that can be measured in the laboratory. In this work, we report on recent experimental attempts to measure such cross sections in radiative proton-capture reactions involving 107,109Ag near the astrophysically relevant energy window. Measurements have been performed at the Tandem Accelerator Laboratory of the N.S.C.R. “Demokritos”. The results are compared to various theoretical models, using the TALYS and EMPIRE codes, in an attempt to provide experimental input to astrophysical models.

scholarly journals Electron Screening in Nuclear Astrophysics

2020 ◽  
Vol 227 ◽  
pp. 01012
Author(s):  
Matej Lipoglavsek ◽  
Aleksandra Cvetinović
Keyword(s):  
Nuclear Reaction ◽  
Cross Sections ◽  
Inverse Kinematics ◽  
Nuclear Reactions ◽  
Nuclear Astrophysics ◽  
Reaction Cross ◽  
Electron Screening ◽  
Low Energies ◽  
Order Of Magnitude ◽  
Reaction Cross Sections

Electron screening in an important effect that cannot be neglected in nuclear astrophysics, since it influences nuclear reaction cross sections at low energies. We are trying to understand why most measurements in inverse kinematics on solid targets give electron screening potentials more than an order of magnitude above predictions. Below we report our latest results on electron screening in nuclear reactions 1H(14N,γ)15O and 2H(19F,ρ)2°F in both inverse and normal kinematics. The analysis is in progress.

scholarly journals Surrogate nuclear reactions: an indirect method for determining reaction cross sections

2005 ◽  
Vol 31 (10) ◽  
pp. S1687-S1690 ◽  
Author(s):  
J Escher ◽  
L Ahle ◽  
L Bernstein ◽  
J Burke ◽  
J A Church ◽  
...  
Keyword(s):  
Cross Sections ◽  
Indirect Method ◽  
Nuclear Reactions ◽  
Reaction Cross ◽  
Reaction Cross Sections

Formation of α clusters in dilute neutron-rich matter

Science ◽  
2021 ◽  
Vol 371 (6526) ◽  
pp. 260-264 ◽  
Author(s):  
Junki Tanaka ◽  
Zaihong Yang ◽  
Stefan Typel ◽  
Satoshi Adachi ◽  
Shiwei Bai ◽  
...  
Keyword(s):  
Cross Sections ◽  
Cluster Formation ◽  
Reaction Cross ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Heavy Nuclei ◽  
Α Decay ◽  
Neutron Skin Thickness ◽  
Reaction Cross Sections ◽  
Α Particles

The surface of neutron-rich heavy nuclei, with a neutron skin created by excess neutrons, provides an important terrestrial model system to study dilute neutron-rich matter. By using quasi-free α cluster–knockout reactions, we obtained direct experimental evidence for the formation of α clusters at the surface of neutron-rich tin isotopes. The observed monotonous decrease of the reaction cross sections with increasing mass number, in excellent agreement with the theoretical prediction, implies a tight interplay between α-cluster formation and the neutron skin. This result, in turn, calls for a revision of the correlation between the neutron-skin thickness and the density dependence of the symmetry energy, which is essential for understanding neutron stars. Our result also provides a natural explanation for the origin of α particles in α decay.

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