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1. Measurement of the 235U(n,f) cross section relative to the 10B(n,α) reaction with Micromegas detectors at the CERN n_TOF facility: First results

Author: Michalopoulou Veatriki, Diakaki Maria, Vlastou Rosa, Kokkoris Michael, Stamatopoulos Athanasios, Tsinganis Andrea, Eleme Zinovia, Patronis Nikolas, Heyse Jan, Schillebeeckx Peter, Tassan-Got Laurent, Barbagallo Massimo, Colonna Nicola, Urlass Sebastian, Macina Daniela, Chiaveri Enrico, Aberle Oliver, Alcayne Victor, Amaducci Simone, Andrzejewski Józef, Audouin Laurent, Babiano-Suarez Victor, Bacak Michael, Bennett Samuel, Berthoumieux Eric, Billowes Jon, Bosnar Damir, Brown Adam, Busso Maurizio, Caamaño Manuel, Caballero-Ontanaya Luis, Calviño Francisco, Calviani Marco, Cano-Ott Daniel, Casanovas Adria, Cerutti Francesco, Cortés Guillem, Cortés-Giraldo Miguel, Cosentino Luigi, Cristallo Sergio, Damone Lucia-Anna, Davies Paul-John, Dietz Mirco, Domingo-Pardo César, Dressler Rugard, Ducasse Quentin, Dupont Emmeric, Durán Ignacio, Fernández-Domínguez Beatriz, Ferrari Alfredo, Finocchiaro Paolo, Göbel Kathrin, Garg Ruchi, Gawlik-Ramięga Aleksandra, Gilardoni Simone, Gonçalves Isabel, González-Romero Enrique, Guerrero Carlos, Gunsing Frank, Harada Hideo, Heinitz Stephan, Jenkins David, Junghans Arnd, Käppeler† Franz, Kadi Yacine, Kimura Atsushi, Knapová Ingrid, Krtička Milan, Kurtulgil Deniz, Ladarescu Ion, Lederer-Woods Claudia, Leeb Helmut, Lerendegui-Marco Jorge, Lonsdale Sarah-Jane, Manna Alice, Martínez Trinitario, Masi Alessandro, Massimi Cristian, Mastinu Pierfrancesco, Mastromarco Mario, Maugeri Emilio-Andrea, Mazzone Annamaria, Mendoza Emilio, Mengoni Alberto, Milazzo Paolo, Mingrone Federica, Moreno-Soto Javier, Musumarra Agatino, Negret Alexandru, Nolte Ralf, Ogállar Francisco, Oprea Andreea, Pavlik Andreas, Perkowski Jarosław, Piersanti Luciano, Petrone Cristina, Pirovano Elisa, Porras Ignacio, Praena Javier, Quesada José-Manuel, Ramos-Doval Diego, Rauscher Thomas, Reifarth René, Rochman Dimitri, Rubbia Carlo, Sabaté-Gilarte Marta, Saxena Alok, Schumann Dorothea, Sekhar Adhitya, Smith Gavin, Sosnin Nikolay, Sprung Peter, Tagliente Giuseppe, Tain José, Tarifeño-Saldivia Ariel, Thomas Benedikt, Torres-Sánchez Pablo, Ulrich Jiri, Valenta Stanislav, Vannini Gianni, Variale Vincenzo, Vaz Pedro, Ventura Alberto, Vescovi Diego, Vlachoudis Vasilis, Wallner Anton, Woods Philip-John, Wright Tobias, and Žugec Petar
Subjects: Physics, QC1-999
Abstract: Neutron cross section measurements are often made relative to a neutron cross section standard. Thus, the accuracy of the neutron standards determines the best possible accuracy of the neutron measurements. The 235U(n,f) cross section is widely used as reference, while it is considered a standard at thermal point and between 0.15 to 200 MeV. For this reason, additional cross section data for the 235U(n,f) reaction are useful in order to improve the accuracy and to extend the energy range of the standard. In this work, preliminary results of the measurement of the 235U(n,f) cross-section relative to the standard 10B(n,a) reaction are presented. The high accuracy measurement was performed at the experimental area EAR-1 of the n_TOF facility at CERN, aiming at covering the energy range from the thermal region up to approximately 100 keV. The samples were produced at JRC-Geel in Belgium, while the experimental setup was based on Micromegas detectors.
Published: 2023
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2. The expected evolution of the binary system PTF J2238+743015.1

Author: Piersanti, Luciano, Yungelson, Lev R., and Bravo, Eduardo
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Binary systems made by a low-mass CO WD and a He-donor represent possible progenitors of explosive events via He-detonation, producing low-luminosity thermonuclear Supernovae with a peculiar nucleosynthetis. Recently, the binary system PTF J223857.11+743015.1 has been suggested as one. We investigate the evolution of the PTF J223857.11+743015.1 system, composed by a 0.75Msun CO WD and a 0.390Msun subdwarf, capped by a thin H-rich layer, considering rotation of the WD component. We compute the evolution of two stars simultaneously, accounting for the possible evolution of the orbital parameters, as determined by mass transfer between components and by mass ejection from the system during RLOF episodes. We consider that the WD gains angular momentum due to accretion and we follow the evolution of the angular velocity profile as due to angular momentum transport via convection and rotation-induced instabilities. As the donor H-rich envelope is transferred, the WD experiences recurrent very strong H-flashes triggering RLOF episodes during which the entire accreted matter is lost from the system. Due to mixing of chemicals by rotation-induced instabilities during the accretion phase, H-flashes occur inside the original WD. Hence, pulse-by pulse, the accretor mass is reduced down to 0.7453Msun. When He-rich matter is transferred, He-detonation does not occur in the rotating WD, which undergoes 6 very strong He-flashes and subsequent RLOF episodes. Also in this case, due to rotation-induced mixing of the accreted layers with the underlying core, the WD is eroded. Finally, when the mass transfer rate from the donor decreases, a massive He-buffer is piled-up onto the accretor which ends its life as a cooling WD. The binary system PTF J2238+743015.1 as all those binaries having similar components masses and orbital parameters are not good candidates as thermonuclear explosions progenitors., Comment: 12 Pages, 9 Figures, 3 Tables. Accepted for the publication on A&A
Published: 2024

3. Type Ia SN progenitors: pre-explosion phase in nearly Chandrasekhar mass WDs

Author: Domínguez Inma, Piersanti Luciano, Bravo Eduardo, Straniero Oscar, and Cristallo Sergio
Subjects: Physics, QC1-999
Abstract: Type Ia supernovae are used as distance indicators to measure the expansion rate of the Universe and to constrain the nature of dark energy. Current and upcoming surveys will allow to extend supernova Hubble diagrams to higher redshifts and to improve further their statistics. It is accepted that Type Ia supernovae are thermonuclear explosions of carbon-oxygen white dwarfs in binary systems. However, the identification of their progenitors, the evolutionary path leading to the explosion and the explosion mechanism itself have not been identified yet. This is critical, as we need to understand the potential evolution of their luminosity with cosmic time and, thus, with their stellar progenitors. We will review the current situation, considering observational hints. We will focus on our recent models, that follow the evolution of carbon-oxygen white dwarfs accreting mass up to thermonuclear runaway, and on their dependence with the initial metallicity of the white dwarf progenitors.
Published: 2022
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4. Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints

Author: Bravo, Eduardo, Piersanti, Luciano, Blondin, Stéphane, Domínguez, Inma, Straniero, Oscar, and Cristallo, Sergio
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The precise progenitor system of type Ia supernovae (SNe Ia), whether it is a white dwarf (WD) close to the Chandrasekhar limit or substantially less massive, has been a matter of debate for decades. Recent research by our group on the accretion and simmering phases preceding the explosion of a massive WD has shown that the central density at thermal runaway lies in the range $(3.6-6.3)\times10^9$ g cm$^{-3}$ for reasonable choices of accretion rate onto the WD and progenitor metallicity. In this work, we have computed one-dimensional simulations of the explosion of such WDs, with special emphasis on the chemical composition of the ejecta, which in all cases is extremely rich in neutronized isotopes of chromium ($^{54}$Cr) and titanium ($^{50}$Ti). We show that, in order to reconcile such a nucleosynthesis with the isotopic abundances of the Solar System, Chandrasekhar-mass white dwarfs can account for at most 26 per cent of normal-luminosity SNe Ia, or at most 20 per cent of all SNe Ia., Comment: 5 pages, 1 table, 3 figures; Letter accepted by MNRAS
Published: 2022
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5. Neutron-captures in Low Mass Stars and the Early Solar System Record of Short-lived Radioactivities

Author: Busso Maurizio, Vescovi Diego, Trippella Oscar, Palmerini Sara, Cristallo Sergio, and Piersanti Luciano
Subjects: Physics, QC1-999
Abstract: Noticeable improvements were recently introduced in the modelling of n-capture nucleosynthesis in the advanced evolutionary stages of giant stars (Asymptotic Giant Branch, or AGB, stars). Two such improvements are closely linked together and concern the introduction of non-parameterized, physical models for extended mixing processes and the adoption of accurate reaction rates for H- and He-burning reactions, including the one for the main neutron source 13C(α,n)16O. These improvements profited of a longstanding collaboration between stellar physicists and C. Spitaleri’s team and of his seminal work both as a leader in the Nuclear Astrophysics scenario and as a talent-scout in the recruitment of young researchers in the field. We present an example of the innovative results that can be obtained thanks to the novelties introduced, by estimating the contributions from a nearby AGB star to the synthesis of short-lived (t1/2 ≤ 10 Myr) radioactive nuclei which were alive in early Solar System condensates. We find that the scenario indicating an AGB star as the source of such radioactivities, discussed for many years by researchers in this field, appears now to be no longer viable, when the mentioned improvements of AGB models and nuclear parameters are considered.
Published: 2017
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6. Pre-explosive accretion and simmering phases of Type Ia Supernovae

Author: Piersanti, Luciano, Bravo, Eduardo, Straniero, Oscar, Cristallo, Sergio, and Dominguez, Inmaculada
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In accreting WDs approaching the Chandrasekhar limit, hydrostatic carbon burning precedes the dynamical breakout. During this \textit{simmering} phase, $e-$captures are energetically favored in the central region of the star, while $\beta-$decays are favored more outside, and the two zones are connected by a growing convective instability. We analyze the interplay between weak interactions and convection, the so-called convective URCA process, during the simmering phase of SNe Ia progenitors and its effects on the physical and chemical properties at the explosion epoch. At variance with previous studies, we find that the convective core powered by the carbon burning remains confined within the ${^{21}(Ne,F)}$ URCA shell. As a result, a much larger amount of carbon has to be consumed before the explosion which eventually occurs at larger density than previously estimated. In addition, we find that the extension of the convective core and its average neutronization depend on the the WD progenitor initial metallicity. For the average neutronization in the convective core at the explosion epoch we obtain ${\overline{\eta}_{exp}} = (1.094\pm 0.143)\times 10^{-3} + (9.168\pm 0.677)\times 10^{-2}\times Z$. Outside the convective core, the neutronization is instead determined by the initial amount of C+N+O in the progenitor star. Since S, Ca, Cr and Mn, the elements usually exploited to evaluate the pre-explosive neutronization, are mainly produced outside the heavily neutronized core, the problem of too high metallicity estimated for the progenitors of the historical Tycho and Kepler SNe Ia remains unsolved., Comment: Accepted for the publication on ApJ. 26 pages, 11 figures, 5 Tables. Modified acknowledgments
Published: 2021
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7. On the mass and metallicity distribution of parent AGB stars of presolar SiC

Author: Cristallo, Sergio, Nanni, Ambra, Cescutti, Gabriele, Minchev, Ivan, Liu, Nan, Vescovi, Diego, Gobrecht, David, and Piersanti, Luciano
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The vast majority (>=90%) of presolar SiC grains identified in primitive meteorites are relics of ancient asymptotic giant branch (AGB) stars, whose ejecta were incorporated into the Solar System during its formation. Detailed characterization of these ancient stardust grains has revealed precious information on mixing processes in AGB interiors in great detail. However, the mass and metallicity distribution of their parent stars still remains ambiguous, although such information is crucial to investigating the slow neutron capture process, whose efficiency is mass- and metallicity-dependent. Using a well-known Milky Way chemo-dynamical model, we follow the evolution of the AGB stars that polluted the Solar System at 4.57 Gyr ago and weighted the stars based on their SiC dust productions. We find that presolar SiC in the Solar System predominantly originated from AGB stars with M~2 Msun and Z~Zsun. Our finding well explains the grain-size distribution of presolar SiC identified in situ in primitive meteorites. Moreover, it provides complementary results to very recent papers dealing with the characterization of parent stars of presolar SiC., Comment: Accepted for publication on Astronomy & Astrophjysics
Published: 2020
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8. The luminosity constraint in the era of precision solar physics

Author: Vescovi, Diego, Mascaretti, Carlo, Vissani, Francesco, Piersanti, Luciano, and Straniero, Oscar
Subjects: Astrophysics - Solar and Stellar Astrophysics, High Energy Physics - Phenomenology, Nuclear Experiment, Nuclear Theory
Abstract: The luminosity constraint is a very precise relationship linking the power released by the Sun as photons and the solar neutrino fluxes. Such a relation, which is a direct consequence of the physical processes controlling the production and the transport of energy in the solar interior, is of great importance for the studies of solar neutrinos and has a special role for the search of neutrinos from the CNO cycle, whose first detection with a 5$\sigma$ significance has been recently announced by the Borexino collaboration. Here we revise the luminosity constraint, discussing and validating its underlying hypotheses, in the light of latest solar neutrino and luminosity measurements. We generalize the current formulation of the luminosity constraint relation so that it can be easily used in future analysis of solar neutrino data, and we provide a specific application showing the link between CNO and pp neutrino fluxes., Comment: 24 pages, 3 figures, 7 tables. Accepted for publication in JPhG
Published: 2020
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9. A high-precision abundance analysis of the nuclear benchmark star HD 20

Author: Hanke, Michael, Hansen, Camilla Juul, Ludwig, Hans-Günter, Cristallo, Sergio, McWilliam, Andrew, Grebel, Eva K., and Piersanti, Luciano
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present our chemical abundance investigation of the metal-poor ([Fe/H]=-1.60 dex), r-process-enriched ([Eu/Fe]=0.73 dex) halo star HD 20 using novel and archival high-resolution spectra at outstanding signal-to-noise ratios. By combining one of the first asteroseismic gravity measurements in the metal-poor regime from a TESS light curve with non-LTE analyses of iron lines, we derive a set of highly accurate and precise stellar parameters. These allow us to delineate a chemical pattern comprised of solid detections of 48 elements, including 28 neutron-capture elements, which establishes HD 20 among the few benchmark stars that have almost complete patterns with low systematic dependencies on the stellar parameters. Our light-element (Z<30) abundances are representative of other, similarly metal-poor stars in the Galactic halo with contributions from core-collapse supernovae of type II. A comparison to the scaled solar r-pattern shows that the lighter neutron-capture elements (37
Published: 2020
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10. Comprehensive models of novae at metallicity $Z = 0.02$ and $Z = 10^{-4}$

Author: Chen, Hai-Liang, Woods, T. E., Yungelson, L. R., Piersanti, Luciano, Gilfanov, M., and Han, Zhanwen
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Novae are the observational manifestations of thermonuclear runaways on the surface of accreting white dwarfs (WDs). Although novae are an ubiquitous phenomenon, their properties at low metallicity are not well understood. Using the publicly-available stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA), we model the evolution of accreting carbon-oxygen WDs and consider models which accrete matter with metallicity Z=0.02 or $10^{-4}$. We consider both models without mixing and with matter enriched by CO-elements assuming that mixing occurs in the process of accretion (with mixing fraction 0.25). We present and contrast ignition mass, ejected mass, recurrence period and maximum luminosity of novae for different WD masses and accretion rates for these metallicities and mixing cases. We find that models with Z = 0.02 have ignition masses and recurrence periods smaller than models with low Z, while the ejected mass and maximum luminosity are larger. Retention efficiency during novae outbursts decreases with increasing metallicity. In our implementation, inclusion of mixing at the H/He interface reduces accreted mass, ejected mass and recurrence period as compared to the no-mixing case, while the maximum luminosity becomes larger. Retention efficiency is significantly reduced, becoming negative in most of our models. For ease of use, we provide a tabular summary of our results., Comment: Accepted by MNRAS, 18 pages, 13 figures
Published: 2019
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11. The initial mass-final luminosity relation of type II supernova progenitors. Hints of new physics?

Author: Straniero, Oscar, Dominguez, Inma, Piersanti, Luciano, Giannotti, Maurizio, and Mirizzi, Alessandro
Subjects: Astrophysics - Solar and Stellar Astrophysics, High Energy Physics - Phenomenology
Abstract: We revise the theoretical initial mass-final luminosity relation for progenitors of type IIP and IIL supernovae. The effects of the major uncertainties, as those due to the treatment of convection, semiconvection, rotation, mass loss, nuclear reaction rates and neutrinos production rates are discussed in some details. The effects of mass transfer between components of close-binary systems are also considered. By comparing the theoretical predictions to a sample of type II supernovae for which the initial mass of the progenitors and the pre-explosive luminosity are available, we conclude that stellar rotation may explain a few progenitors which appear brighter than expected in case of non-rotating models. In the most extreme case, SN2012ec, an initial rotational velocity up to 300 km s$^{-1}$ is required. Alternatively, these objects could be mass-loosing components of close binaries. However, most of the observed progenitors appear fainter than expected. This occurrence seems to indicate that the Compton and pair neutrino energy-loss rates, as predicted by the standard electro-weak theory, are not efficient enough and that an additional negative contribution to the stellar energy balance is required. We show that axions coupled with parameters accessible to currently planned experiments, such as IAXO and, possibly, Baby-IAXO and ALPS II, may account for the missing contribution to the stellar energy-loss., Comment: paper accepted to be publiished on ApJ
Published: 2019
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12. On the mass of supernova progenitors: the role of the $^{12}$C$+^{12}$C reaction

Author: Straniero, Oscar, Piersanti, Luciano, Dominguez, Inmaculata, and Tumino, Aurora
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: A precise knowledge of the masses of supernova progenitors is essential to answer various questions of modern astrophysics, such as those related to the dynamical and chemical evolution of Galaxies. In this paper we revise the upper bound for the mass of the progenitors of CO white dwarfs (\mup) and the lower bound for the mass of the progenitors of normal type II supernovae (\mups). In particular, we present new stellar models with mass between 7 and 10 \msun, discussing their final destiny and the impact of recent improvements in our understanding of the low energy rate of the \c12c12 reaction., Comment: To be published on the proceedings of NIC 2018
Published: 2019
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13. Observational Properties of SNe Ia Progenitors Close to the Explosion

Author: Tornambe', Amedeo, Piersanti, Luciano, Raimondo, Gabriella, and Delgrande, Raffaele
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We determine the expected signal in various observational bands of Supernovae Ia progenitors just before the explosion by assuming the rotating Double Degenerate scenario. Our results are valid also for all the evolutionary scenarios invoking rotation as the driving mechanism of the accretion process as well as the evolution up to the explosion. We find that the observational properties depend mainly on the mass of the exploding object, even if the angular momentum evolution after the end of the mass accretion phase and before the onset of C-burning plays a non-negligible role. Just before the explosion the magnitude M_V ranges between 9 and 11 mag, while the colour (F225W-F555W) is about -1.64 mag. The photometric properties remain constant for a few decades before the explosion. During the last few months the luminosity decreases very rapidly. The corresponding decline in the optical bands varies from few hundredths up to one magnitude, the exact value depending on both the WD total mass and the braking efficiency at the end of the mass transfer. This feature is related to the exponentially increasing energy production which drives the formation of a convective core rapidly extending over a large part of the exploding object. Also a drop in the angular velocity occurs. We find that observations in the soft X band (0.5 -2 keV) may be used to check if the SNe Ia progenitors evolution up to explosion is driven by rotation and, hence, to discriminate among different progenitor scenarios., Comment: 8 pages, 6 figures, 2 tables. Accepted for the publication on MNRAS
Published: 2017
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14. Nucleation of small silicon carbide dust clusters in AGB stars

Author: Gobrecht, David, Cristallo, Sergio, Piersanti, Luciano, and Bromley, Stefan T.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Silicon carbide (SiC) grains are a major dust component in carbon-rich AGB stars. The formation pathways of these grains are, however, not fully understood.\ We calculate ground states and energetically low-lying structures of (SiC)$_n$, $n=1,16$ clusters by means of simulated annealing (SA) and Monte Carlo simulations of seed structures and subsequent quantum-mechanical calculations on the density functional level of theory. We derive the infrared (IR) spectra of these clusters and compare the IR signatures to observational and laboratory data.\ According to energetic considerations, we evaluate the viability of SiC cluster growth at several densities and temperatures, characterising various locations and evolutionary states in circumstellar envelopes.\ We discover new, energetically low-lying structures for Si$_{4}$C$_{4}$, Si$_{5}$C$_{5}$, Si$_{15}$C$_{15}$ and Si$_{16}$C$_{16}$, and new ground states for Si$_{10}$C$_{10}$ and Si$_{15}$C$_{15}$. The clusters with carbon-segregated substructures tend to be more stable by 4-9 eV than their bulk-like isomers with alternating Si-C bonds. However, we find ground states with cage ("bucky"-like) geometries for Si$_{12}$C$_{12}$ and Si$_{16}$C$_{16}$ and low-lying, stable cage structures for n $\ge$ 12. The latter findings indicate thus a regime of clusters sizes that differs from small clusters as well as from large-scale crystals. Thus, and owing to their stability and geometry, the latter clusters may mark a transition from a quantum-confined cluster regime to crystalline, solid bulk-material. The calculated vibrational IR spectra of the ground-state SiC clusters shows significant emission. They include the 10-13 $\mu$m wavelength range and the 11.3 $\mu$m feature inferred from laboratory measurements and observations, respectively, though the overall intensities are rather low., Comment: 16 pages, 25 figures, 3 tables, accepted for publication in ApJ
Published: 2017
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15. Type Ia Supernovae keep memory of their progenitor metallicity

Author: Piersanti, Luciano, Bravo, Eduardo, Cristallo, Sergio, Dominguez, Inmaculada, Straniero, Oscar, Tornambe', Amedeo, and Martinez-Pinedo, Gabriel
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The ultimate understanding of Type Ia Supernovae diversity is one of the most urgent issues to exploit thermonuclear explosions of accreted White Dwarfs (WDs) as cosmological yardsticks. In particular, we investigate the impact of the progenitor system metallicity on the physical and chemical properties of the WD at the explosion epoch. We analyze the evolution of CO WDs through the accretion and simmering phases by using evolutionary models based on time-dependent convective mixing and an extended nuclear network including the most important electron captures, beta decays and URCA processes. We find that, due to URCA processes and electron-captures, the neutron excess and density at which the thermal runaway occurs are substantially larger than previously claimed. Moreover, we find that the higher the progenitor metallicity, the larger the neutron excess variation during the accretion and simmering phases and the higher the central density and the convective velocity at the explosion. Hence, the simmering phase acts as an amplifier of the differences existing in SNe Ia progenitors. When applying our results to the neutron excess estimated for the Tycho and Kepler young Supernova remnants, we derive that the metallicity of the progenitors should be in the range Z=0.030-0.032, close to the average metallicity value of the thin disk of the Milky Way. As the amount of ${^{56}}$Ni produced in the explosion depends on the neutron excess and central density at the thermal runaway, our results suggest that the light curve properties depend on the progenitor metallicity., Comment: 7 pages, 3 figures, 2 tables, accepted for the publication on ApJ Letter
Published: 2017
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16. He-Accreting WDs: AM CVn stars with WD Donors

Author: Piersanti, Luciano, Yungelson, Lev R., and Tornambe', Amedeo
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We study the physical and evolutionary properties of the "WD family" of AM CVn stars by computing realistic models of IDD systems. We evaluate self-consistently both the mass transfer rate from the donor, as determined by GW emission and interaction with the binary companion, and the thermal response of the accretor to mass deposition. We find that, after the onset of mass transfer, all the considered systems undergo a strong non-dynamical He-flash. However, due to the compactness of these systems, the expanding accretors fill their Roche lobe very soon, thus preventing the efficient heating of the external layers of the accreted CO WDs. Moreover, due to the loss of matter from the systems, the orbital separations enlarge and mass transfer comes to a halt. The further evolution depends on the value of $\dot{M}$, after the donors fill again their lobe. On one hand, if the accretion rate, as determined by the actual value of (M$_{don}$,M$_{acc}$), is high enough, the accretors experience several He-flashes of decreasing strength and then quiescent He-burning sets in. Later on, since the mass transfer rate in IDD is a permanently decreasing function of time, accretors experience several recurrent strong flashes. On the other hand, for intermediate and low values of $\dot{M}$, the accretors enter the strong flashes accretion regime. As expected, in all the considered systems the last He-flash is the strongest one, even if a dynamical event never occurs. When the mass accretion rate decreases below (2-3)$\times 10^{-8} M_\odot yr^{-1}$, the compressional heating of the He-shell becomes less efficient than the neutrino cooling, so that all the accretors in the considered systems evolve into massive degenerate objects. Our results suggest that SNe .Ia or type Ia Supernovae due to Edge-Lit Detonation in the WD family of AM CVn stars should be much more rare than previously expected., Comment: 14 pages, 13 figures, 3 tables. Accepted for the publication on MNRAS. Corrected typos in the Abstract
Published: 2015
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17. On the need of the Light Elements Primary Process (LEPP)

Author: Cristallo, Sergio, Abia, Carlos, Straniero, Oscar, and Piersanti, Luciano
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Extant chemical evolution models underestimate the Galactic production of Sr, Y and Zr as well as the Solar System abundances of s-only isotopes with 904.0 M_SUN) are negligible; 4) the inclusion of rotation implies a downward shift of the whole distribution with an higher efficiency for the heavy s-only isotopes, leading to a flatter s-only distribution; 5) different prescriptions on convection or mass-loss produce nearly rigid shifts of the whole distribution. In summary, a variation of the standard paradigm of AGB nucleosynthesis would allow to reconcile models predictions with Solar System s-only abundances. Nonetheless, the LEPP cannot be definitely ruled out, because of the uncertainties still affecting stellar and Galactic chemical evolution models., Comment: Accepted for publication on ApJ
Published: 2015
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18. TOF Facility at CERN

Author: The n_TOF Collaboration, Damone, L. A., Barbagallo, M., Mastromarco, M., Mengoni, A., Colonna, N., Cosentino, L., Maugeri, E. A., Heinitz, S., Schumann, D., Dressler, R., Käppeler, F., Finocchiaro, P., Andrzejewski, J., Perkowski, J., Gawlik, A., Aberle, O., Altstadt, S., Ayranov, M., Audouin, L., Bacak, M., Balibrea-Correa, J., Ballof, J., Bcares, V., Bečvař, F., Beinrucker, C., Bellia, G., Bernardes, A. P., Berthoumieux, E., Billowes, J., Borge, M. J. G., Bosnar, D., Brown, A., Brugger, M., Busso, Maurizio, Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Castelluccio, D. M., Catherall, R., Cerutti, F., Chen, Y. H., Chiaveri, E., Corts, G., Cortès-Giraldo, M. A., Cristallo, Sergio, Diakaki, M., Dietz, M., Domingo-Pardo, C., Dorsival, A., Dupont, E., Durán, I., Fernàndez-Dominguez, B., Ferrari, A., Ferreira, P., Furman, W., Ganesan, S., Garca-Rios, A., Gilardoni, S., Glodariu, T., Göbel, Kathrin, Gonçalves, I. F., Gonzalez-Romero, E., Goodacre, T. D., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heftrich, Tanja, Heyse, J., Jenkins, D. G., Jericha, E., Johnston, K., Kadi, Y., Kalamara, A., Katabuchi, T., Kavrigin, P., Kimura, A., Kivel, N., Kohester, U., Kokkoris, M., Krtička, M., Kurtulgil, Deniz, Leal-Cidoncha, E., Lederer-Woods, Claudia, Leeb, H., Lerendegui-Marco, J., Lo Meo, S., Lonsdale, S. J., Losito, R., Macina, D., Marganiec, J., Marsh, B., Martínez, T., Martins Correia, J. G., Masi, A., Massimi, C., Mastinu, P., Matteucci, F., Mazzone, A., Mendoza, E., Milazzo, P. M., Mingrone, Federica, Mirea, M., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Piersanti, Luciano, Piscopo, M., Plompen, A., Porras, I., Praena, J., Quesada, J. M., Radeck, D., Rajeev, K., Rauscher, Thomas, Reifarth, René, Riego-Perez, A., Rothe, S., Rout, P., Rubbia, C., Ryan, J., Sabaté-Gilarte, M., Saxena, A., Schell, J., Schillebeeckx, P., Schmidt, S., Sedyshev, P., Seiffert, C., Smith, A. G., Sosnin, N. V., Stamatopoulos, A., Stora, T., Tagliente, G., Tain, J. L., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weigand, Mario, Weiß, C., Wolf, C., Woods, P. J., Wright, T., Žugec, P., Formicola, Alba, editor, Junker, Matthias, editor, Gialanella, Lucio, editor, and Imbriani, Gianluca, editor
Published: 2019
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19. Data for the s Process from n_TOF

Author: The n_TOF Collaboration, Massimi, C., Aberle, O., Alcayne, V., Andrzejewski, J., Audouin, L., Bécares, V., Babiano-Suarez, V., Bacak, M., Barbagallo, M., Benedikt, Th., Bennett, S., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Busso, Maurizio, Caamaño, M., Caballero-Ontanaya, L., Calviño, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chiaveri, E., Clai, G., Colonna, N., Cortés, G., Cortès-Giraldo, M. A., Cosentino, L., Cristallo, Sergio, Damone, L. A., Davies, P. J., Dietz, M., Domingo-Pardo, C., Dressler, R., Ducasse, Q., Dupont, E., Durán, I., Eleme, Z., Fernàndez-Dominguez, B., Ferrari, A., Finocchiaro, P., Furman, V., Göbel, Kathrin, Gawlik, A., Gilardoni, S., Gonçalves, I. F., González-Romero, E., Guerrero, C., Gunsing, F., Heinitz, S., Heyse, J., Jenkins, D. G., Junghans, Arnd R., Käppeler, F., Kadi, Y., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krtička, M., Kurtulgil, Deniz, Ladarescu, I., Lederer-Woods, Claudia, Lonsdale, S. J., Macina, D., Manna, A., Martínez, T., Masi, A., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, Federica, Moreno-Soto, J., Musumarra, A., Negret, A., Ogállar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Piersanti, Luciano, Petrone, C., Pirovano, E., Porras, I., Praena, J., Quesada, J. M., Ramos-Doval, D., Rauscher, Thomas, Reifarth, René, Rochman, D., Sabaté-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Simone, S., Smith, A. G., Sosnin, N. V., Sprung, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Ulrich, J., Urlass, Sebastian, Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vescovi, Diego, Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Žugec, P., Formicola, Alba, editor, Junker, Matthias, editor, Gialanella, Lucio, editor, and Imbriani, Gianluca, editor
Published: 2019
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20. Heavy elements in Globular Clusters: the role of AGB stars

Author: Straniero, Oscar, Cristallo, Sergio, and Piersanti, Luciano
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Recent observations of heavy elements in Globular Clusters reveal intriguing deviations from the standard paradigm of the early galactic nucleosynthesis. If the r-process contamination is a common feature of halo stars, s-process enhancements are found in a few Globular Clusters only. We show that the combined pollution of AGB stars with mass ranging between 3 to 6 M$_\odot$ may account for most of the features of the s-process overabundance in M4 and M22. In these stars, the s process is a mixture of two different neutron-capture nucleosynthesis episodes. The first is due to the 13C(a,n)16O reaction and takes place during the interpulse periods. The second is due to the 22Ne(a,n)25Mg reaction and takes place in the convective zones generated by thermal pulses. The production of the heaviest s elements (from Ba to Pb) requires the first neutron burst, while the second produces large overabundances of light s (Sr, Y, Zr). The first mainly operates in the less-massive AGB stars, while the second dominates in the more-massive. From the heavy-s/light-s ratio, we derive that the pollution phase should last for $150\pm 50$ Myr, a period short enough compared to the formation timescale of the Globular Cluster system, but long enough to explain why the s-process pollution is observed in a few cases only. With few exceptions, our theoretical prediction provides a reasonable reproduction of the observed s-process abundances, from Sr to Hf. However, Ce is probably underproduced by our models, while Rb and Pb are overproduced. Possible solutions are discussed., Comment: Accepted by the ApJ
Published: 2014
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21. He-accreting WDs as SNe Ia Progenitors

Author: Piersanti, Luciano, Tornambe', Amedeo, Yungelson, Lev, and Straniero, Oscar
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We investigate the thermal response of CO WDs accreting He-rich matter directly from their companions in binary systems. Our results suggest that the He-channel cannot provide progenitors for majority of "normal" SNe Ia., Comment: 4 pages, 3 figures, contribution to the Proceeding of IAU 281 "Binary Paths to Type Ia Supernovae Explosions"
Published: 2011

22. Evolution, nucleosynthesis and yields of low mass AGB stars at different metallicities (II): the FRUITY database

Author: Cristallo, Sergio, Piersanti, Luciano, Straniero, Oscar, Gallino, Roberto, Dominguez, Inma, Abia, Carlos, DiRico, Gianluca, Quintini, Massimo, and Bisterzo, Sara
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: By using updated stellar low mass stars models, we can systematically investigate the nucleosynthesis processes occurring in AGB stars, when these objects experience recurrent thermal pulses and third dredge-up episodes. In this paper we present the database dedicated to the nucleosynthesis of AGB stars: the FRUITY (FRANEC Repository of Updated Isotopic Tables & Yields) database. An interactive web-based interface allows users to freely download the full (from H to Bi) isotopic composition, as it changes after each third dredge-up episode and the stellar yields the models produce. A first set of AGB models, having masses in the range 1.5 < M/Msun < 3.0 and metallicities 1e-3 < Z < 2e-2, is discussed here. For each model, a detailed description of the physical and the chemical evolution is provided. In particular, we illustrate the details of the s-process and we evaluate the theoretical uncertainties due to the parametrization adopted to model convection and mass loss. The resulting nucleosynthesis scenario is checked by comparing the theoretical [hs/ls] and [Pb/hs] ratios to those obtained from the available abundance analysis of s-enhanced stars. On the average, the variation with the metallicity of these spectroscopic indexes is well reproduced by theoretical models, although the predicted spread at a given metallicity is substantially smaller than the observed one. Possible explanations for such a difference are briefly discussed. An independent check of the third dredge-up efficiency is provided by the C-stars luminosity function. Consequently, theoretical C-stars luminosity functions for the Galactic disk and the Magellanic Clouds have been derived. We generally find a good agreement with observations., Comment: Accepted for Publication on The Astrophysical Journal Supplements
Published: 2011
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23. Carbon-Oxygen White Dwarfs Accreting CO-Rich Matter I: A Comparison Between Rotating and Non-Rotating Models

Author: Piersanti, Luciano, Gagliardi, Simona, Iben Jr, Icko, and Tornambe', Amedeo
Subjects: Astrophysics
Abstract: We investigate the lifting effect of rotation on the thermal evolution of CO WDs accreting CO-rich matter. We find that rotation induces the cooling of the accreting star so that the delivered gravitational energy causes a greater expansion with respect to the standard non-rotating case. The increase in the surface radius produces a decrease in the surface value of the critical angular velocity and, therefore, the accreting WD becomes gravitationally unbound (Roche instability). This occurrence is due to an increase in the total angular momentum of the accreting WD and depends critically on the amount of specific angular momentum deposited by the accreted matter. If the specific angular momentum of the accreted matter is equal to that of the outer layers of the accreting structure, the Roche instability occurs well before the accreting WD can attain the physical conditions for C-burning. If the values of both initial angular velocity and accretion rate are small, we find that the accreting WD undergoes a secular instability when its total mass approaches 1.4 Msun. At this stage, the ratio between the rotational and the gravitational binding energy of the WD becomes of the order of 0.1, so that the star must deform by adopting an elliptical shape. In this case, since the angular velocity of the WD is as large as 1 rad/s, the anisotropic mass distribution induces the loss of rotational energy and angular momentum via GWR. We find that, independent of the braking efficiency, the WD contracts and achieves the physical conditions suitable for explosive C-burning at the center so that a type Ia supernova event is produced., Comment: 39 pages, 22 eps-figures; accepted for publication in Astrophysical Journal
Published: 2002
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24. The chemical composition of White Dwarfs as a test of convective efficiency during core He-burning

Author: Straniero, Oscar, Dominguez, Inma, Imbriani, Gianluca, and Piersanti, Luciano
Subjects: Astrophysics
Abstract: Pulsating white dwarfs provide constraints to the evolution of progenitor stars. We revise He-burning stellar models, with particular attention to core convection and to its connection with the nuclear reactions powering energy generation and chemical evolution Theoretical results are compared to the available measurements for the variable white dwarf GD 358, which indicate a rather large abundance of central oxygen. We show that the attempt to constrain the relevant nuclear reaction rate by means of the white dwarf composition is faced with a large degree of uncertainty related to evaluating the efficiency of convection-induced mixing.By combining the uncertainty of the convection theory with the error on the relevant reaction rate we derive that the present theoretical prediction for the central oxygen mass fraction in white dwarfs varies between 0.3 and 0.9. Unlike previous claims, we find that models taking into account semiconvection and a moderate C12(alpha,gamma)O16 reaction rate are able to account for a high central oxygen abundance. The rate of the C12(alpha,gamma)O16 used in these models agrees with the one recently obtained in laboratory experiments (Kunz et al. 2002). On the other hand, when semiconvection is inhibited, as in the case of classical models (bare Schwarzschild criterion) or in models with mechanical overshoot, an extremely high rate of the C12(\alpha,\gamma)O16 reaction is needed to account for a large oxygen production. Finally, we show that the apparent discrepancy between our result and those reported in previous studies depends on the method used to avoid the convective runaways (the so called breathing pulses), which are usually encountered in modeling late stage of core He-burning phase., Comment: 19 pages, 4 figures, accepted for publication in The Astrophysical Journal
Published: 2002
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25. The Influence of N14(e-,nu)C14(alpha,gamma)O18 reaction on the He-Ignition in Degenerate Physical Conditions

Author: Piersanti, Luciano, Cassisi, Santi, and Tornambe', Amedeo
Subjects: Astrophysics
Abstract: The importance of NCO chain on the onset of the He-flash in degenerate physical conditions has been reevaluated. We find that low-mass, metal-rich (Z $\ge$ 0.001) structures climbing the Red Giant Branch do never attain the physical conditions suitable for the onset of this chain, while at lower metallicities the energy contribution provided by NCO reaction is too low to affect the onset of the central He-flash. At the same time, our evolutionary models suggest that for a Carbon-Oxygen White Dwarf of mass M_{WD}=0.6 M_sun accreting He-rich matter, directly or as a by-product of an overlying H-burning shell, at rates suitable for a dynamical He-flash, the NCO energy contribution is not able to keep hot enough the He-shell and in turn to avoid the occurrence of a strong electron degeneracy and the ensuing final explosion., Comment: 15 pages, 3 tables, 10 figure, to appear in Ap J
Published: 2001
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26. On the Mass of Supernova Progenitors: The Role of the $$^{12}$$ C $$+^{12}$$ C Reaction

Author: Straniero, Oscar, primary, Piersanti, Luciano, additional, Dominguez, Inma, additional, and Tumino, Aurora, additional
Published: 2019
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27. Chandrasekhar-mass white dwarfs are the progenitors of a small fraction of Type Ia supernovae according to nucleosythesis constraints

Author: Bravo, Eduardo, primary, Piersanti, Luciano, additional, Blondin, Stéphane, additional, Domínguez, Inma, additional, Straniero, Oscar, additional, and Cristallo, Sergio, additional
Published: 2022
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28. Pre-explosive Accretion and Simmering Phases of SNe Ia

Author: Piersanti, Luciano, primary, Bravo, Eduardo, additional, Straniero, Oscar, additional, Cristallo, Sergio, additional, and Domínguez, Inmaculada, additional
Published: 2022
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29. Extremely Metal-Poor Asymptotic Giant Branch Stars

Author: Cirillo, Mario, primary, Piersanti, Luciano, additional, and Straniero, Oscar, additional
Published: 2022
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30. First results of the 140Ce(n,γ)141Ce cross-section measurement at n_TOF

Author: n_TOF Collaboration, Amaducci, Simone, Colonna, Nicola, Cosentino, Luigi, Cristallo, Sergio, Finocchiaro, Paolo, Krtička, Milan, Massimi, Cristian, Mastromarco, Mario, Mazzone, Annamaria, Mengoni, Alberto, Valenta, Stanislav, Aberle, Oliver, Alcayne, Victor, Andrzejewski, Józef, Audouin, Laurent, Babiano-Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Billowes, Jon, Bosnar, Damir, Brown, Adam, Busso, Maurizio, Caamaño, Manuel, Caballero-Ontanaya, Luis, Calviño, Francisco, Calviani, Marco, Cano-Ott, Daniel, Casanovas, Adria, Cerutti, Francesco, Chiaveri, Enrico, Cortés, Guillem, Cortés-Giraldo, Miguel, Damone, Lucia-Anna, Davies, Paul-John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, Cesar, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández-Domínguez, Beatriz, Ferrari, Alfredo, Furman, Valter, Göbel, Kathrin, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Gonçalves, Isabel, González-Romero, Enrique, Guerrero, Carlos, Gunsing, Frank, Harada, Hideo, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Junghans, Arnd, Käppeler, Franz, Kadi, Yacine, Kimura, Atsushi, Knapova, Ingrid, Kokkoris, Michael, Kopatch, Yuri, Kurtulgil, Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Leeb, Helmut, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martínez, Trinitario, Masi, Alessandro, Mastinu, Pierfrancesco, Maugeri, Emilio-Andrea, Mendoza, Emilio, Michalopoulou, Veatriki, Milazzo, Paolo, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Piersanti, Luciano, Petrone, Cristina, Pirovano, Elisa, Porras, Ignacio, Praena, Javier, Quesada, José-Manuel, Ramos-Doval, Diego, Rauscher, Thomas, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Gavin, Sosnin, Nikolay, Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Tain, José, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Ulrich, Jiri, Urlass, Sebastian, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, PhilipJohn, Wright, Tobias, Žugec, Petar, n_TOF Collaboration, Universidade de Santiago de Compostela. Departamento de Física de Partículas, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. ANT - Advanced Nuclear Technologies Research Group, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, n_TOF, ITA, FRA, DEU, ESP, GRC, Amaducci S., Colonna N., Cosentino L., Cristallo S., Finocchiaro P., Krticka M., Massimi C., Mastromarco M., Mazzone A., Mengoni A., Valenta S., Aberle O., Alcayne V., Andrzejewski J., Audouin L., Babiano-Suarez V., Bacak M., Barbagallo M., Bennett S., Berthoumieux E., Billowes J., Bosnar D., Brown A., Busso M., Caamano M., Caballero-Ontanaya L., Calvino F., Calviani M., Cano-Ott D., Casanovas A., Cerutti F., Chiaveri E., Cortes G., Cortes-Giraldo M., Damone L.-A., Davies P.-J., Diakaki M., Dietz M., Domingo-Pardo C., Dressler R., Ducasse Q., Dupont E., Duran I., Eleme Z., Fernandez-Dominguez B., Ferrari A., Furman V., Gobel K., Garg R., Gawlik A., Gilardoni S., Goncalves I., Gonzalez-Romero E., Guerrero C., Gunsing F., Harada H., Heinitz S., Heyse J., Jenkins D., Junghans A., Kappeler F., Kadi Y., Kimura A., Knapova I., Kokkoris M., Kopatch Y., Kurtulgil D., Ladarescu I., Lederer-Woods C., Leeb H., Lerendegui-Marco J., Lonsdale S.-J., Macina D., Manna A., Martinez T., Masi A., Mastinu P., Maugeri E.-A., Mendoza E., Michalopoulou V., Milazzo P., Mingrone F., Moreno-Soto J., Musumarra A., Negret A., Ogallar F., Oprea A., Patronis N., Pavlik A., Perkowski J., Piersanti L., Petrone C., Pirovano E., Porras I., Praena J., Quesada J.-M., Ramos-Doval D., Rauscher T., Reifarth R., Rochman D., Rubbia C., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Sekhar A., Smith G., Sosnin N., Sprung P., Stamatopoulos A., Tagliente G., Tain J., Tarifeno-Saldivia A., Tassan-Got L., Thomas B., Torres-Sanchez P., Tsinganis A., Ulrich J., Urlass S., Vannini G., Variale V., Vaz P., Ventura A., Vescovi D., Vlachoudis V., Vlastou R., Wallner A., Woods P.J., Wright T., Zugec P., and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: cross-section, Cerium oxide, Capture, General Physics and Astronomy, QC793-793.5, 7. Clean energy, 01 natural sciences, Ce, chemistry.chemical_compound, neutron, $^{140}$Ce, n_TOF, 010303 astronomy & astrophysics, Physics, Deuterated benzene, Elementary particle physics, nucleosynthesis, Cerium, cerium, Cosmic electrodynamics, Atomic physics, Nucleosynthesis, neutron capture, Cross-section, chemistry.chemical_element, Neutron, Scintillator, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 0103 physical sciences, Nuclear Physics - Experiment, ddc:530, 010306 general physics, capture, Nucleosynthesi, Ones electromagnètiques, Física [Àrees temàtiques de la UPC], Electromagnetic waves, Nuclear data, 140Ce, TheoryofComputation_MATHEMATICALLOGICANDFORMALLANGUAGES, chemistry, 13. Climate action, s-process, MACS, Electrodinàmica còsmica
Abstract: The cerium oxide material for this measurement was provided by T. Katabuchi of the Tokyo Institute of Technology., An accurate measurement of the 140Ce(n,g) energy-dependent cross-section was performed at the n_TOF facility at CERN. This cross-section is of great importance because it represents a bottleneck for the s-process nucleosynthesis and determines to a large extent the cerium abundance in stars. The measurement was motivated by the significant difference between the cerium abundance measured in globular clusters and the value predicted by theoretical stellar models. This discrepancy can be ascribed to an overestimation of the 140Ce capture cross-section due to a lack of accurate nuclear data. For this measurement, we used a sample of cerium oxide enriched in 140Ce to 99.4%. The experimental apparatus consisted of four deuterated benzene liquid scintillator detectors, which allowed us to overcome the difficulties present in the previous measurements, thanks to their very low neutron sensitivity. The accurate analysis of the p-wave resonances and the calculation of their average parameters are fundamental to improve the evaluation of the 140Ce Maxwellian-averaged cross-section.
Published: 2021
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31. The Origin of Type Ia Supernovae: A Theoretical Investigation and Observational Evidence

Author: Piersanti, Luciano
Published: 2002
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32. AGB Stars and Their Circumstellar Envelopes: An Operative Approach to Computing Their Atmospheres

Author: Crivellari, Lucio, primary, Cristallo, Sergio, additional, and Piersanti, Luciano, additional
Published: 2021
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33. First Results of the 140Ce(n,γ)141Ce Cross-Section Measurement at n_TOF

Author: Amaducci, Simone, primary, Colonna, Nicola, additional, Cosentino, Luigi, additional, Cristallo, Sergio, additional, Finocchiaro, Paolo, additional, Krtička, Milan, additional, Massimi, Cristian, additional, Mastromarco, Mario, additional, Mazzone, Annamaria, additional, Mengoni, Alberto, additional, Valenta, Stanislav, additional, Aberle, Oliver, additional, Alcayne, Victor, additional, Andrzejewski, Józef, additional, Audouin, Laurent, additional, Babiano-Suarez, Victor, additional, Bacak, Michael, additional, Barbagallo, Massimo, additional, Bennett, Samuel, additional, Berthoumieux, Eric, additional, Billowes, Jon, additional, Bosnar, Damir, additional, Brown, Adam, additional, Busso, Maurizio, additional, Caamaño, Manuel, additional, Caballero-Ontanaya, Luis, additional, Calviño, Francisco, additional, Calviani, Marco, additional, Cano-Ott, Daniel, additional, Casanovas, Adria, additional, Cerutti, Francesco, additional, Chiaveri, Enrico, additional, Cortés, Guillem, additional, Cortés-Giraldo, Miguel, additional, Damone, Lucia-Anna, additional, Davies, Paul-John, additional, Diakaki, Maria, additional, Dietz, Mirco, additional, Domingo-Pardo, Cesar, additional, Dressler, Rugard, additional, Ducasse, Quentin, additional, Dupont, Emmeric, additional, Durán, Ignacio, additional, Eleme, Zinovia, additional, Fernández-Domínguez, Beatriz, additional, Ferrari, Alfredo, additional, Furman, Valter, additional, Göbel, Kathrin, additional, Garg, Ruchi, additional, Gawlik, Aleksandra, additional, Gilardoni, Simone, additional, Gonçalves, Isabel, additional, González-Romero, Enrique, additional, Guerrero, Carlos, additional, Gunsing, Frank, additional, Harada, Hideo, additional, Heinitz, Stephan, additional, Heyse, Jan, additional, Jenkins, David, additional, Junghans, Arnd, additional, Käppeler, Franz, additional, Kadi, Yacine, additional, Kimura, Atsushi, additional, Knapova, Ingrid, additional, Kokkoris, Michael, additional, Kopatch, Yuri, additional, Kurtulgil, Deniz, additional, Ladarescu, Ion, additional, Lederer-Woods, Claudia, additional, Leeb, Helmut, additional, Lerendegui-Marco, Jorge, additional, Lonsdale, Sarah-Jane, additional, Macina, Daniela, additional, Manna, Alice, additional, Martínez, Trinitario, additional, Masi, Alessandro, additional, Mastinu, Pierfrancesco, additional, Maugeri, Emilio-Andrea, additional, Mendoza, Emilio, additional, Michalopoulou, Veatriki, additional, Milazzo, Paolo, additional, Mingrone, Federica, additional, Moreno-Soto, Javier, additional, Musumarra, Agatino, additional, Negret, Alexandru, additional, Ogállar, Francisco, additional, Oprea, Andreea, additional, Patronis, Nikolas, additional, Pavlik, Andreas, additional, Perkowski, Jarosław, additional, Piersanti, Luciano, additional, Petrone, Cristina, additional, Pirovano, Elisa, additional, Porras, Ignacio, additional, Praena, Javier, additional, Quesada, José-Manuel, additional, Ramos-Doval, Diego, additional, Rauscher, Thomas, additional, Reifarth, René, additional, Rochman, Dimitri, additional, Rubbia, Carlo, additional, Sabaté-Gilarte, Marta, additional, Saxena, Alok, additional, Schillebeeckx, Peter, additional, Schumann, Dorothea, additional, Sekhar, Adhitya, additional, Smith, Gavin, additional, Sosnin, Nikolay, additional, Sprung, Peter, additional, Stamatopoulos, Athanasios, additional, Tagliente, Giuseppe, additional, Tain, José, additional, Tarifeño-Saldivia, Ariel, additional, Tassan-Got, Laurent, additional, Thomas, Benedikt, additional, Torres-Sánchez, Pablo, additional, Tsinganis, Andrea, additional, Ulrich, Jiri, additional, Urlass, Sebastian, additional, Vannini, Gianni, additional, Variale, Vincenzo, additional, Vaz, Pedro, additional, Ventura, Alberto, additional, Vescovi, Diego, additional, Vlachoudis, Vasilis, additional, Vlastou, Rosa, additional, Wallner, Anton, additional, Woods, PhilipJohn, additional, Wright, Tobias, additional, and Žugec, Petar, additional
Published: 2021
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34. Group II Oxide Grains: How Massive Are Their AGB Star Progenitors?

Author: Palmerini, Sara, primary, Cristallo, Sergio, additional, Piersanti, Luciano, additional, Vescovi, Diego, additional, and Busso, Maurizio, additional
Published: 2021
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35. Group II oxide grains: how massive are their AGB star progenitors?

Author: Palmerini, Sara, Cristallo, Sergio, Piersanti, Luciano, Vescovi, Diego, Busso, Maurizio, Palmerini, Sara, Cristallo, Sergio, Piersanti, Luciano, Vescovi, Diego, and Busso, Maurizio
Abstract: Presolar grains and their isotopic compositions provide valuable constraints to AGB star nucleosynthesis. However, there is a sample of O- and Al-rich dust, known as group 2 oxide grains, whose origin is difficult to address. On the one hand, the 17O/16O isotopic ratios shown by those grains are similar to the ones observed in low-mass red giant stars. On the other hand, their large 18O depletion and 26Al enrichment are challenging to account for. Two different classes of AGB stars have been proposed as progenitors of this kind of stellar dust: intermediate mass AGBs with hot bottom burning, or low mass AGBs where deep mixing is at play. Our models of low-mass AGB stars with a bottom-up deep mixing are shown to be likely progenitors of group 2 grains, reproducing together the 17O/16O, 18O/16O and 26Al/27Al values found in those grains and being less sensitive to nuclear physics inputs than our intermediate-mass models with hot bottom burning.
Published: 2021

36. AGB Stars and Their Circumstellar Envelopes. I. the VULCAN Code

Author: Cristallo, Sergio, primary, Piersanti, Luciano, additional, Gobrecht, David, additional, Crivellari, Lucio, additional, and Nanni, Ambra, additional
Published: 2021
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37. Measurement of the energy-differential cross-section of the 12C(n,p)12B and 12C(n,d)11B reactions at the n_TOF facility at CERN

Author: International Conference on Nuclear Data for Science and Technology (2019 : Peking), Barbagallo, Massimo, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté- Gilarte, M., Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., Žugec, Petar, International Conference on Nuclear Data for Science and Technology (2019 : Peking), Barbagallo, Massimo, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté- Gilarte, M., Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., and Žugec, Petar
Abstract: Although the 12C(n,p)12B and 12C(n,d)11B reactions are of interest in several fields of basic and applied Nuclear Physics the present knowledge of these two cross-sections is far from being accurate and reliable, with both evaluations and data showing sizable discrepancies. As part of the challenging n_TOF program on (n,cp) nuclear reactions study, the energy differential cross-sections of the 12C(n,p)12B and 12C(n,d)11 B reactions have been measured at CERN from the reaction thresholds up to 30 MeV neutron energy. Both measurements have been recently performed at the long flight-path (185 m) experimental area of the n_TOF facility at CERN using a pure (99.95%) rigid graphite target and two silicon telescopes. In this paper an overview of the experiment is presented together with a few preliminary results.
Published: 2020

38. Measurement of the 244Cm capture cross sections at both CERN n_TOF experimental areas

Author: International Conference on Nuclear Data for Science and Technology (2019 : Peking), Alcayne, Victor, Mendoza Cembranos, Emilio, Cano-Ott, Daniel, Kimura, Atsushi, Aberle, Oliver, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bécares, Vicente, Bečvář, František, Bellia, Giorgio, Berthoumieux, Eric, Billowes, Jonathan, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Casanovas Hoste, Adrià, Cerutti, Francesco, Chen, Yonghao, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Glodariu, Tudor, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Kadi, Yacine, Käppeler, Franz, Kivel, Nikolay, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lo Meo, Sergio, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Matteucci, Francesca, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Mingrone, Federica, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Piersanti, Luciano, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Radeck, Désirée, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Smith, Alastair Gavin, Sosnin, Nikolay V., Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Talip, Zeynep, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Torres-Sánchez, Pablo, Tsinganis, Andrea, Ulrich, Jiri, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., Žugec, Petar, International Conference on Nuclear Data for Science and Technology (2019 : Peking), Alcayne, Victor, Mendoza Cembranos, Emilio, Cano-Ott, Daniel, Kimura, Atsushi, Aberle, Oliver, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bécares, Vicente, Bečvář, František, Bellia, Giorgio, Berthoumieux, Eric, Billowes, Jonathan, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Casanovas Hoste, Adrià, Cerutti, Francesco, Chen, Yonghao, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Glodariu, Tudor, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Kadi, Yacine, Käppeler, Franz, Kivel, Nikolay, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lo Meo, Sergio, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Matteucci, Francesca, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Mingrone, Federica, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Piersanti, Luciano, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Radeck, Désirée, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Smith, Alastair Gavin, Sosnin, Nikolay V., Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Talip, Zeynep, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Torres-Sánchez, Pablo, Tsinganis, Andrea, Ulrich, Jiri, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., and Žugec, Petar
Abstract: Accurate neutron capture cross section data for minor actinides (MAs) are required to estimate the production and transmutation rates of MAs in light water reactors with a high burnup, critical fast reactors like Gen-IV systems and other innovative reactor systems such as accelerator driven systems (ADS). Capture reactions of 244Cm open the path for the formation of heavier Cm isotopes and of heavier elements such as Bk and Cf. In addition, 244Cm shares nearly 50% of the total actinide decay heat in irradiated reactor fuels with a high burnup, even after three years of cooling. Experimental data for this isotope are very scarce due to the difficulties of providing isotopically enriched samples and because the high intrinsic activity of the samples requires the use of neutron facilities with high instantaneous flux. The only two previous experimental data sets for this neutron capture cross section have been obtained in 1969 using a nuclear explosion and, more recently, at J-PARC in 2010. The neutron capture cross sections have been measured at n_TOF with the same samples that the previous experiments in J-PARC. The samples were measured at n_TOF Experimental Area 2 (EAR-2) with three C6D6 detectors and also in Experimental Area 1 (EAR-1) with the Total Absorption Calorimeter (TAC). Preliminary results assessing the quality and limitations of these new experimental datasets are presented for the experiments in both areas. Preliminary yields of both measurements will be compared with evaluated libraries for the first time.
Published: 2020

39. Setup for the measurement of the 235U(n,f) cross section relative to n-p scattering up to 1 GeV

Author: International Conference on Nuclear Data for Science and Technology (2019 : Peking), Manna, Alice, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeno-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., Žugec, Petar, International Conference on Nuclear Data for Science and Technology (2019 : Peking), Manna, Alice, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeno-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., and Žugec, Petar
Abstract: The neutron induced fission of 235U is extensively used as a reference for neutron fluence measurements in various applications, ranging from the investigation of the biological effectiveness of high energy neutrons, to the measurement of high energy neutron cross sections of relevance for accelerator driven nuclear systems. Despite its widespread use, no data exist on neutron induced fission of 235U above 200 MeV. The neutron facility n_TOF offers the possibility to improve the situation. The measurement of 235U(n,f) relative to the differential n-p scattering cross-section, was carried out in September 2018 with the aim of providing accurate and precise cross section data in the energy range from 10 MeV up to 1 GeV. In such measurements, Recoil Proton Telescopes (RPTs) are used to measure the neutron flux while the fission events are detected and counted with dedicated detectors. In this paper the measurement campaign and the experimental set-up are illustrated.
Published: 2020

40. Status and perspectives of the neutron time-of-flight facility n_TOF at CERN

Author: International Conference on Nuclear Data for Science and Technology (2019 : Peking), Chiaveri, Enrico, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., Žugec, Petar, International Conference on Nuclear Data for Science and Technology (2019 : Peking), Chiaveri, Enrico, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jericha, Erwin, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Manna, Alice, Martı́nez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Sekhar, Adhitya, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., and Žugec, Petar
Abstract: Since the start of its operation in 2001, based on an idea of Prof. Carlo Rubbia [1], the neutron time of-flight facility of CERN, n_TOF, has become one of the most forefront neutron facilities in the world for wide-energy spectrum neutron cross section measurements. Thanks to the combination of excellent neutron energy resolution and high instantaneous neutron flux available in the two experimental areas, the second of which has been constructed in 2014, n_TOF is providing a wealth of new data on neutron-induced reactions of interest for nuclear astrophysics, advanced nuclear technologies and medical applications. The unique features of the facility will continue to be exploited in the future, to perform challenging new measurements addressing the still open issues and long-standing quests in the field of neutron physics. In this document the main characteristics of the n_TOF facility and their relevance for neutron studies in the different areas of research will be outlined, addressing the possible future contribution of n_TOF in the fields of nuclear astrophysics, nuclear technologies and medical applications. In addition, the future perspectives of the facility will be described including the upgrade of the spallation target, the setup of an imaging installation and the construction of a new irradiation area.
Published: 2020

41. Nuclear reactions

Author: Straniero, Oscar, primary, Imbriani, Gianluca, additional, and Piersanti, Luciano, additional
Published: 2010
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42. The luminosity constraint in the era of precision solar physics

Author: Vescovi, Diego, primary, Mascaretti, Carlo, additional, Vissani, Francesco, additional, Piersanti, Luciano, additional, and Straniero, Oscar, additional
Published: 2020
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43. A high-precision abundance analysis of the nuclear benchmark star HD 20

Author: Hanke, Michael, primary, Hansen, Camilla Juul, additional, Ludwig, Hans-Günter, additional, Cristallo, Sergio, additional, McWilliam, Andrew, additional, Grebel, Eva K., additional, and Piersanti, Luciano, additional
Published: 2020
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44. ⁷Be(n,p)⁷ Li Cross Section Measurement for the Cosmological Lithium Problem at the n_TOF Facility at CERN

Author: Damone, L.A., Barbagallo, M., Mastromarco, M., Mengoni, A., Colonna, N., Cosentino, L., Maugeri, E.A., Heinitz, S., Schumann, D., Dressler, R., Käppeler, F., Finocchiaro, P., Andrzejewski, J., Perkowski, J., Gawlik, A., Aberle, O., Altstadt, S., Ayranov, M., Audouin, L., Bacak, M., Balibrea-Correa, J., Ballof, J., Bcares, V., Bečvař, F., Beinrucker, C., Bellia, G., Bernardes, A.P., Berthoumieux, E., Billowes, J., Borge, M.J.G., Bosnar, D., Brown, A., Brugger, M., Busso, Maurizio, Caamaño, M., Calviño, F., Calviani, M., Cano-Ott, D., Cardella, R., Casanovas, A., Castelluccio, D.M., Catherall, R., Cerutti, F., Chen, Y.H., Chiaveri, E., Corts, G., Cortès-Giraldo, M.A., Cristallo, Sergio, Diakaki, M., Dietz, M., Domingo-Pardo, C., Dorsival, A., Dupont, E., Durán, I., Fernàndez-Dominguez, B., Ferrari, A., Ferreira, P., Furman, W., Ganesan, S., Garca-Rios, A., Gilardoni, S., Glodariu, T., Göbel, Kathrin, Gonçalves, I.F., Gonzalez-Romero, E., Goodacre, T.D., Griesmayer, E., Guerrero, C., Gunsing, F., Harada, H., Heftrich, Tanja, Heyse, J., Jenkins, D.G., Jericha, E., Johnston, K., Kadi, Y., Kalamara, A., Katabuchi, T., Kavrigin, P., Kimura, A., Kivel, N., Kohester, U., Kokkoris, M., Krtička, M., Kurtulgil, Deniz, Leal-Cidoncha, E., Lederer-Woods, Claudia, Leeb, H., Lerendegui-Marco, J., Lo Meo, S., Lonsdale, S.J., Losito, R., Macina, D., Marganiec, J., Marsh, B., Martínez, T., Martins Correia, J.G., Masi, A., Massimi, C., Mastinu, P., Matteucci, F., Mazzone, A., Mendoza, E., Milazzo, P.M., Mingrone, Federica, Mirea, M., Musumarra, A., Negret, A., Nolte, R., Oprea, A., Patronis, N., Pavlik, A., Piersanti, Luciano, Piscopo, M., Plompen, A., Porras, I., Praena, J., Quesada, J.M., Radeck, D., Rajeev, K., Rauscher, Thomas, Reifarth, René, Riego-Perez, A., Rothe, S., Rout, P., Rubbia, C., Ryan, J., Sabaté-Gilarte, M., Saxena, A., Schell, J., Schillebeeckx, P., Schmidt, S., Sedyshev, P., Seiffert, C., Smith, A.G., Sosnin, N.V., Stamatopoulos, A., Stora, T., Tagliente, G., Tain, J.L., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vlachoudis, V., Vlastou, R., Wallner, A., Warren, S., Weigand, Mario, Weiß, C., Wolf, C., Woods, P.J., Wright, T., and Žugec, P.
Subjects: Bauwissenschaften
Published: 2019

45. Thermonuclear oubursts of AM CVn stars

Author: Yungelson, L. R., PIERSANTI, Luciano, Tornambé, A., CRISTALLO, Sergio, ITA, and RUS
Subjects: Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We consider initial stage of the evolution of AM CVn type stars with white dwarf donors, which is accompanied by thermonuclear explosions in the layer of accreted He. It is shown that the accretion never results in detonation of He and accretors in AM CVn stars finish their evolution as massive WDs. We found, for the first time, that in the outbursts the synthesis of n-rich isotopes, initiated by the ${\mathrm{^{22}{Ne}(\alpha,n)^{25}Mg}}$ reaction becomes possible., Comment: 6 pages, 4 figures, English translation of the paper to be published in Russian only in INASAN Science Proceedings
Published: 2019
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46. Fission program at n_TOF

Author: International Workshop on Nuclear Data Evaluation for Reactor Applications (5. : 2018 : Aix-en-Provence), Tassan-Got, Laurent, Colonna, Nicola, Diakaki, Maria, Eleme, Zinovia, Manna, Alice, Sekhar, Adhitya, Stamatopoulos, Athanasios, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Martinez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., Žugec, Petar, International Workshop on Nuclear Data Evaluation for Reactor Applications (5. : 2018 : Aix-en-Provence), Tassan-Got, Laurent, Colonna, Nicola, Diakaki, Maria, Eleme, Zinovia, Manna, Alice, Sekhar, Adhitya, Stamatopoulos, Athanasios, Aberle, Oliver, Alcayne, Victor, Amaducci, Simone, Andrzejewski, Józef, Audouin, Laurent, Babiano Suarez, Victor, Bacak, Michael, Barbagallo, Massimo, Bennett, Samuel, Berthoumieux, Eric, Bosnar, Damir, Brown, Adam S., Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviani, Marco, Calviño Tavares, Francisco, Cano-Ott, Daniel, Casanovas Hoste, Adrià, Cerutti, Francesco, Chiaveri, Enrico, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Davies, Paul John, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Ducasse, Quentin, Dupont, Emmeric, Durán, Ignacio, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Gonçalves, Isabel Maria Ferro, Finocchiaro, Paolo, Furman, Valter, Garg, Ruchi, Gawlik, Aleksandra, Gilardoni, Simone, Göbel, Kathrin, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Jiri, U., Junghans, Arnd Rudolf, Kadi, Yacine, Käppeler, Franz, Kimura, Atsushi, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lonsdale, Sarah-Jane, Macina, Daniela, Martinez, Trinitario, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mendoza Cembranos, Emilio, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Millán Callado, María de los Ángeles, Mingrone, Federica, Moreno-Soto, Javier, Musumarra, Agatino, Negret, Alexandru, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Petrone, Cristina, Piersanti, Luciano, Pirovano, Elisa, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Ramos Doval, Diego, Reifarth, René, Rochman, Dimitri, Rubbia, Carlo, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Smith, Alastair Gavin, Sosnin, Nikolay V., Sprung, Peter, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Tarifeño-Saldivia, Ariel, Thomas, Benedikt, Torres-Sánchez, Pablo, Tsinganis, Andrea, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias J., and Žugec, Petar
Abstract: Since its start in 2001 the n_TOF collaboration developed a measurement program on fission, in view of advanced fuels in new generation reactors. A special effort was made on measurement of cross sections of actinides, exploiting the peculiarity of the n_TOF neutron beam which spans a huge energy domain, from the thermal region up to GeV. Moreover fission fragment angular distributions have also been measured. An overview of the cross section results achieved with different detectors is presented, including a discussion of the 237Np case where discrepancies showed up between different detector systems. The results on the anisotropy of the fission fragments and its implication on the mechanism of neutron absorption, and in applications, are also shown.
Published: 2019

47. Measurement of the 244Cm and 246Cm neutron-induced capture cross sections at the n_TOF facility

Author: International Workshop on Nuclear Data Evaluation for Reactor Applications (5. : 2018 : Aix-en-Provence), Alcayne, Victor, Kimura, Atsushi, Mendoza Cembranos, Emilio, Cano-Ott, Daniel, Martı́nez, Trinitario, Aberle, Oliver, Andrzejewski, Józef, Audouin, Laurent, Bécares, Vicente, Bacak, Michael, Barbagallo, Massimo, Bečvář, František, Bellia, Giorgio, Berthoumieux, Eric, Billowes, Jonathan, Bosnar, Damir, Brown, Adam, Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviño Tavares, Francisco, Calviani, Marco, Casanovas Hoste, Adrià, Cerutti, Francesco, Chen, Yonghao, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Finocchiaro, Paolo, Furman, Valter, Göbel, Kathrin, Gawlik, Aleksandra, Gilardoni, Simone, Glodariu, Tudor, Gonçalves, Isabel Maria Ferro, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Harada, Hideo, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Käppeler, Franz, Kadi, Yacine, Katabuchi, Tatsuya, Kivel, Nikolay, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lo Meo, Sergio, Lonsdale, Sarah Jane, Macina, Daniela, Manna, Alice, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Matteucci, Francesca, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Mingrone, Federica, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Piersanti, Luciano, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Radeck, Désirée, Ramos Doval, Diego, Rauscher, Thomas, Reifarth, René, Rochman, Dimitri, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Simone, S., Smith, Alastair Gavin, Sosnin, Nikolay V., Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Talip, T., Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Tsinganis, Andrea, Ulrich, Jiri, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias, Žugec, Petar, International Workshop on Nuclear Data Evaluation for Reactor Applications (5. : 2018 : Aix-en-Provence), Alcayne, Victor, Kimura, Atsushi, Mendoza Cembranos, Emilio, Cano-Ott, Daniel, Martı́nez, Trinitario, Aberle, Oliver, Andrzejewski, Józef, Audouin, Laurent, Bécares, Vicente, Bacak, Michael, Barbagallo, Massimo, Bečvář, František, Bellia, Giorgio, Berthoumieux, Eric, Billowes, Jonathan, Bosnar, Damir, Brown, Adam, Busso, Maurizio, Caamaño, Manuel, Caballero Ontanaya, Luis, Calviño Tavares, Francisco, Calviani, Marco, Casanovas Hoste, Adrià, Cerutti, Francesco, Chen, Yonghao, Chiaveri, Enrico, Colonna, Nicola, Cortés Rossell, Guillem Pere, Cortés-Giraldo, Miguel Antonio, Cosentino, Luigi, Cristallo, Sergio, Damone, Lucia Anna, Diakaki, Maria, Dietz, Mirco, Domingo-Pardo, César, Dressler, Rugard, Dupont, Emmeric, Durán, Ignacio, Eleme, Zinovia, Fernández Domínguez, Beatriz, Ferrari, Alfredo, Finocchiaro, Paolo, Furman, Valter, Göbel, Kathrin, Gawlik, Aleksandra, Gilardoni, Simone, Glodariu, Tudor, Gonçalves, Isabel Maria Ferro, González Romero, Enrique Miguel, Guerrero Sánchez, Carlos, Gunsing, Frank, Harada, Hideo, Heinitz, Stephan, Heyse, Jan, Jenkins, David, Käppeler, Franz, Kadi, Yacine, Katabuchi, Tatsuya, Kivel, Nikolay, Knapová, Ingrid, Kokkoris, Michael, Kopatch, Yuri N., Krtička, Milan, Kurtulgil, Cem Deniz, Ladarescu, Ion, Lederer-Woods, Claudia, Lerendegui-Marco, Jorge, Lo Meo, Sergio, Lonsdale, Sarah Jane, Macina, Daniela, Manna, Alice, Masi, Alessandro, Massimi, Cristian, Mastinu, Pierfrancesco, Mastromarco, Mario, Matteucci, Francesca, Maugeri, Emilio Andrea, Mazzone, Annamaria, Mengoni, Alberto, Michalopoulou, Veatriki, Milazzo, Paolo Maria, Mingrone, Federica, Musumarra, Agatino, Negret, Alexandru, Nolte, Ralf, Ogállar Ruiz, Francisco, Oprea, Andreea, Patronis, Nikolas, Pavlik, Andreas, Perkowski, Jarosław, Piersanti, Luciano, Porras Sánchez, José Ignacio, Praena, Javier, Quesada Molina, José Manuel, Radeck, Désirée, Ramos Doval, Diego, Rauscher, Thomas, Reifarth, René, Rochman, Dimitri, Sabaté-Gilarte, Marta, Saxena, Alok, Schillebeeckx, Peter, Schumann, Dorothea, Simone, S., Smith, Alastair Gavin, Sosnin, Nikolay V., Stamatopoulos, Athanasios, Tagliente, Giuseppe, Taı́n Enríquez, José Luis, Talip, T., Tarifeño-Saldivia, Ariel, Tassan-Got, Laurent, Tsinganis, Andrea, Ulrich, Jiri, Urlaß, Sebastian, Valenta, Stanislav, Vannini, Gianni, Variale, Vincenzo, Vaz, Pedro, Ventura, Alberto, Vescovi, Diego, Vlachoudis, Vasilis, Vlastou, Rosa, Wallner, Anton, Woods, Philip John, Wright, Tobias, and Žugec, Petar
Abstract: The neutron capture reactions of the 244Cm and 246Cm isotopes open the path for the formation of heavier Cm isotopes and heavier elements such as Bk and Cf in a nuclear reactor. In addition, both isotopes belong to the minor actinides with a large contribution to the decay heat and to the neutron emission in irradiated fuels. There are only two previous 244Cm and 246Cm capture cross section measurements: one in 1969 using a nuclear explosion [1] and the most recent data measured at J-PARC in 2010 [2]. The data for both isotopes are very scarce due to the difficulties in performing the measurements: high intrinsic activity of the samples and limited facilities capable of providing isotopically enriched samples. We have measured both neutron capture cross sections at the n_TOF Experimental Area 2 (EAR-2) with three C6 D6 detectors and also at Area 1 (EAR-1) with the TAC. Preliminary results assessing the quality and limitations (back-ground subtraction, measurement technique and counting statistics) of this new experimental datasets are presented and discussed.
Published: 2019

48. Data for the s Process from n_TOF

Author: Massimi, C., Aberle, O., Alcayne, V., Andrzejewski, J., Audouin, L., Bécares, V., Babiano-Suarez, V., Bacak, M., Barbagallo, M., Benedikt, Th., Bennett, S., Göbel, Kathrin, Gawlik, A., Gilardoni, S., Gonçalves, I. F., González-Romero, E., Guerrero, C., Gunsing, F., Heinitz, S., Heyse, J., Jenkins, D. G., Matteucci, F., Junghans, Arnd R., Käppeler, F., Kadi, Y., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krtička, M., Kurtulgil, Deniz, Ladarescu, I., Maugeri, E. A., Lederer-Woods, Claudia, Lonsdale, S. J., Macina, D., Manna, A., Martínez, T., Masi, A., Mastinu, P., Mastromarco, M., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, Federica, Moreno-Soto, J., Musumarra, A., Schillebeeckx, P., Negret, A., Ogállar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., PIERSANTI, Luciano, Petrone, C., Pirovano, E., Porras, I., Schumann, D., Praena, J., Quesada, J. M., Ramos-Doval, D., Rauscher, Thomas, Reifarth, René, Rochman, D., Sabaté-Gilarte, M., Saxena, A., Sekhar, A., Simone, S., Smith, A. G., Sosnin, N. V., Sprung, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Berthoumieux, E., Tarifeño-Saldivia, A., Tassan-Got, L., Tsinganis, A., Ulrich, J., Urlass, Sebastian, Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Billowes, J., VESCOVI, DIEGO, Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Žugec, P., n TOF Collaboration, Bosnar, D., Brown, A., Busso, Maurizio, Caamaño, M., Caballero-Ontanaya, L., Calviño, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chiaveri, E., Clai, G., Colonna, N., Cortés, G., Cortès-Giraldo, M. A., Cosentino, L., CRISTALLO, Sergio, Damone, L. A., Davies, P. J., Dietz, M., Domingo-Pardo, C., Dressler, R., Ducasse, Q., Dupont, E., Durán, I., Eleme, Z., Fernàndez-Dominguez, B., Ferrari, A., Finocchiaro, P., Furman, V., Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Massimi, C., Aberle, O., Alcayne, V., Andrzejewski, J., Audouin, L., Becares, V., Babiano-Suarez, V., Bacak, M., Barbagallo, M., Benedikt, T., Bennett, S., Berthoumieux, E., Billowes, J., Bosnar, D., Brown, A., Busso, M., Caamano, M., Caballero-Ontanaya, L., Calvino, F., Calviani, M., Cano-Ott, D., Casanovas, A., Castelluccio, D. M., Cerutti, F., Chiaveri, E., Clai, G., Colonna, N., Cortes, G., Cortes-Giraldo, M. A., Cosentino, L., Cristallo, S., Damone, L. A., Davies, P. J., Dietz, M., Domingo-Pardo, C., Dressler, R., Ducasse, Q., Dupont, E., Duran, I., Eleme, Z., Fernandez-Dominguez, B., Ferrari, A., Finocchiaro, P., Furman, V., Gobel, K., Gawlik, A., Gilardoni, S., Goncalves, I. F., Gonzalez-Romero, E., Guerrero, C., Gunsing, F., Heinitz, S., Heyse, J., Jenkins, D. G., Junghans, A. R., Kappeler, F., Kadi, Y., Kimura, A., Knapova, I., Kokkoris, M., Kopatch, Y., Krticka, M., Kurtulgil, D., Ladarescu, I., Lederer-Woods, C., Lonsdale, S. J., Macina, D., Manna, A., Martinez, T., Masi, A., Mastinu, P., Mastromarco, M., Matteucci, F., Maugeri, E. A., Mazzone, A., Mendoza, E., Mengoni, A., Michalopoulou, V., Milazzo, P. M., Mingrone, F., Moreno-Soto, J., Musumarra, A., Negret, A., Ogallar, F., Oprea, A., Patronis, N., Pavlik, A., Perkowski, J., Piersanti, L., Petrone, C., Pirovano, E., Porras, I., Praena, J., Quesada, J. M., Ramos-Doval, D., Rauscher, T., Reifarth, R., Rochman, D., Sabate-Gilarte, M., Saxena, A., Schillebeeckx, P., Schumann, D., Sekhar, A., Simone, S., Smith, A. G., Sosnin, N. V., Sprung, P., Stamatopoulos, A., Tagliente, G., Tain, J. L., Tarifeno-Saldivia, A., Tassan-Got, L., Tsinganis, A., Ulrich, J., Urlass, S., Valenta, S., Vannini, G., Variale, V., Vaz, P., Ventura, A., Vescovi, D., Vlachoudis, V., Vlastou, R., Wallner, A., Woods, P. J., Wright, T., Zugec, P., Formicola, Alba, Junker, Matthias, Gialanella, Lucio, Imbriani, Gianluca, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Massimi C., Aberle O., Alcayne V., Andrzejewski J., Audouin L., Becares V., Babiano-Suarez V., Bacak M., Barbagallo M., Benedikt T., Bennett S., Berthoumieux E., Billowes J., Bosnar D., Brown A., Busso M., Caamano M., Caballero-Ontanaya L., Calvino F., Calviani M., Cano-Ott D., Casanovas A., Castelluccio D.M., Cerutti F., Chiaveri E., Clai G., Colonna N., Cortes G., Cortes-Giraldo M.A., Cosentino L., Cristallo S., Damone L.A., Davies P.J., Dietz M., Domingo-Pardo C., Dressler R., Ducasse Q., Dupont E., Duran I., Eleme Z., Fernandez-Dominguez B., Ferrari A., Finocchiaro P., Furman V., Gobel K., Gawlik A., Gilardoni S., Goncalves I.F., Gonzalez-Romero E., Guerrero C., Gunsing F., Heinitz S., Heyse J., Jenkins D.G., Junghans A.R., Kappeler F., Kadi Y., Kimura A., Knapova I., Kokkoris M., Kopatch Y., Krticka M., Kurtulgil D., Ladarescu I., Lederer-Woods C., Lonsdale S.J., Macina D., Manna A., Martinez T., Masi A., Mastinu P., Mastromarco M., Matteucci F., Maugeri E.A., Mazzone A., Mendoza E., Mengoni A., Michalopoulou V., Milazzo P.M., Mingrone F., Moreno-Soto J., Musumarra A., Negret A., Ogallar F., Oprea A., Patronis N., Pavlik A., Perkowski J., Piersanti L., Petrone C., Pirovano E., Porras I., Praena J., Quesada J.M., Ramos-Doval D., Rauscher T., Reifarth R., Rochman D., Sabate-Gilarte M., Saxena A., Schillebeeckx P., Schumann D., Sekhar A., Simone S., Smith A.G., Sosnin N.V., Sprung P., Stamatopoulos A., Tagliente G., Tain J.L., Tarifeno-Saldivia A., Tassan-Got L., Tsinganis A., Ulrich J., Urlass S., Valenta S., Vannini G., Variale V., Vaz P., Ventura A., Vescovi D., Vlachoudis V., Vlastou R., Wallner A., Woods P.J., Wright T., Zugec P., and n_TOF
Subjects: Physics, Large Hadron Collider, Isotope, 010308 nuclear & particles physics, s-process, n_TOF, neutron capture data, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, 3. Good health, Nuclear physics, Nucleosynthesis, s process, nucleosynthesis, 0103 physical sciences, Neutron, s-process, 010303 astronomy & astrophysics
Abstract: International audience; A considerable amount of (n, $\gamma $ ) reactions has been studied, so far, at the neutron time-of-flight facility n_TOF at CERN. The experimental program aims at determining and improving cross sections for a number of isotopes relevant to s-process nucleosynthesis. A brief summary of some physical cases related to the s-process nucleosyntheis is presented in this work together with ongoing experiments and challenging future programs.
Published: 2018
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49. Comprehensive models of novae at metallicity Z = 0.02 and Z = 10−4

Author: Chen, Hai-Liang, primary, Woods, T E, additional, Yungelson, L R, additional, Piersanti, Luciano, additional, Gilfanov, M, additional, and Han, Zhanwen, additional
Published: 2019
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50. The Initial Mass–Final Luminosity Relation of Type II Supernova Progenitors: Hints of New Physics?

Author: Straniero, Oscar, primary, Dominguez, Inma, additional, Piersanti, Luciano, additional, Giannotti, Maurizio, additional, and Mirizzi, Alessandro, additional
Published: 2019
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