Zobrazeno 1 - 10
of 160
pro vyhledávání: '"G. D’Agata"'
Autor:
G. L. Guardo, L. Lamia, J. P. Fernández-García, S. Piskor, M. La Cognata, G. D’Agata, S. Palmerini, D. Vescovi, V. Burjan, R. J. deBoer, V. Kroha, D. Lattuada, J. Mrazek, A. A. Oliva, R. G. Pizzone, G. G. Rapisarda, S. Romano, M. L. Sergi, R. Spartá, A. Tumino
Publikováno v:
The Astrophysical Journal, Vol 975, Iss 1, p 32 (2024)
Indirect methods have proven to be a complementary approach for extending our knowledge of nuclear structure and low-energy cross sections. Among these, the neutron-induced reaction cross sections appear to be of particular interest since their role
Externí odkaz:
https://doaj.org/article/d4bc6305f7224b5898d1e195b0c7c0b8
Autor:
R. Spartà, M. La Cognata, G. L. Guardo, S. Palmerini, M. L. Sergi, G. D’Agata, L. Lamia, D. Lattuada, A. A. Oliva, R. G. Pizzone, G. G. Rapisarda, S. Romano, A. Tumino
Publikováno v:
Frontiers in Physics, Vol 10 (2022)
A large uncertainty for the slow neutron capture nucleosynthesis (s-process) models is caused by the amount of neutrons available to the process itself. This quantity is strongly affected by the 13C(α,n)16O, and 22Ne(α,n)25Mg reaction cross section
Externí odkaz:
https://doaj.org/article/06770c37d3174fc8ab593c2be45214b0
Autor:
G.G. Kiss, M. La Cognata, C. Spitaleri, R. Yarmukhamedov, I. Wiedenhöver, L.T. Baby, S. Cherubini, A. Cvetinović, G. D'Agata, P. Figuera, G.L. Guardo, M. Gulino, S. Hayakawa, I. Indelicato, L. Lamia, M. Lattuada, F. Mudò, S. Palmerini, R.G. Pizzone, G.G. Rapisarda, S. Romano, M.L. Sergi, R. Spartà, O. Trippella, A. Tumino, M. Anastasiou, S.A. Kuvin, N. Rijal, B. Schmidt, S.B. Igamov, S.B. Sakuta, K.I. Tursunmakhatov, Zs. Fülöp, Gy. Gyürky, T. Szücs, Z. Halász, E. Somorjai, Z. Hons, J. Mrázek, R.E. Tribble, A.M. Mukhamedzhanov
Publikováno v:
Physics Letters B, Vol 807, Iss , Pp 135606- (2020)
The detection of the neutrinos produced in the p−p chain and in the CNO cycle can be used to test the Standard Solar Model. The 3He(α,γ)7Be reaction is the first reaction of the 2nd and 3rd branch of the p−p chain, therefore, the uncertainty of
Externí odkaz:
https://doaj.org/article/a80b526e70be4ffcb24cd571d27516a2
Autor:
G. L. Guardo, T. Petruse, D. Lattuada, M. La Cognata, D. L. Balabanski, E. Açıksöz, L. Acosta, L. Capponi, D. Carbone, S. Cherubini, D. Choudhury, G. D’Agata, A. Di Pietro, P. Figuera, M. Gulino, A. I. Kilik, M. La Commara, L. Lamia, C. Matei, S. Palmerini, R. G. Pizzone, G. G. Rapisarda, S. Romano, M. L. Sergi, P.-A. Söderström, R. Spartà, A. Tumino, S. Viñals
Publikováno v:
The European Physical Journal A. 59
Akademický článek
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Autor:
A. A. Oliva, A. Tumino, N. Soic, P. M. Prajapati, L. Acosta, R. Alba, F. Barba, S. Cherubini, G. D’Agata, D. Dell’Aquila, A. Di Pietro, J.P. Fernandez, P. Figuera, D. Galaviz Redondo, L. Guardo, M. Gulino, F. Hammache, D. Jelavic Malenica, A.I. Kiliç, M. La Cognata, M. La Commara, L. Lamia, D. Lattuada, C. Maiolino, G. Manicò, M. Mazzocco, M. Milin, Ma Nanru, A. Nurmukhanbetova, D. Nurkic, S. Palmerini, T. Parascandolo, D. Pierroutsakou, R.G. Pizzone, R. Popocovski, G.G. Rapisarda, S. Romano, D. Santonocito, M.L. Sergi, A. Shotter, R. Spartà, A. Spiridon, L. Trache, N. Vukman, H. Yamaguchi
12C +12 C is the main reaction during core and shell carbon burning in massive stars, however, at temperatures higher than 109K when most of the carbon is depleted and its abundance is lower than 16O, the 12C +16 O fusion can also become relevant. Mo
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::5d6ccaa6cadc3b0aabcc2a45eff433f6
https://hdl.handle.net/20.500.11769/558663
https://hdl.handle.net/20.500.11769/558663
Autor:
A.A. Oliva, A. Tumino, N. Soic, M.P. Prajapati, L. Acosta, R. Alba, F. Barba, S. Cherubini, G. D’Agata, D. Dell’Aquila, A. Di Pietro, P.J. Fernandez, P. Figuera, D. Galaviz Redondo, L. Guardo, M. Gulino, F. Hammache, D. Jelavic Malenica, A.I. Kiliç, M. La Cognata, M. La Commara, L. Lamia, D. Lattuada, C. Maiolino, G. Manicò, M. Mazzocco, M. Milin, Ma Nanru, A. Nurmukhanbetova, D. Nurkic, S. Palmerini, T. Parascandolo, D. Pierroutsakou, R.G. Pizzone, R. Popocovski, G.G. Rapisarda, S. Romano, D. Santonocito, M.L. Sergi, A. Shotter, R. Spartà, A. Spiridon, L. Trache, N. Vukman, H. Yamaguchi
The carbon-burning process in massive stars mainly occurs via the 12C +12 C. However, at temperatures higher than 109K and considering the increased abundance of 16O produced during the later stages of the heliumburning,the 12C+16O fusion can also be
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::30ec1accd2af6e1d0672088ddc277306
https://hdl.handle.net/20.500.11769/558666
https://hdl.handle.net/20.500.11769/558666
Autor:
V. Girard-Alcindor, A. Mercenne, I. Stefan, F. de Oliveira Santos, N. Michel, M. Płoszajczak, M. Assié, A. Lemasson, E. Clément, F. Flavigny, A. Matta, D. Ramos, M. Rejmund, J. Dudouet, D. Ackermann, P. Adsley, M. Assunção, B. Bastin, D. Beaumel, G. Benzoni, R. Borcea, A. J. Boston, D. Brugnara, L. Cáceres, B. Cederwall, I. Celikovic, V. Chudoba, M. Ciemala, J. Collado, F. C. L. Crespi, G. D'Agata, G. De France, F. Delaunay, C. Diget, C. Domingo-Pardo, J. Eberth, C. Fougères, S. Franchoo, F. Galtarossa, A. Georgiadou, J. Gibelin, S. Giraud, V. González, N. Goyal, A. Gottardo, J. Goupil, S. Grévy, V. Guimaraes, F. Hammache, L. J. Harkness-Brennan, H. Hess, N. Jovančević, D. S. Judson Oliver, O. Kamalou, A. Kamenyero, J. Kiener, W. Korten, S. Koyama, M. Labiche, L. Lalanne, V. Lapoux, S. Leblond, A. Lefevre, C. Lenain, S. Leoni, H. Li, A. Lopez-Martens, A. Maj, I. Matea, R. Menegazzo, D. Mengoni, A. Meyer, B. Million, B. Monteagudo, P. Morfouace, J. Mrazek, M. Niikura, J. Piot, Zs. Podolyak, C. Portail, A. Pullia, B. Quintana, F. Recchia, P. Reiter, K. Rezynkina, T. Roger, J. S. Rojo, F. Rotaru, M. D. Salsac, A. M. Sánchez Benítez, E. Sanchis, M. Şenyigit, N. de Séréville, M. Siciliano, J. Simpson, D. Sohler, O. Sorlin, M. Stanoiu, C. Stodel, D. Suzuki, C. Theisen, D. Thisse, J. C.Thomas, P. Ujic, J. J. Valiente-Dobón, M. Zielińska
Publikováno v:
Physical Review C. 105
Akademický článek
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Publikováno v:
EPJ Web of Conferences. 275:01008
The Asymptotic Normalization Coefficient (ANC) method, has proven to be useful in retrieving the direct part of the radiative capture cross section for a number of reactions of astrophysical interest. In this work, some of the latest results obtained