Zobrazeno 1 - 10
of 345
pro vyhledávání: '"R.G. Pizzone"'
Autor:
A. Cvetinović, D. Đeorđić, G.L. Guardo, M. Kelemen, M. La Cognata, L. Lamia, S. Markelj, U. Mikac, R.G. Pizzone, T. Schwarz-Selinger, I. Tišma, M. Vencelj, J. Vesić, M. Lipoglavšek
Publikováno v:
Physics Letters B, Vol 838, Iss , Pp 137684- (2023)
The electron screening effect was studied in the 1H(7Li,α)4He, 1H(19F,αγ)16O and 2H(19F,p)20F nuclear reactions on two different hydrogen-containing palladium foils. In one of the targets we did not detect a large enhancement of the cross section
Externí odkaz:
https://doaj.org/article/a86484adcddc4fd781546b0eb0bd84a6
Autor:
M. La Cognata, S. Palmerini, P. Adsley, F. Hammache, A. Di Pietro, P. Figuera, R. Alba, S. Cherubini, F. Dell'Agli, G.L. Guardo, M. Gulino, L. Lamia, D. Lattuada, C. Maiolino, A. Oliva, R.G. Pizzone, P.M. Prajapati, S. Romano, D. Santonocito, R. Spartá, M.L. Sergi, A. Tumino
Publikováno v:
Physics Letters B, Vol 826, Iss , Pp 136917- (2022)
The 26Al abundance holds a special role in present-day astrophysics, since it is a probe of active nucleosynthesis in the Galaxy and a valuable constraint of Galactic core-collapse supernovae rate. It is estimated through the detection of the 1809-ke
Externí odkaz:
https://doaj.org/article/f1f3b29797ee4b8fb716c4a2851bd416
Autor:
G.G. Rapisarda, L. Lamia, A. Caciolli, Chengbo Li, S. Degl’Innocenti, R. Depalo, S. Palmerini, R.G. Pizzone, S. Romano, C. Spitaleri, E. Tognelli, Qungang Wen
Publikováno v:
Frontiers in Astronomy and Space Sciences, Vol 7 (2021)
Light elements offer a unique opportunity for studying several astrophysical scenarios from Big Bang Nucleosynthesis to stellar physics. Understanding the stellar abundances of light elements is key to obtaining information on internal stellar struct
Externí odkaz:
https://doaj.org/article/b82d8df3aff2472fa1e871fb0ada7b8b
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:
A. Tumino, A. Bonasera, G. Giuliani, M. Lattuada, M. Milin, R.G. Pizzone, C. Spitaleri, S. Tudisco
Publikováno v:
Physics Letters B, Vol 750, Iss C, Pp 59-63 (2015)
The 6Li + 6Li → 3α reaction has been measured in a kinematically complete experiment at 3.1 MeV of beam energy. The reaction mainly proceeds via intermediate 8Be states. The interaction between any two of the three α particles provides events wit
Externí odkaz:
https://doaj.org/article/cb05f6801205494eb2b18f5923a3f1bb
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:
H. Yamaguchi, S. Hayakawa, N.R. Ma, H. Shimizu, K. Okawa, Q. Zhang, L. Yang, D. Kahl, M. La Cognata, L. Lamia, K. Abe, O. Beliuskina, S.M. Cha, K.Y. Chae, S. Cherubini, P. Figuera, Z. Ge, M. Gulino, J. Hu, A. Inoue, N. Iwasa, A. Kim, D. Kim, G. Kiss, S. Kubono, M. La Commara, M. Lattuada, E.J. Lee, J.Y. Moon, S. Palmerini, C. Parascandolo, S.Y. Park, V.H. Phong, D. Pierroutsakou, R.G. Pizzone, G.G. Rapisarda, S. Romano, C. Spitaleri, X.D. Tang, O. Trippella, A. Tumino, N.T. Zhang, Y.H. Lam, A. Heger, A.M. Jacobs, S.W. Xu, S.B. Ma, L.H. Ru, E.Q. Liu, T. Liu, C.B. Hamill, A. St J. Murphy, J. Su, X. Fang, M.S. Kwag, N.N. Duy, N.K. Uyen, D.H. Kim, J. Liang, A. Psaltis, M. Sferrazza, Z. Johnston, Y.Y. Li
Astrophysical reactions involving radioactive isotopes (RI) often play an important role in high-temperature stellar environments. The experimental studies on the reaction rates for those are still limited mainly due to the technical difficulties in
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::a57900e370742a76d423f6cf84bdac3d
https://hdl.handle.net/20.500.11769/558667
https://hdl.handle.net/20.500.11769/558667
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
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Akademický článek
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