Zobrazeno 1 - 10
of 156
pro vyhledávání: '"M. L., Sergi"'
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
Publikováno v:
Frontiers in Astronomy and Space Sciences, Vol 7 (2021)
Among presolar grains, oxide ones are made of oxygen, aluminum, and a small fraction of magnesium, produced by the 26Al decay. The largest part of presolar oxide grains belong to the so-called group 1 and 2, which have been suggested to form in Red G
Externí odkaz:
https://doaj.org/article/ea9924839137439ab72a59946cf65319
Autor:
M. L. Sergi, G. L. Guardo, M. La Cognata, M. Gulino, J. Mrazek, S. Palmerini, C. Spitaleri, M. Wiescher
Publikováno v:
Frontiers in Astronomy and Space Sciences, Vol 7 (2020)
Observations of abundances and isotopic ratio determinations in stars yield powerful constraints on stellar models. In particular, the oxygen isotopic ratios are of particular interest because they are affected not only by nucleosynthesis but also by
Externí odkaz:
https://doaj.org/article/7e7aea83d8a44a5f9e46263e928e3ec0
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
Autor:
M. La Cognata, S. Palmerini, P. Adsley, F. Hammache, A. Di Pietro, P. Figuera, F. Dell’Agli, R. Alba, S. Cherubini, G. L. Guardo, M. Gulino, L. Lamia, D. Lattuada, C. Maiolino, A. Oliva, R. G. Pizzone, P. M. Prajapati, G. G. Rapisarda, S. Romano, D. Santonocito, R. Spartá, M. L. Sergi, A. Tumino, P. Ventura
The abundance of 26Al carries a special role in astrophysics, since it probes active nucleosynthesis in the Milky Way and constrains the Galactic core-collapse supernovae rate. It is estimated through the detection of the 1809 keV γ-line and from th
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::32a9e1a0d676115efadd04bce719c7a9
https://hdl.handle.net/11391/1544494
https://hdl.handle.net/11391/1544494
Autor:
G. Manicò, M. L. Sergi, E. Chávez, R. Alba, J. Mrazek, G. D’Agata, A. Cvetinović, S. Hayakawa, Fairouz Hammache, G. G. Kiss, T. Parascandolo, Luis Acosta, K. Gaitán De Los Rios, Domenico Santonocito, Roberta Spartà, Catalin Matei, Silvio Cherubini, G. G. Rapisarda, Sara Palmerini, Livio Lamia, A. Tumino, T. Petruse, D. Pierroutsakou, M. Mazzocco, R. G. Pizzone, V. Burjan, M. La Commara, N. de Séréville, M. La Cognata, Zsolt Fülöp, Marisa Gulino, P. Figuera, G. L. Guardo, H. Yamaguchi, A. Di Pietro, S. Romano, C. Maiolino
Publikováno v:
The European Physical Journal Plus. 136
The $$^{27}\hbox {Al}(\hbox {p},\alpha )^{24}\hbox {Mg}$$ 27 Al ( p , α ) 24 Mg reaction, which drives the destruction of $$^{27}$$ 27 Al and the production of $$^{24}\hbox {Mg}$$ 24 Mg in stellar hydrogen burning, has been investigated via the Troj
Autor:
R. G. Pizzone, M. Anastasiou, G. L. Guardo, E. Somorjai, M. L. Sergi, M. Lattuada, Z. Hons, S. Cherubini, M. La Cognata, K. I. Tursunmakhatov, Nabin Rijal, A. M. Mukhamedzhanov, G. G. Rapisarda, Roberta Spartà, P. Figuera, S. B. Sakuta, F. Mudò, B. Schmidt, S. Hayakawa, Giuseppe D’Agata, S. Palmerini, R. E. Tribble, R. Yarmukhamedov, Tamás Szücs, A. Cvetinović, J. Mrazek, G. G. Kiss, M. Gulino, Oscar Trippella, S. A. Kuvin, Zs. Fülöp, Lagy Baby, Gy. Gyürky, L. Lamia, C. Spitaleri, S. Romano, I. Wiedenhöver, A. Tumino, S. B. Igamov, Zoltán Halász, I. Indelicato
Publikováno v:
Physical Review C. 104
Background: The Li 6 ( p , γ ) Be 7 cross section influences a variety of astrophysical scenarios, including big-bang and stellar nucleosynthesis. In recent years, conflicting results of direct measurements have been published, reporting contradicto
Autor:
Stefan Typel, M. Lattuada, M. Gulino, D. Lattuada, G. L. Guardo, A. Di Pietro, Livio Lamia, Giuseppe D’Agata, Roberta Spartà, G. G. Rapisarda, A. Tumino, C. Spitaleri, S. Palmerini, S. Romano, Silvio Cherubini, M. La Cognata, P. Figuera, R. G. Pizzone, M. L. Sergi
Publikováno v:
The European Physical Journal A. 57
The neutron capture reaction $$^{10}$$ B(n, $$\alpha $$ ) $$^{7}$$ Li has been investigated via the Trojan Horse Method from 0 to 1 MeV. The $$\alpha _{0}$$ and $$\alpha _{1}$$ channels, corresponding to $$^{7}$$ Li in its g.s. and 1st excited level
Autor:
V. Kroha, V. Burjan, A. I. Kilic, Livio Lamia, V. Glagolev, A. Tumino, I. Siváček, Roberta Spartà, M. La Cognata, J. Mrazek, R. G. Pizzone, G. D’Agata, M. L. Sergi, C. Spitaleri, S. Romano, G. G. Rapisarda, G. L. Guardo, Sara Palmerini
Publikováno v:
Physical Review C. 103
The $^{26}\mathrm{Si}(p,\ensuremath{\gamma})^{27}\mathrm{P}$ reaction might be relevant in understanding the $^{26}\mathrm{Si}$ depletion and $^{26}\mathrm{Al}$ production in stars. The asymptotic normalization coefficients (ANC) for the $^{26}\mathr