@article{MTMT:34816299,
	title = {Low-lying dipole response of Ni 64},
	url = {https://m2.mtmt.hu/api/publication/34816299},
	author = {Müscher, M. and Litvinova, E. and Schwengner, R. and Beck, T. and Bemmerer, D. and Fiedler, F. and Finch, S.W. and Friman-Gayer, U. and Hammer, S. and Isaak, J. and Janssens, R.V.F. and Junghans, A.R. and Kelly, N. and Kluwig, F. and Krishichayan, X and Müller, S.E. and Papst, O. and Römer, K. and Savran, D. and Scheck, M. and Schüttler, T. and Sinclair, J. and Szücs, Tamás and Tornow, W. and Wagner, A. and Wilhelmy, J. and Zilges, A.},
	doi = {10.1103/PhysRevC.109.044318},
	journal-iso = {PHYS REV C},
	journal = {PHYSICAL REVIEW C},
	volume = {109},
	unique-id = {34816299},
	issn = {2469-9985},
	year = {2024},
	eissn = {2469-9993},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34206815,
	title = {Experimental 7Be production cross section from the Li 7 ( p , n ) 7 Be reaction at Ep = 3.5 − 13 MeV},
	url = {https://m2.mtmt.hu/api/publication/34206815},
	author = {Tóth, Ákos and Gyürky, György and Papp, Enikő Ivett and Szücs, Tamás},
	doi = {10.1016/j.nuclphysa.2023.122778},
	journal-iso = {NUCL PHYS A},
	journal = {NUCLEAR PHYSICS A},
	volume = {1041},
	unique-id = {34206815},
	issn = {0375-9474},
	keywords = {Cross section; Activation method; Thin target},
	year = {2024},
	eissn = {1873-1554},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34417047,
	title = {First measurement of the low-energy direct capture in Ne 20 ( p , γ ) Na 21 and improved energy and strength of the E c.m. = 368 keV resonance},
	url = {https://m2.mtmt.hu/api/publication/34417047},
	author = {Masha, E. and Barbieri, L. and Skowronski, J. and Aliotta, M. and Ananna, C. and Barile, F. and Bemmerer, D. and Best, A. and Boeltzig, A. and Broggini, C. and Bruno, C. G. and Caciolli, A. and Campostrini, M. and Casaburo, F. and Cavanna, F. and Ciani, G. F. and Ciapponi, A. and Colombetti, P. and Compagnucci, A. and Corvisiero, P. and Csedreki, László and Davinson, T. and Depalo, R. and Di Leva, A. and Elekes, Zoltán and Ferraro, F. and Fiore, E. M. and Formicola, A. and Fülöp, Zsolt and Gervino, G. and Guglielmetti, A. and Gustavino, C. and Gyürky, György and Imbriani, G. and José, J. and Junker, M. and Lugaro, Maria and Manoj, P. and Marigo, P. and Menegazzo, R. and Paticchio, V. and Piatti, D. and Prati, P. and Rapagnani, D. and Rigato, V. and Robb, D. and Schiavulli, L. and Sidhu, R. S. and Straniero, O. and Szücs, Tamás and Zavatarelli, S.},
	doi = {10.1103/PhysRevC.108.L052801},
	journal-iso = {PHYS REV C},
	journal = {PHYSICAL REVIEW C},
	volume = {108},
	unique-id = {34417047},
	issn = {2469-9985},
	year = {2023},
	eissn = {2469-9993},
	orcid-numbers = {Masha, E./0000-0002-6532-4255; Barbieri, L./0009-0001-0213-7137; Skowronski, J./0000-0001-7292-6353; Ananna, C./0000-0003-2513-7348; Bemmerer, D./0000-0003-0470-8367; Best, A./0000-0001-8869-9757; Boeltzig, A./0000-0002-7209-2499; Broggini, C./0000-0001-8512-0308; Bruno, C. G./0000-0003-3241-3371; Caciolli, A./0000-0003-4673-714X; Campostrini, M./0000-0001-8902-6618; Casaburo, F./0000-0002-2260-9322; Cavanna, F./0000-0002-2548-4764; Ciani, G. F./0000-0002-1772-9872; Colombetti, P./0000-0002-9944-1265; Compagnucci, A./0000-0002-6577-4483; Davinson, T./0000-0002-8769-6893; Depalo, R./0000-0003-3943-7982; Di Leva, A./0000-0002-8762-0522; Fiore, E. M./0000-0002-3548-2690; Guglielmetti, A./0000-0002-6008-1629; Gustavino, C./0000-0003-3232-7027; Imbriani, G./0000-0002-7037-6770; José, J./0000-0002-9937-2685; Junker, M./0000-0003-2609-2698; Lugaro, Maria/0000-0002-6972-3958; Manoj, P./0009-0001-6234-0735; Menegazzo, R./0000-0002-3060-5276; Paticchio, V./0000-0002-2916-1671; Piatti, D./0000-0002-5405-2506; Prati, P./0000-0002-8097-9460; Rapagnani, D./0000-0001-8183-0994; Rigato, V./0000-0003-0671-7750; Robb, D./0009-0002-1235-7480; Sidhu, R. S./0000-0002-1637-7502; Straniero, O./0000-0002-5514-6125; Szücs, Tamás/0000-0002-9980-4847; Zavatarelli, S./0000-0002-5722-8896}
}

@article{MTMT:34181127,
	title = {Towards a direct measurement of the E cm = 65 keV resonance strength in 17 O(p, γ) 18 F at LUNA},
	url = {https://m2.mtmt.hu/api/publication/34181127},
	author = {Ciani, G.F. and Piatti, D. and Fülöp, Zsolt and Gyürky, György and Szücs, Tamás and Halász, Zoltán and Somorjai, Endre and LUNA, Coll},
	doi = {10.1088/1742-6596/2586/1/012095},
	journal-iso = {J PHYS CONF SER},
	journal = {JOURNAL OF PHYSICS-CONFERENCE SERIES},
	volume = {2586},
	unique-id = {34181127},
	issn = {1742-6588},
	abstract = {The 17 O( p, γ ) 18 F reaction plays a crucial role in several stellar scenarios where the hydrogen burning phases takes place. In particular, in the temperature energy range of interest for AGB nucleosynthesis (20 MK< T <80 MK) the main contribution to the astrophysical reaction rate comes from the elusive 65 keV resonance. Indeed, this resonance strength is at the moment determined only through indirect measurements, with a reported value of ωγ = (1.6 ± 0.3) × 10 −11 eV. With typical experimental quantities for beam current, isotopic enrichment and detection efficiency, this strength yields an expected count rate of less than one count per Coulomb, making the direct measurement of this resonance extremely challenging. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400kV accelerator installed in Laboratori Nazionali del Gran Sasso (Italy) provides a unique possibility to directly measure this low resonance thanks to the reduction of cosmic ray background by six orders of magnitude with respect surface laboratories and thanks to an intense, narrow proton beam. To improve the experimental sensitivity, the environmental background was further reduced designing a lead and borated (5%) polyethylene shielding and the absorption of γ − rays emitted by the reaction was minimised by the installation of target chamber and holder made of aluminum.},
	year = {2023},
	eissn = {1742-6596},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34181125,
	title = {The 13 C(α,n) 16 O cross section measurement at low energies at LUNA},
	url = {https://m2.mtmt.hu/api/publication/34181125},
	author = {Ciani, G.F. and Fülöp, Zsolt and Gyürky, György and Szücs, Tamás and Halász, Zoltán and Somorjai, Endre and LUNA, Coll},
	doi = {10.1088/1742-6596/2586/1/012094},
	journal-iso = {J PHYS CONF SER},
	journal = {JOURNAL OF PHYSICS-CONFERENCE SERIES},
	volume = {2586},
	unique-id = {34181125},
	issn = {1742-6588},
	abstract = {One of the main neutron sources for the astrophysical s-process is the 13 C( α ,n) 16 O. This reaction takes place in thermally pulsing asymptotic giant branch (TP-AGB) stars in a stellar environmental with temperature of about 90 MK. To model the nucleosynthesis process connected with the reaction, it is important the cross section reaction evaluation inside the so called Gamow peak, in the energy window 150-240 keV. In this work the results of the first 13 C( α ,n) 16 O direct measurement performed by the LUNA collaboration in the underground laboratory of LNGS are presented.},
	year = {2023},
	eissn = {1742-6596},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34181119,
	title = {Study of proton capture on carbon-13 isotope at LUNA},
	url = {https://m2.mtmt.hu/api/publication/34181119},
	author = {Rapagnani, David and Skowronski, Jakub and Boeltzig, Axel and Kiss, Gábor Gyula and Fülöp, Zsolt and Gyürky, György and Szücs, Tamás and Halász, Zoltán and Somorjai, Endre and LUNA, Coll},
	doi = {10.1088/1742-6596/2586/1/012103},
	journal-iso = {J PHYS CONF SER},
	journal = {JOURNAL OF PHYSICS-CONFERENCE SERIES},
	volume = {2586},
	unique-id = {34181119},
	issn = {1742-6588},
	abstract = {13 C(p,γ) 14 N is a key reaction in different stellar environments for which both accurate and precise measurements of its cross section are required to constraint stellar models. This is currently ongoing at the Laboratory for Underground Nuclear Astrophysics where in addition to the low-background environment, the use of different detection systems (HPGe and BGO detectors) and analysis techniques (Peak Shape Analysis and Sum Peak Method) allowed to perform reaction cross section measurements at the lowest energy ever. Both the setup employed in the measurements and the analysis performed are presented in this paper.},
	year = {2023},
	eissn = {1742-6596},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34181117,
	title = {Determination of the astrophysical factor of the 3 He(α,γ) 7 Be down to zero energy using the asymptotic normalization coefficient method},
	url = {https://m2.mtmt.hu/api/publication/34181117},
	author = {La Cognata, M. and Kiss, Gábor Gyula and Yarmukhamedov, R. and Tursunmakhatov, K. I. and Wiedenhöver, I. and Baby, L. T. and Cherubini, S. and Cvetinović, A. and D’Agata, G. and Figuera, P. and Guardo, G. L. and Gulino, M. and Hayakawa, S. and Indelicato, I. and Lamia, L. and Lattuada, M. and Mudò, F. and Palmerini, S. and Pizzone, R. G. and Rapisarda, G. G. and Romano, S. and Sergi, M. L. and Spartà, R. and Spitaleri, C. and Trippella, O. and Tumino, A. and Anastasiou, M. and Kuvin, S.A. and Rijal, N. and Schmidt, B. and Igamov, S. B. and Sakuta, S. B. and Fülöp, Zsolt and Gyürky, György and Szücs, Tamás and Halász, Zoltán and Somorjai, Endre and Hons, Z. and Mrázek, J. and Tribble, R. E. and Mukhamedzhanov, A. M.},
	doi = {10.1088/1742-6596/2586/1/012093},
	journal-iso = {J PHYS CONF SER},
	journal = {JOURNAL OF PHYSICS-CONFERENCE SERIES},
	volume = {2586},
	unique-id = {34181117},
	issn = {1742-6588},
	abstract = {The observation of neutrinos emitted in the p − p chain and in the CNO cycle can be employed to test the Standard Solar Model. The 3 He( α,γ ) 7 Be reaction is the first reaction of the 2nd and 3rd branch of the p − p chain, so the indetermination of its cross section significantly affects the predicted 7 Be and 8 B neutrino fluxes. Notwithstanding its relevance and the great deal of experimental and theoretical papers, information of the reaction cross section at energies of the core of the Sun (15 keV - 30 keV) is sparse and additional experimental work is necessary to attain the target (~ 3%) accuracy. The precise understanding of the external capture component to the 3 He( α,γ ) 7 Be reaction cross section is pivotal for the theoretical assessment of the reaction mechanism. In this work, the indirect measurement of this external capture component using the Asymptotic Normalization Coefficient (ANC) technique is discussed. To extract the ANC, the angular distributions of deuterons yielded in the 6 Li( 3 He, d ) 7 Be α -transfer reaction were detected with high precision at E 3 He =3.0 MeV and 5.0 MeV. The ANCs were then deduced from the juxtaposition of DWBA and CC calculations with the experimental angular distributions and the zero energy astrophysical S-factor for 3 He( α,γ ) 7 Be reaction was calculated to equal 0.534 ± 0.025 keVb. Both our experimental and theoretical approaches were tested through the analysis of the 6 Li(p, γ ) 7 Be astrophysical factor, with further interesting astrophysical implications.},
	year = {2023},
	eissn = {1742-6596},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34148036,
	title = {Proton-Capture Rates on Carbon Isotopes and Their Impact on the Astrophysical 12C/13C Ratio},
	url = {https://m2.mtmt.hu/api/publication/34148036},
	author = {Skowronski, J. and Boeltzig, A. and Ciani, G. F. and Csedreki, László and Piatti, D. and Aliotta, M. and Ananna, C. and Barile, F. and Bemmerer, D. and Best, A. and Broggini, C. and Bruno, C. G. and Caciolli, A. and Campostrini, M. and Cavanna, F. and Colombetti, P. and Compagnucci, A. and Corvisiero, P. and Davinson, T. and Depalo, R. and Di Leva, A. and Elekes, Zoltán and Ferraro, F. and Formicola, A. and Fülöp, Zsolt and Gervino, G. and Gesuè, R. M. and Guglielmetti, A. and Gustavino, C. and Gyürky, György and Imbriani, G. and Junker, M. and Lugaro, Maria and Marigo, P. and Masha, E. and Menegazzo, R. and Paticchio, V. and Perrino, R. and Prati, P. and Rapagnani, D. and Rigato, V. and Schiavulli, L. and Sidhu, R. S. and Straniero, O. and Szücs, Tamás and Zavatarelli, S.},
	doi = {10.1103/PhysRevLett.131.162701},
	journal-iso = {PHYS REV LETT},
	journal = {PHYSICAL REVIEW LETTERS},
	volume = {131},
	unique-id = {34148036},
	issn = {0031-9007},
	year = {2023},
	eissn = {1079-7114},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34139317,
	title = {The challenging direct measurement of the 65 keV resonance strength of the 17 O( p , γ ) 18 F reaction at LUNA},
	url = {https://m2.mtmt.hu/api/publication/34139317},
	author = {Gesuè, Riccardo Maria and Csedreki, László and Elekes, Zoltán and Fülöp, Zsolt and Gyürky, György and Szücs, Tamás and LUNA, Coll},
	doi = {10.1051/epjconf/202327502004},
	journal-iso = {EPJ WEB CONF},
	journal = {EPJ WEB OF CONFERENCES},
	volume = {275},
	unique-id = {34139317},
	issn = {2101-6275},
	abstract = {The 17 O( p , γ ) 18 F reaction plays a crucial role in AGB nucleosynthesis as well as in explosive hydrogen burning occurring in type Ia novae. At the temperatures of interest for the former scenario ( 20MK < T < 80MK) the main contribution to the astrophysical reaction rate comes from the poorly constrained E R = 65 keV resonance. The strength of this resonance is presently determined only through indirect measurements, with an adopted value ωγ =(16 ± 3) peV.},
	year = {2023},
	eissn = {2100-014X},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}

@article{MTMT:34094940,
	title = {Direct measurement of the 13 C(α,n) 16 O reaction in the Gamow window of the s-process nucleosynthesis},
	url = {https://m2.mtmt.hu/api/publication/34094940},
	author = {Ciani, G.F. and Formicola, A. and Skowronski, J and Gesuè, R M and Boeltzig, A and Piatti, D and Rapagnani, D and Aliotta, M and Ananna, C and Barile, F and Bemmerer, D and Best, A and Broggini, C and Bruno, C G and Caciolli, A and Campostrini, M and Cavanna, F and Colombetti, P and Compagnucci, A and Corvisiero, P and Csedreki, László and Davinson, T and Depalo, R and Di Leva, A and Elekes, Zoltán and Ferraro, F and Fülöp, Zsolt and Gervino, G and Guglielmetti, A and Gustavino, C and Gyürky, Gy and Imbriani, G and Junker, M and Lugaro, M and Marigo, P and Masha, E and Menegazzo, R and Paticchio, V and Perrino, R and Prati, P and Rigato, V and Schiavulli, L and Sidhu, R S and Straniero, O and Szücs, Tamás and Zavatarelli, S},
	doi = {10.1088/1742-6596/2453/1/012018},
	journal-iso = {J PHYS CONF SER},
	journal = {JOURNAL OF PHYSICS-CONFERENCE SERIES},
	volume = {2453},
	unique-id = {34094940},
	issn = {1742-6588},
	abstract = {One of the main neutron sources for the astrophysical s process is the 13 C( α ,n) 16 O reaction, which takes place in thermally pulsing asymptotic giant branch (TP-AGB) stars at environmental temperature around 90 MK. To model the nucleosynthesis process connected with the reaction, it is important to know with high accuracy the cross section reaction in the energy window 240-150 keV, the so called Gamow window. At these sub-Coulomb energies, direct cross section measurements are severely affected by the low event rate and low signal-to-noise ratio. In this work, a new study of the astrophysical S(E)-factor for the 13 C( α ,n) 16 O reaction is presented.},
	year = {2023},
	eissn = {1742-6596},
	orcid-numbers = {Szücs, Tamás/0000-0002-9980-4847}
}