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    188宝金博页面版: New measurements and phase shift analysis of p~(16)O elastic scattering at astrophysical energies

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    内容提示： Chinese Physics C Vol. 41, No. 1 (2017) 014001New measurements and phase shift analysis of p 16 O elastic scatteringat astrophysical energies*Sergey Dubovichenko 1,2;1) Nassurlla Burtebayev 2;2) Albert Dzhazairov-Kakhramanov 1,2;3) Denis Zazulin 2,3Zhambul Kerimkulov 2 Marzhan Nassurlla 2 Chingis Omarov 1 Alesya Tkachenko 1Tatyana Shmygaleva 1,3 Stanislaw Kliczewski 4 Turlan Sadykov 51 Fesenkov Astrophysical Institute “NCSRT”ASC MID, Republic of Kazakhstan2Institute of Nuclear Physics ME RK, Almaty, Repu...

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    Chinese Physics C Vol. 41, No. 1 (2017) 014001New measurements and phase shift analysis of p 16 O elastic scatteringat astrophysical energies*Sergey Dubovichenko 1,2;1) Nassurlla Burtebayev 2;2) Albert Dzhazairov-Kakhramanov 1,2;3) Denis Zazulin 2,3Zhambul Kerimkulov 2 Marzhan Nassurlla 2 Chingis Omarov 1 Alesya Tkachenko 1Tatyana Shmygaleva 1,3 Stanislaw Kliczewski 4 Turlan Sadykov 51 Fesenkov Astrophysical Institute “NCSRT”ASC MID, Republic of Kazakhstan2Institute of Nuclear Physics ME RK, Almaty, Republic of Kazakhstan3Kazakh National University al-Farabi, Almaty, Republic of Kazakhstan4H. Niewodnicza´ nski Institute of Nuclear Physics, Polish Academy of Sciences, Cracow, Poland5Institute of Physics and Technology, Almaty, Republic of KazakhstanAbstract: The results of new experimental measurements of p 16 O elastic scattering in the energy range of 0.6–1.0MeV at angles of 40 ? –160 ? are given. Phase shift analysis of p 16 O elastic scattering was made using these and otherexperimental data on dif f erential cross sections in excitation functions and angular distributions at energies of up to2.5 MeV.Keywords: astrophysical energies; phase shift analysis; angular distributions; cluster model.PACS: 21.45.Bc; 25.40.Cm DOI: 10.1088/1674-1137/41/1/0140011 IntroductionAbout 20 years ago in our previous work [1], weshowed a possible way to describe lithium nuclei in theframework of the potential cluster model (PCM) [2, 3].This PCM takes into account forbidden states (FSs) [3,4] in intercluster potentials that we used in Ref. [5].Finally, the possibility of describing the astrophysical S-factors or total cross sections for radiative capture ofp 2 H, n 2 H, p 3 H, p 6 Li, n 6 Li, p 7 Li, n 7 Li, p 9 Be, n 9 Be, p 10 B,n 10 B, p 11 B, n 11 B, p 12 C, n 12 C, p 13 C, n 13 C, p 14 C, n 14 C,n 15 N, p 15 N, n 14 N, n 16 O and2 H 4 He, 3 He 4 He, 3 H 4 He,4 He 12 C systems at thermal and astrophysical energieswas shown in [2,3,5–15]. Calculations of these 27 pro-cesses were made on the basis of a modif i ed PCM variantwith classif i cation of states according to Young tableauxand forbidden, in some cases, states (MPCM), describedin detail in Refs. [5, 9–16].Some success of this MPCM can be explained bythe fact that intercluster interaction potentials are con-structed not only on the basis of known elastic scatteringphase shifts but also taking into account classif i cation ofcluster states according to Young tableaux [17]. Thus,the elastic scattering phase shifts, extracted from the ex-perimental dif f erential cross sections, taking into accountsuch a classif i cation, allow one to construct interactionpotentials of two particles in a continuous spectrum.Continuing the study of thermonuclear reactions inthe frame of the MPCM with FSs [18], let us considerthe16 O(p, γ) 17 F process, which is part of the CNO cycle[19] and has additional interest, since it is the reactionat the last nucleus of the 1p-shell with the forming of17 F that gives its limit. As we usually assume [16,19],the bound state (BS) of17 F is caused by the clusterchannel of the initial particles which take part in thereaction.Many stars, including the Sun, will eventually passthrough an evolutionary phase that is referred to asthe asymptotic giant branch [20]. This phase involvesa hydrogen and a helium shell that burn alternately sur-rounding an inactive stellar core. The16 O(p, γ) 17 F re-action rate sensitively inf l uences the17 O/ 16 O isotopicratio predicted by models of massive (>4M ? ) AGB stars,where proton captures occur at the base of the con-vective envelope (hot bottom burning). A f i ne-tuningof the16 O(p,γ) 17 F reaction rate may account for themeasured anomalous17 O/ 16 O abundance ratio in smallgrains which are formed by the condensation of the ma-terial ejected from the surface of AGB stars via strongstellar winds [21].Received 13 April 2016, Revised 20 June 2016∗ Supported by the Ministry of Education and Science of the Republic of Kazakhstan (0073/PCF-IS-MES)1)E-mail:dubovichenko@mail.ru2)E-mail:burteb@inp.kz3)E-mail:albert-j@yandex.ru© 2017 Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Sciences and the Institute ofModern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd014001-1

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