Rate of Radiative p 2 H Capture
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RATE OF RADIATIVE p2H CAPTURE S. B. Dubovichenko,1,2 L. M. Chechin, N. A. Burkova,2 A. V. Dzhazairov-Kakhramanov,1 Ch. T. Omarov,1 S. Zh. Nurakhmetova,2 B. U. Beisenov,2 A. Ertaiuly,2 and B. Eleusheva2
UDC 539.17; 519.6; 52-1/-8:539.14; 524.1:539.14
Within the framework of the modified potential cluster model with forbidden states, we consider radiative p2H capture at energies from 1 keV to 10 MeV. It is shown that on the basis of potentials that have been matched with the energy of the bound state and its asymptotic constant, it is possible to correctly reproduce the available experimental data. On the basis of the obtained total cross sections, a calculation of the reaction rate of p2H capture in the temperature range from 0.01 T9 to 10 T9 is performed. Results of this calculation are approximated by simple expressions, which simplifies their use in other studies. Keywords: nuclear astrophysics, light atomic nuclei, low and astrophysical energies, elastic scattering, p2H system, potential description, radiative capture, total cross sections, thermonuclear reactions, potential cluster model, forbidden states, classification of orbital states according to Young tableaux.
INTRODUCTION As is well known, the thermonuclear process of p+2Н 3He+ radiative capture is the first nuclear reaction of the proton-proton (рр) cycle, which takes place as a result of electromagnetic interactions and weakens the observed rate of heating of the Sun and the majority of stars of the Main Sequence of our Universe [1]. In the рр cycle, the process of p2Н radiative capture is important for the transition from primordial fusion of protons p+p 2H+e–+e, which proceeds due to weak interactions, to one of the final two 3Не nuclei in the рр chain of the capture reaction [2]: 3 He+3He 4He+2p, proceeding due to strong interactions. A detailed study of the p2Н radiative capture reaction continues without letup and at the beginning of the 2000’s decade, thanks to the European project LUNA, new experimental data have been obtained for the astrophysical S-factor at energies from 2.5 keV. We have already considered this process in several works, beginning in 1995 [3] and extending up to 2011 [4, 5]. These results were then presented in two reviews [6, 7] and a monograph [8], which in 2019 was revised into a fourth edition in the Russian language and a second edition in English [9]. But we never previously investigated the rate of this reaction, which we will now do here on the basis of the modified potential cluster model (MPCM), used in all of our previous work, with classification of orbital states according to Young tableaux and leading to allowed (ASs) and forbidden states (FSs) [8–11].
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V. G. Fesenkov Astrophysical Institute of the National Center for Space Research and Technology of the Aerospace Agency of the Ministry of Digital Development, Innovations and Aerospace Industry of The Republic of Kazakhstan, Almaty, The Republic of Kazakhstan (RK), e-mail: [email protected]; [email protected]; [email protected]; chingis.om
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