Počet záznamů: 1  

Thermonuclear F-19(p,alpha(0))O-16 reaction rate

  1. 1.
    0486563 - ÚJF 2019 RIV CN eng J - Článek v odborném periodiku
    He, J. J. - Lombardo, I. - Dell'Aquila, D. - Xu, Yi - Zang, L. Y. - Liu, W. P.
    Thermonuclear F-19(p,alpha(0))O-16 reaction rate.
    Chinese Physics C. Roč. 42, č. 1 (2018), č. článku 015001. ISSN 1674-1137. E-ISSN 2058-6132
    Institucionální podpora: RVO:61389005
    Klíčová slova: asymptotic giant branch (AGB) star * nucleosynthesis * astrophysical S factor * cross section * reaction rate
    Obor OECD: Astronomy (including astrophysics,space science)
    Impakt faktor: 5.861, rok: 2018

    The thermonuclear F-19(p,0)O-16 reaction rate in the temperature region 0.007-10 GK has been derived by re-evaluating the availa alpha(b)le experimental data, together with the low-energy theoretical R-matrix extrapolations. Our new rate deviates by up to about 30% compared to the previous results, although all rates are consistent within the uncertainties. At very low temperature (e.g. 0.01 GK) our reaction rate is about 20% lower than the most recently published rate, because of a difference in the low energy extrapolated S-factor and a more accurate estimate of the reduced mass used in the calculation of the reaction rate. At temperatures above similar to 1 GK, our rate is lower, for instance, by about 20% around 1.75 GK, because we have re-evaluated the previous data (Isoya et al., Nucl. Phys. 7, 116 (1958)) in a meticulous way. The present interpretation is supported by the direct experimental data. The uncertainties of the present evaluated rate are estimated to be about 20% in the temperature region below 0.2 GK, and are mainly caused by the lack of low-energy experimental data and the large uncertainties in the existing data. Asymptotic giant branch (AGB) stars evolve at temperatures below 0.2 GK, where the F-19(p,alpha.)O-16 reaction may play a very important role. However, the current accuracy of the reaction rate is insufficient to help to describe, in a careful way, the fluorine over-abundances observed in AGB stars. Precise cross section (or S factor) data in the low energy region are therefore needed for astrophysical nucleosynthesis studies.
    Trvalý link: http://hdl.handle.net/11104/0281344

     
     
Počet záznamů: 1  

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