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

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F61389005%3A_____%2F18%3A00486563" target="_blank" >RIV/61389005:_____/18:00486563 - isvavai.cz</a>

Result on the web

<a href="http://dx.doi.org/10.1088/1674-1137/42/1/015001" target="_blank" >http://dx.doi.org/10.1088/1674-1137/42/1/015001</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/1674-1137/42/1/015001" target="_blank" >10.1088/1674-1137/42/1/015001</a>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

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Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2018

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Chinese Physics C

ISSN

1674-1137

e-ISSN

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Volume of the periodical

42

Issue of the periodical within the volume

1

Country of publishing house

CN - CHINA

Number of pages

10

Pages from-to

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UT code for WoS article

000423839100017

EID of the result in the Scopus database

2-s2.0-85039979449