THE FLUORINE DESTRUCTION IN STARS: FIRST EXPERIMENTAL STUDY OF THE
 19
 F(
 p
 , α
 0
 )
 16
 O REACTION AT ASTROPHYSICAL ENERGIES

Cognata, M. La; Mukhamedzhanov, A. M.; Spitaleri, C.; Indelicato, I.; Aliotta, M.; Burjan, V.; Cherubini, S.; Coc, A.; Gulino, M.; Hons, Z.; Kiss, G. G.; Kroha, V.; Lamia, L.; Mrázek, J.; Palmerini, S.; Piskoř, Š.; Pizzone, R. G.; Puglia, S. M. R.; Rapisarda, G. G.; Romano, S.; Sergi, M. L.; Туміно, А.

doi:10.1088/2041-8205/739/2/l54

Cited by 91 publications

(55 citation statements)

References 38 publications

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“…the presence of resonances not seen before in this process at energies corresponding to typical AGB temperatures, thus implying a significant increase in the reaction rate. Thus, the reaction rate proposed by La Cognata et al (2011) is used in our calculations. The uncertainty at relevant temperatures is about 30%.…”

Section: Reaction Rate Uncertaintiesmentioning

confidence: 99%

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Cristallo

Leva

Imbriani

et al. 2014

A&A

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Context. The origin of fluorine is a longstanding problem in nuclear astrophysics. It is widely recognized that asymptotic giant branch (AGB) stars are among the most important contributors to the Galactic fluorine production. Aims. In general, extant nucleosynthesis models overestimate the fluorine production by AGB stars with respect to observations. Although those differences are rather small at solar metallicity, low metallicity AGB stellar models predict fluorine surface abundances up to one order of magnitude larger than the observed ones. Methods. As part of a project devoted to reducing the uncertainties in the nuclear physics that affect the nucleosynthesis in AGB stellar models, we review the relevant nuclear reaction rates involved in the fluorine production or destruction. We perform this analysis on a model with initial mass M = 2 M and Z = 0.001. Results. We found that the major uncertainties are due to the 13 C(α,n) 16 O, the 19 F(α,p) 22 Ne, and the 14 N(p,γ) 15 O reactions. A change in the corresponding reaction rates within the present experimental uncertainties implies surface 19 F variations at the AGB tip lower than 10%, thus much smaller than observational uncertainties. For some α capture reactions, however, cross sections at astrophysically relevant energies are determined on the basis of nuclear models, in which some low-energy resonance parameters are very poorly known. Thus, larger variations in the rates of those processes cannot be excluded. That being so, we explore the effects of the variation in some α capture rates well beyond the current published uncertainties. The largest 19 F variations are obtained by varying the 15 N(α,γ) 19 F and the 19 F(α,p) 22 Ne reactions. Conclusions. The currently estimated uncertainties of the nuclear reaction rates involved in the production and destruction of fluorine produce minor 19 F variations in the ejecta of AGB stars. Analysis of some α capture processes that assume a wider uncertainty range determines 19 F abundances in better agreement with recent spectroscopic fluorine measurements at low metallicity. In the framework of this scenario, the 15 N(α,γ) 19 F and the 19 F(α,p) 22 Ne reactions show the strongest effects on fluorine nucleosynthesis. The presence of poorly known low-energy resonances make such a scenario possible, even if it is unlikely. We plan to measure these resonances directly.

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Section: Reaction Rate Uncertaintiesmentioning

confidence: 99%

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Cristallo

Leva

Imbriani

et al. 2014

A&A

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“…The Trojan Horse Method (THM) has been widely developed and exploited over the past two decades to study bare nuclear cross sections at very low energy and it is now routinely used to study reactions between charged particles even at zero energy. A detailed description of the method can be found elsewhere [1][2][3][4][5][6][7][8][9][10][11][12] and goes be- * Electronic address: cherubini@lns.infn.it yond the scope of this paper: a review of the method can be found in [13]. Here we present a pioneering work where the THM has been applied for the first time to a reaction induced by a RIB, namely the 18 F(p,α) 15 O process at nova energies.…”

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confidence: 99%

First application of the Trojan horse method with a radioactive ion beam: Study of the18F(p,α)15Oreaction at astrophysical energies

et al. 2015

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“…Actually, additional resonances might be populated in 20 Ne [32]. A recent experiment [33] measured the 19 F(p,α 0 ) 16 O astrophysical S (E)-factor by indirect means of the Trojan Horse method, and found that the largest rate difference, about 70%, occurs at temperatures relevant for post-AGB stars (∼0.1 GK), exceeding the upper limit set by the previous uncertainties [28]. Such difference is clearly due to the presence of the 113 keV resonance (E x =12.957 MeV, 2 + ).…”

Section: (Pα 0 ) Channelmentioning

confidence: 97%

A proposed direct measurement of cross section at Gamow window for key reaction 19F(p,α) 16O in Asymptotic Giant Branch stars with a planned accelerator in CJPL

et al. 2016

Sci. China Phys. Mech. Astron.

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In 2014, the National Natural Science Foundation of China (NSFC) approved the Jinping Underground Nuclear Astrophysics laboratory (JUNA) project, which aims at direct cross-section measurements of four key stellar nuclear reactions right down to the Gamow windows. In order to solve the observed fluorine overabundances in Asymptotic Giant Branch (AGB) stars, measuring the key 19 F(p,α) 16 O reaction at effective burning energies (i.e., at Gamow window) is established as one of the scientific research sub-projects. The present paper describes this sub-project in details, including motivation, status, experimental setup, yield and background estimation, aboveground test, as well as other relevant reactions.Jinping Underground Nuclear Astrophysics laboratory (JUNA), direct measurement, Gamow window, cross section, AGB star, nucleosynthesis PACS number(s): 26.20.+f; 26.30.+k; 25.40.Ny, 27.20+n Citation:He J J, et al. A proposed direct measurement of cross section at Gamow window for key reaction 19 F(p,α) 16 O in Asymptotic Giant Branch stars with a planned accelerator in CJPL, Sci China-Phys Mech Astron, 2015, 58: 1-7, doi:

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THE FLUORINE DESTRUCTION IN STARS: FIRST EXPERIMENTAL STUDY OF THE ¹⁹ F( p , α ₀ ) ¹⁶ O REACTION AT ASTROPHYSICAL ENERGIES

Cited by 91 publications

References 38 publications

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

First application of the Trojan horse method with a radioactive ion beam: Study of the18F(p,α)15Oreaction at astrophysical energies

A proposed direct measurement of cross section at Gamow window for key reaction 19F(p,α) 16O in Asymptotic Giant Branch stars with a planned accelerator in CJPL

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THE FLUORINE DESTRUCTION IN STARS: FIRST EXPERIMENTAL STUDY OF THE 19 F( p , α 0 ) 16 O REACTION AT ASTROPHYSICAL ENERGIES

Cited by 91 publications

References 38 publications

Effects of nuclear cross sections on19F nucleosynthesis at low metallicities

Effects of nuclear cross sections on19F nucleosynthesis at low metallicities

First application of the Trojan horse method with a radioactive ion beam: Study of the18F(p,α)15Oreaction at astrophysical energies

A proposed direct measurement of cross section at Gamow window for key reaction 19F(p,α) 16O in Asymptotic Giant Branch stars with a planned accelerator in CJPL

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THE FLUORINE DESTRUCTION IN STARS: FIRST EXPERIMENTAL STUDY OF THE ¹⁹ F( p , α ₀ ) ¹⁶ O REACTION AT ASTROPHYSICAL ENERGIES

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities