A NOVEL APPROACH TO MEASURE THE CROSS SECTION OF THE18O(p, α)15N RESONANT REACTION IN THE 0-200 keV ENERGY RANGE

Cognata, M. La; Spitaleri, C.; Mukhamedzhanov, A. M.; Banu, A.; Cherubini, S.; Coc, A.; Crucillá, V.; Goldberg, V. Z.; Gulino, M.; Irgaziev, B. F.; Kiss, G. G.; Lamia, L.; Mrázek, J.; Pizzone, R. G.; Puglia, S. M. R.; Rapisarda, G. G.; Romano, S.; Sergi, M. L.; Tăbăcaru, G.; Trache, L.; Tribble, R. E.; Trzaska, W. H.; Туміно, А.

doi:10.1088/0004-637x/708/1/796

Cited by 79 publications

(69 citation statements)

References 59 publications

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“…Sellin et al (1969), Orihara et al (1973), Almanza et al (1975), and Murillo et al (1979) provided values for the higher resonance energies and partial widths, and Q values and masses are from Wang et al (2012). Our adopted strengths for the 20 and 90 keV resonances agree with La Cognata et al (2010a).…”

Section: C2supporting

confidence: 72%

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

Sallaska¹,

Iliadis²,

Chapmagne³

et al. 2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

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STARLIB is a next-generation, all-purpose nuclear reaction-rate library. For the first time, this library provides the rate probability density at all temperature grid points for convenient implementation in models of stellar phenomena. The recommended rate and its associated uncertainties are also included. Currently, uncertainties are absent from all other rate libraries, and, although estimates have been attempted in previous evaluations and compilations, these are generally not based on rigorous statistical definitions. A common standard for deriving uncertainties is clearly warranted. STARLIB represents a first step in addressing this deficiency by providing a tabular, up-to-date database that supplies not only the rate and its uncertainty but also its distribution. Because a majority of rates are lognormally distributed, this allows the construction of rate probability densities from the columns of STARLIB. This structure is based on a recently suggested Monte Carlo method to calculate reaction rates, where uncertainties are rigorously defined. In STARLIB, experimental rates are supplemented with: (1) theoretical TALYS rates for reactions for which no experimental input is available, and (2) laboratory and theoretical weak rates. STARLIB includes all types of reactions of astrophysical interest to Z = 83, such as (p, γ ), (p, α), (α, n), and corresponding reverse rates. Strong rates account for thermal target excitations. Here, we summarize our Monte Carlo formalism, introduce the library, compare methods of correcting rates for stellar environments, and discuss how to implement our library in Monte Carlo nucleosynthesis studies. We also present a method for accessing STARLIB on the Internet and outline updated Monte Carlo-based rates.

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Section: C2supporting

confidence: 72%

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

Sallaska¹,

Iliadis²,

Chapmagne³

et al. 2013

Proceedings of XII International Symposium on Nuclei in the Cosmos — PoS(NIC XII)

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“…In recent years, THM data allowed for a better understanding of different astrophysical problems, such as the study of light element burning reactions (Pizzone et al 2005(Pizzone et al , 2014Lamia et al 2008Lamia et al , 2012bLamia et al , 2012cLamia et al , 2013Tumino et al 2011aTumino et al , 2011bTumino et al , 2014Grineviciute et al 2015), CNO reactions (see La Cognata et al 2010Sergi et al 2010;Palmerini et al 2013), and removing/producing neutron reactions (Lamia et al 2008;Gulino et al 2010Gulino et al , 2013La Cognata et al 2012). …”

Section: The Thmmentioning

confidence: 99%

ASTROPHYSICAL IMPACT OF THE UPDATED⁹Be(p,α)⁶Li AND¹⁰B(p,α)⁷Be REACTION RATES AS DEDUCED BY THM

Lamia

Spitaleri

Tognelli

et al. 2015

ApJ

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The complete understanding of the stellar abundances of lithium, beryllium, and boron represents one of the most interesting open problems in astrophysics. These elements are largely used to probe stellar structure and mixing phenomena in different astrophysical scenarios, such as pre-main-sequence or main-sequence stars. Their different fragility against (p,α) burning reactions allows one to investigate different depths of the stellar interior. Such fusion mechanisms are triggered at temperatures between T ≈ (2-5) × 10 6 K, thus defining a corresponding Gamow energy between ≈ 3-10 keV, where S(E)-factor measurements need to be performed to get reliable reaction rate evaluations. The Trojan Horse Method is a well defined procedure to measure cross sections at Gamow energies overcoming the uncertainties due to low-energy S(E)-factor extrapolation as well as electron screening effects. Taking advantage of the THM measure of the 9 Be(p,α) 6 Li and 10 B(p,α) 7 Be cross sections, the corresponding reaction rates have been calculated and compared with the evaluations by the NACRE collaboration, widely used in the literature. The impact on surface abundances of the updated 9 Be and 10 B (p,α) burning rates is discussed for pre-MS stars.

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“…The THM cross section represents the bare-nucleus cross section, as extensively discussed by Spitaleri et al (2004Spitaleri et al ( , 2011. The application of the THM has shed light on different astrophysical problems, including the study of light element burning reactions (Pizzone et al 2003;Romano et al 2006;Lamia et al 2007Lamia et al , 2008Lamia et al , 2012bLamia et al , 2012cTumino et al 2011aTumino et al , 2011b, CNO reactions (see La Cognata et al 2005Sergi et al 2010;La Cognata et al 2010, and removing/producing neutron reactions Lamia et al 2008;Gulino et al 2010Gulino et al , 2012La Cognata et al 2012). …”

Section: The Trojan Horse Methodsmentioning

confidence: 99%

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

Lamia

Spitaleri

Pizzone

et al. 2013

ApJ

Self Cite

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The lithium problem influencing primordial and stellar nucleosynthesis is one of the most interesting unsolved issues in astrophysics. 6 Li is the most fragile of lithium's stable isotopes and is largely destroyed in most stars during the pre-main-sequence (PMS) phase. For these stars, the convective envelope easily reaches, at least at its bottom, the relatively low 6 Li ignition temperature. Thus, gaining an understanding of 6 Li depletion also gives hints about the extent of convective regions. For this reason, charged-particle-induced reactions in lithium have been the subject of several studies. Low-energy extrapolations of these studies provide information about both the zero-energy astrophysical S(E) factor and the electron screening potential, U e . Thanks to recent direct measurements, new estimates of the 6 Li(p, α) 3 He bare-nucleus S(E) factor and the corresponding U e value have been obtained by applying the Trojan Horse method to the 2 H( 6 Li, α 3 He)n reaction in quasi-free kinematics. The calculated reaction rate covers the temperature window 0.01 to 2T 9 and its impact on the surface lithium depletion in PMS models with different masses and metallicities has been evaluated in detail by adopting an updated version of the FRANEC evolutionary code.

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A NOVEL APPROACH TO MEASURE THE CROSS SECTION OF THE¹⁸O(p, α)¹⁵N RESONANT REACTION IN THE 0-200 keV ENERGY RANGE

Cited by 79 publications

References 59 publications

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

ASTROPHYSICAL IMPACT OF THE UPDATED⁹Be(p,α)⁶Li AND¹⁰B(p,α)⁷Be REACTION RATES AS DEDUCED BY THM

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

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A NOVEL APPROACH TO MEASURE THE CROSS SECTION OF THE18O(p, α)15N RESONANT REACTION IN THE 0-200 keV ENERGY RANGE

Cited by 79 publications

References 59 publications

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

STARLIB: A next-generation reaction-rate library for nuclear astrophysics

ASTROPHYSICAL IMPACT OF THE UPDATED9Be(p,α)6Li AND10B(p,α)7Be REACTION RATES AS DEDUCED BY THM

AN UPDATED6Li(p, α)3He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

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A NOVEL APPROACH TO MEASURE THE CROSS SECTION OF THE¹⁸O(p, α)¹⁵N RESONANT REACTION IN THE 0-200 keV ENERGY RANGE

ASTROPHYSICAL IMPACT OF THE UPDATED⁹Be(p,α)⁶Li AND¹⁰B(p,α)⁷Be REACTION RATES AS DEDUCED BY THM

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD