NEW DETERMINATION OF THE2H(d,p)3H AND2H(d,n)3He REACTION RATES AT ASTROPHYSICAL ENERGIES

Туміно, А.; Spartà, R.; Spitaleri, C.; Mukhamedzhanov, A. M.; Typel, S.; Pizzone, R. G.; Tognelli, E.; Degl’Innocenti, S.; Burjan, V.; Kroha, V.; Hons, Z.; Cognata, M. La; Lamia, L.; Mrázek, J.; Piskoř, Š.; Moroni, P. G. Prada; Rapisarda, G. G.; Romano, S.; Sergi, M. L.

doi:10.1088/0004-637x/785/2/96

Cited by 85 publications

(60 citation statements)

References 35 publications

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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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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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“…It has already been applied several times to reactions of relevance for astrophysics ( [26][27][28][29][30][31][32][33][34][35] and references therein). The purpose of the THM is to determine the cross section for the binary reaction (2 particles → 2 particles) A + x → C + c, from the measured cross section for the TH reaction 2 particles → 3 particles A + a → C + c + s in the quasifree (QF) kinematics regime, where the "Trojan Horse" (TH) particle, a = (x s), has a strong (s x) cluster structure.…”

Section: The Trojan Horse Methodsmentioning

confidence: 99%

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method

Туміно

Spitaleri

Cherubini

et al. 2016

EPJ Web of Conferences

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A measurement of the 12 C( 14 N,α 20 Ne) 2 H and 12 C( 14 N,p 23 Na) 2 H reactions has been performed at a 14 N beam energy of 30.0 MeV. The experiment aims to explore the extent to which contributing 24 Mg excited states can be populated in the quasi-free reaction off the deuteron in 14 N. In particular, the 24 Mg excitation region explored in the measurement plays a key role in stellar carbon burning whose cross section is commonly determined by extrapolating high-energy fusion data. From preliminary results, α and proton channels are clearly identified. In particular, ground and first excited states of 20 Ne and 23 Na play a major role.

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“…We adopted the following uncertainties in the quoted reactions: ±3% for the p+ 2 H reaction (Descouvemont et al 2004, for temperatures of about 10 6 K, typical of d-burning), ±5% for the 2 H+ 2 H channels (Tumino et al 2014), and ±10% for the 7 Li+p reaction (Lamia et al 2012). Notwithstanding the crucial role played by deuterium burning during the early pre-MS evolution, due to the slight variation of the reaction rates within the current uncertainties, the effect on the LDB age is completely negligible.…”

Section: Quantitymentioning

confidence: 99%

Cumulative theoretical uncertainties in lithium depletion boundary age

2016

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We performed a detailed analysis of the main theoretical uncertainties affecting the age at the lithium depletion boundary (LDB). To do that we computed almost 12 000 premain sequence models with mass in the range [0.06, 0.4] M ⊙ by varying input physics (nuclear reaction cross-sections, plasma electron screening, outer boundary conditions, equation of state, and radiative opacity), initial chemical elements abundances (total metallicity, helium and deuterium abundances, and heavy elements mixture), and convection efficiency (mixing length parameter, α ML ). As a first step, we studied the effect of varying these quantities individually within their extreme values. Then, we analysed the impact of simultaneously perturbing the main input/parameters without an a priori assumption of independence. Such an approach allowed us to build for the first time the cumulative error stripe, which defines the edges of the maximum uncertainty region in the theoretical LDB age.We found that the cumulative error stripe is asymmetric and dependent on the adopted mixing length value. For α ML = 1.00, the positive relative age error ranges from 5 to 15%, while for solar-calibrated mixing length, the uncertainty reduces to 5 − 10%. A large fraction of such an error (≈ 40%) is due to the uncertainty in the adopted initial chemical elements abundances.

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NEW DETERMINATION OF THE²H(d,p)³H AND²H(d,n)³He REACTION RATES AT ASTROPHYSICAL ENERGIES

Cited by 85 publications

References 35 publications

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

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

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method

Cumulative theoretical uncertainties in lithium depletion boundary age

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NEW DETERMINATION OF THE2H(d,p)3H AND2H(d,n)3He REACTION RATES AT ASTROPHYSICAL ENERGIES

Cited by 85 publications

References 35 publications

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

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

The12C(12C,α)20Ne and12C(12C,p)23Na reactions at the Gamow peak via the Trojan Horse Method

Cumulative theoretical uncertainties in lithium depletion boundary age

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NEW DETERMINATION OF THE²H(d,p)³H AND²H(d,n)³He REACTION RATES AT ASTROPHYSICAL ENERGIES

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

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

The¹²C(¹²C,α)²⁰Ne and¹²C(¹²C,p)²³Na reactions at the Gamow peak via the Trojan Horse Method