Indirect measurement of the $$^3\hbox {He}$$(n,p)$$^3\hbox {H}$$ reaction cross section at Big Bang energies

Pizzone, R. G.; Spampinato, C.; Spartà, R.; Couder, M.; Tan, Wanpeng; Burjan, V.; D’Agata, G.; Guardo, G. L.; Cognata, M. La; Lamia, L.; Mrázek, J.; Palmerini, S.; Typel, S.; Туміно, А.; Wiescher, M.; Anguilar, S.; Bardayan, D. W.; Blankstein, D.; Boccioli, Luca; Callahan, Lauren; M., S.; Chae, K. Y.; Clark, Adam M.; Frentz, B.; Hall, M. R.; Gula, A.; Henderson, S. L.; Kelmar, R.; Kwag, M. S.; Indelicato, I.; Commara, M. La; Lattuada, D.; Liu, Q.; Long, J.; Mazzocco, M.; Majumdar, A. K. Dutta; McGuinness, Sean; Nelson, A.; Oliva, A.; O’Malley, P. D.; Prajapati, P. M.; Rapisarda, G. G.; Романо, С.; Sergi, M. L.; Seymour, C.; Skulski, Michael; Spitaleri, C.; Wilkinson, John

doi:10.1140/epja/s10050-020-00212-x

Cited by 22 publications

(4 citation statements)

References 53 publications

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“…Moreover in the last years THM was successfully applied to reactions induced by unstable beams [154,108] as well as neutron induced reactions which may play a role also in the context of light element nucleosynthesis and BBN. In particular the 3 He(n,p) 3 H was studied at the astrophysically relevant energies (see [155] and references therein). THM was also applied to reactions between heavier systems, which are relevant in the late stellar evolutionary stages (Tumino et al [211]).…”

Section: Effects Of Light Element Burning Cross Sections On Pre-main ...mentioning

confidence: 99%

Theoretical predictions of surface light element abundances in protostellar and pre-Main Sequence phase

Tognelli,

Degl'Innocenti,

Moroni

et al. 2021

Preprint

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Theoretical prediction of surface stellar abundances of light elements -lithium, beryllium, and boron -represents one of the most interesting open problems in astrophysics. As well known, several measurements of 7 Li abundances in stellar atmospheres point out a disagreement between predictions and observations in different stellar evolutionary phases, rising doubts about the capability of present stellar models to precisely reproduce stellar envelope characteristics. The problem takes different aspects in the various evolutionary phases; the present analysis is restricted to protostellar and pre-Main Sequence phases. Light elements are burned at relatively low temperatures (T from ≈ 2 to ≈ 5 million degrees) and thus in the early evolutionary stages of a star they are gradually destroyed at different depths of stellar interior mainly by (p, α) burning reactions, in dependence on the stellar mass. Their surface abundances are strongly influenced by the nuclear cross sections, as well as by the extension toward the stellar interior of the convective envelope and by the temperature at its bottom, which depend on the characteristics of the star (mass and chemical composition) as well as on the energy transport in the convective stellar envelope. In recent years, a great effort has been made to improve the precision of light element burning cross sections. However, theoretical predictions surface light element abundance are challenging because they are also influenced by the uncertainties in the input physics adopted in the calculations as well as the efficiency of several standard and non-standard physical processes active in young stars (i.e. diffusion, radiative levitation, magnetic fields, rotation). Moreover, it is still not completely clear how much the previous protostellar evolution affects the pre-Main Sequence characteristics and thus the 1 Tognelli et al.Light element abundances in protostellar and pre-main sequence phase. light element depletion. This paper presents the state-of-the-art of theoretical predictions for protostars and pre-Main Sequence stars and their light element surface abundances, discussing the role of (p, α) nuclear reaction rates and other input physics on the stellar evolution and on the temporal evolution of the predicted surface abundances.

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Section: Effects Of Light Element Burning Cross Sections On Pre-main ...mentioning

confidence: 99%

Theoretical predictions of surface light element abundances in protostellar and pre-Main Sequence phase

Tognelli,

Degl'Innocenti,

Moroni

et al. 2021

Preprint

Self Cite

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“…A measurement was recently performed by means of the THM with the same methodology reported for the other reactions. Data analysis is still in progress (Pizzone et al, 2020;Spampinato et al, 2020). A preliminary reaction rate, calculated upon FIGURE 8 | (Left) Trojan Horse 2 H(d,p) 3 H reaction rates as a ratio to the one obtained from direct data fit in the upper panel; the middle and lower panels show rates as a ratio to rates published in NACRE (Angulo et al, 1999;Cyburt, 2004).…”

Section: He(np) 3 Hmentioning

confidence: 99%

“…The figure is adapted from Pizzone et al (2014). the data shown in Pizzone et al (2020) is plotted in Figure 7 with a comparison with the reaction rate published by Brune et al (1999). In the energy region important for astrophysics a deviation up to 20% is present and will be investigated in future works.…”

Section: He(np) 3 Hmentioning

confidence: 99%

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Direct and Indirect Measurements for a Better Understanding of the Primordial Nucleosynthesis

Spartà

Pizzone

Bertulani

et al. 2020

Front. Astron. Space Sci.

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The Big Bang Nucleosynthesis (BBN) model is a great success of nuclear astrophysics due to the outstanding agreement between observational and predicted light elements abundances. One exception, however, is the so-called "lithium problem." In this context, experimental efforts to measure the relevant reactions have been brought to an increased level of accuracy in measuring primordial abundances, and the introduction of indirect methods has allowed researchers to overcome the natural limitations of direct measurements in the energy range of interest for BBN. Here we review the results obtained from the application of the Trojan Horse Method to some of the most influential reactions of the standard network, such as 2 H(d,p) 3 H, 2 H(d,n) 3 He, 3 He(d,p) 4 He, 7 Li(p,α) 4 He, and 7 Be(n,α) 4 He. The relevant cross sections have been then used as new inputs to a classical BBN code, resulting in important constraints that make suggestions for a possible solution for the lithium problem outside of nuclear physics.

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Indirect Methods in Nuclear Astrophysics with Transfer Reactions

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2022

Handbook of Nuclear Physics

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Indirect measurement of the $$^3\hbox {He}$$(n,p)$$^3\hbox {H}$$ reaction cross section at Big Bang energies

Cited by 22 publications

References 53 publications

Theoretical predictions of surface light element abundances in protostellar and pre-Main Sequence phase

Theoretical predictions of surface light element abundances in protostellar and pre-Main Sequence phase

Direct and Indirect Measurements for a Better Understanding of the Primordial Nucleosynthesis

Indirect Methods in Nuclear Astrophysics with Transfer Reactions

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