The Status and Future of Direct Nuclear Reaction Measurements for Stellar Burning

Aliotta, M.; Buompane, R.; Couder, M.; Couture, A.; deBoer, R. J.; Formicola, A.; Gialanella, L.; Glorius, J.; Imbriani, G.; Junker, M.; Langer, C.; Lennarz, A.; Litvinov, Yu. A.; Liu, W. -P.; Lugaro, M.; Matei, C.; Meisel, Z.; Piersanti, L.; Reifarth, R.; Robertson, D.; Simon, A.; Straniero, O.; Tumino, A.; Wiescher, M.; Xu, Y.

doi:10.48550/arxiv.2109.14418

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References 240 publications

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“…Instead, the low energy cross-section is largely influenced by the 1 −1 (𝐸 𝑥 = 7.12 MeV) and 2 + (𝐸 𝑥 = 6.92 MeV) subthreshold states (see Figure 2 of Deboer et al 2017, for details). The primary influence of these two nearby subthreshold states and the addition of possible resonant transitions in the wings of the broad channel at 𝐸 𝑥 = 9.59 MeV makes the nuclear cross-section extremely difficult to estimate (see Fowler et al 1967;Kunz et al 2002;An et al 2016;Deboer et al 2017Deboer et al , 2019Aliotta et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The impact of the uncertainties in the 12C(α,γ)16O reaction rate on the evolution of low- to intermediate-mass stars

Pepper,

Istrate,

Romero

et al. 2022

Preprint

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One of the largest uncertainties in stellar evolutionary computations is the accuracy of the considered reaction rates. The 12 C(𝛼, 𝛾) 16 O reaction is particularly important for the study of low-and intermediate-mass stars as it determines the final C/O ratio in the core which influences the white dwarf cooling evolution. Thus, there is a need for a study of how the computations of white dwarfs and their progenitors that are made to date may be affected by the uncertainties of the 12 C(𝛼, 𝛾) 16 O reaction rates. In this work we compute fully evolutionary sequences using the MESA code with initial masses in the range of 0.90 ≤ 𝑀 𝑖 /𝑀 ≤ 3.05. We consider different adopted reaction rates, obtained from the literature, as well as the extreme limits within their uncertainties. As expected, we find that previous to the core helium burning stage, there are no changes to the evolution of the stars. However, the subsequent stages are all affected by the uncertainties of the considered reaction rate. In particular, we find differences to the convective core mass during the core helium burning stage which may affect pulsation properties of subdwarfs, the number of thermal pulses during the asymptotic giant branch and trends between final oxygen abundance in the core and the progenitor masses of the remnant white dwarfs.

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Section: Introductionmentioning

confidence: 99%