Lithium Synthesis in Microquasar Accretion

Iocco, Fabio; Pato, Miguel

doi:10.1103/physrevlett.109.021102

Cited by 8 publications

(3 citation statements)

References 24 publications

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“…Lastly, the observational status and interpretation of the ''Spite plateau'' of lithium abundances in Population III stars is still uncertain (see, e.g., Refs. [83,90,91] and references therein).…”

Section: Discussionmentioning

confidence: 99%

Varying the light quark mass: Impact on the nuclear force and big bang nucleosynthesis

et al. 2013

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The quark mass dependences of light-element binding energies and nuclear scattering lengths are derived using chiral perturbation theory in combination with nonperturbative methods. In particular, we present new, improved values for the quark mass dependence of meson resonances that enter the nuclear force. A detailed analysis of the theoretical uncertainties arising in this determination is presented. As an application, we derive from a comparison of observed and calculated primordial deuterium and helium abundances a stringent limit on the variation of the light quark mass, m q =m q ¼ 0:02 AE 0:04. Inclusion of the neutron lifetime modification, under the assumption of a variation of the Higgs vacuum expectation value that translates into changing quark, electron, and weak gauge boson masses, leads to a stronger limit, jm q =m q j < 0:009.

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Section: Discussionmentioning

confidence: 99%

Varying the light quark mass: Impact on the nuclear force and big bang nucleosynthesis

et al. 2013

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“…Standard BBN results in 6 Li/ 7 Li = (2 ± 3) • 10 −5 [2], much below the detected levels. As a possible solution, it has been suggested that both stable lithium isotopes may be created in the hot tori formed around stellar black holes, but this interesting possibility actually worsens the 7 Li puzzle while solving the 6 Li one [70]. More exotic possible solutions include catalysis by long-living particles not included in the standard model [22,23] and non-equilibrium BBN [24].…”

Section: H(α γ) 6 LImentioning

confidence: 99%

Primordial nucleosynthesis

et al. 2016

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Big Bang nucleosynthesis (BBN) describes the production of light nuclei in the early phases of the Universe. For this, precise knowledge of the cosmological parameters, such as the baryon density, as well as the cross section of the fusion reactions involved are needed. In general, the energies of interest for BBN are so low (E < 1 MeV) that nuclear cross section measurements are practically unfeasible at the Earth's surface. As of today, LUNA (Laboratory for Underground Nuclear Astrophysics) has been the only facility in the world available to perform direct measurements of small cross section in a very low background radiation. Owing to the background suppression provided by about 1400 meters of rock at the Laboratori Nazionali del Gran Sasso (LNGS), Italy, and to the high current offered by the LUNA accelerator, it has been possible to investigate cross sections at energies of interest for Big Bang nucleosynthesis using protons, 3 He and alpha particles as projectiles. The main reaction studied in the past at LUNA is the 2 H(4 He, γ) 6 Li. Its cross section was measured directly, for the first time, in the BBN energy range. Other processes like 2 H(p, γ) 3 He, 3 He(2 H, p) 4 He and 3 He(4 He, γ) 7 Be were also studied at LUNA, thus enabling to reduce the uncertainty on the overall reaction rate and consequently on the determination of primordial abundances. The improvements on BBN due to the LUNA experimental data will be discussed and a perspective of future measurements will be outlined.

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“…There has been many attempts to solve this problem by testing all kinds of modifications of the parameters of the BBN or the physics it (a sample of this literature is found in Refs. [8,31,71,[79][80][81][82][83][84] and references therein). In the present case, the use of a non-Maxwellian velocity distribution seems to worsen this scenario.…”

Section: A Elemental Abundancesmentioning

confidence: 99%

Big Bang Nucleosynthesis With a Non-Maxwellian Distribution

Bertulani

Fuqua

Hussein

2013

ApJ

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The abundances of light elements based on the big bang nucleosynthesis model are calculated using the Tsallis non-extensive statistics. The impact of the variation of the non-extensive parameter q from the unity value is compared to observations and to the abundance yields from the standard big bang model. We find large differences between the reaction rates and the abundance of light elements calculated with the extensive and the non-extensive statistics. We found that the observations are consistent with a non-extensive parameter q = 1 +0.05 −0.12 , indicating that a large deviation from the Boltzmann-Gibbs statistics (q = 1) is highly unlikely. arXiv:1205.4000v2 [nucl-th]

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Lithium Synthesis in Microquasar Accretion

Cited by 8 publications

References 24 publications

Varying the light quark mass: Impact on the nuclear force and big bang nucleosynthesis

Varying the light quark mass: Impact on the nuclear force and big bang nucleosynthesis

Primordial nucleosynthesis

Big Bang Nucleosynthesis With a Non-Maxwellian Distribution

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