Big Bang Nucleosynthesis Elements

Big Bang Nucleosynthesis Elements-40
After freeze-out, the neutrons were free to β-decay, so the neutron fraction dropped to n/p ≃ 1/7 by the time nuclear reactions began. formation about the nucleosynthesis processes operating at the earliest times in the evolution of our Galaxy. proto-neutron star and the shock front expanding through the outer layers, is subject to a large neu-. Moreover, the sensitivity to the Hubble expansion rate affords a probe of, e.g., the number of relativistic neutrino species [9].

After freeze-out, the neutrons were free to β-decay, so the neutron fraction dropped to n/p ≃ 1/7 by the time nuclear reactions began.

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With nγ fixed by the present CMB temperature 2.7255 K (see ‘Cosmic Microwave Background’ review), this can be stated as the allowed range for the baryon mass density today, ρb = (3.9–4.6) × 10−31 g cm−3 , or as the baryonic fraction of the critical density, Ωb = ρb /ρcrit ≃ η10 h−2 /274 = (0.021–0.025)h−2 , where h ≡ H0 /100 km s−1 Mpc−1 is the present Hubble parameter (see Cosmological Parameters review). Big-Bang nucleosynthesis production of deuterium (and other complex nuclei) until well after T drops below the binding energy of deuterium, ∆D = 2.23 Me V.

As we shall see, all the light-element abundances can be explained with η10 ≡ η × 1010 in the range 5.7–6.7 (95% CL). C38, 090001 (2014) available on the PDG WWW pages (URL: December 4, 2014 2 1.

This motivates corresponding improvement in BBN precision and thus in the key reaction cross sections. The narrow vertical band indicates the CMB measure of the cosmic baryon density, while the wider band indicates the BBN concordance range (both at 95% CL). For all of the light elements, systematic errors are the dominant limitation to the precision with which primordial abundances can be inferred.

For example, it has been suggested [30] that d(p, γ)3He measurements may suffer from systematic errors and be inferior to ab initio theory; if so, this could alter D/H abundances at a level that is now significant. BBN is the only significant source of deuterium, which is entirely destroyed when it is cycled into stars [31].

1.16E-06 3.31E-08 2.84E-04 2.69E-04 1.82E-04 9.06E-05 9.03E-05. The rates of these reactions depend on the density of baryons (strictly speaking, nucleons), which is usually expressed normalized to the relic blackbody photon density as η ≡ nb /nγ .

A simplified analytic model of freeze-out yields the n/p ratio to an accuracy of ∼ 1% [10,11]. Nearly all neutrons end up bound in the most stable light element 4 He. Heavier nuclei do not form in any significant quantity both because of the absence of stable nuclei with mass number 5 or 8 (which impedes nucleosynthesis via n4 He, p4 He or 4 He4 He reactions), and the large Coulomb barriers for reactions such as 3 He(4 He, γ)7Li and 3 He(4 He, γ)7 Be. Predictions of the abundances of the light elements, D, 3 He, 4 He, and 7 Li, synthesized at the end of the ‘first three minutes’, are in good overall agreement with the primordial abundances inferred from observational data, thus validating the standard hot Big-Bang cosmology (see [2–4] for reviews). Big-Bang nucleosynthesis (BBN) offers the deepest reliable probe of the early Universe, being based on well-understood Standard Model physics [1]. The available D measurements are performed in systems with metallicities from 0.1 to 0.001 Solar where no significant astration is expected [34]. In the best-measured systems, D/H shows no Rhint of correlation with metallicity, redshift or the hydrogen column density N (H) (= los n H ds) integrated over the line-of-sight through the absorber. Make your own flashcards that can be shared with others.Learn with extra-efficient algorithm, developed by our team, to save your time.1 Department of Astronomy, University of Tokyo, Tokyo 113-0033, Japan. However, photo-dissociation by the high number density of photons delays CITATION: K. Only 2-body reactions, such as D(p, γ)3 He, 3 He(D, p)4 He, are important because the density by this time has become rather low – comparable to that of air! The nucleosynthesis chain begins with the formation of deuterium in the process p(n, γ)D. The quantity η −1 e−∆D /T , i.e., the number of photons per baryon above the deuterium photo-dissociation threshold, falls below unity at T ≃ 0.1 Me V; nuclei can then begin to form without being immediately photo-dissociated again.


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