Big Bang nucleosynthesis | Wikipedia audio article
Channel: wikipedia tts
Date: 08/12/2018

This is an audio version of the Wikipedia Article:
Big Bang nucleosynthesis


00:01:19 1 Characteristics
00:03:24 2 Important parameters
00:03:46 2.1 Neutron–proton ratio
00:04:54 2.2 Baryon–photon ratio
00:05:49 3 Sequence
00:06:59 3.1 History of theory
00:08:53 3.2 Heavy elements
00:09:20 3.3 Helium-4
00:10:05 3.4 Deuterium
00:11:25 3.5 Lithium
00:13:38 4 Measurements and status of theory
00:16:35 5 Non-standard scenarios
00:16:55 6 See also
00:19:30 7 References
00:21:05 8 External links



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SUMMARY
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In physical cosmology, Big Bang nucleosynthesis (abbreviated BBN, also known as primordial nucleosynthesis, arch(a)eonucleosynthesis, archonucleosynthesis, protonucleosynthesis and pal(a)eonucleosynthesis) refers to the production of nuclei other than those of the lightest isotope of hydrogen (hydrogen-1, 1H, having a single proton as a nucleus) during the early phases of the Universe. Primordial nucleosynthesis is believed by most cosmologists to have taken place in the interval from roughly 10 seconds to 20 minutes after the Big Bang, and is calculated to be responsible for the formation of most of the universe's helium as the isotope helium-4 (4He), along with small amounts of the hydrogen isotope deuterium (2H or D), the helium isotope helium-3 (3He), and a very small amount of the lithium isotope lithium-7 (7Li). In addition to these stable nuclei, two unstable or radioactive isotopes were also produced: the heavy hydrogen isotope tritium (3H or T); and the beryllium isotope beryllium-7 (7Be); but these unstable isotopes later decayed into 3He and 7Li, as above.
Essentially all of the elements that are heavier than lithium were created much later, by stellar nucleosynthesis in evolving and exploding stars.