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As the universe expanded, it cooled. Free neutrons and protons are less stable than helium nuclei, and the protons and neutrons have a strong tendency to form helium-4 [via] the intermediate step of forming deuterium. At the time at which nucleosynthesis occured, the temperature was high enough for the mean energy per particle to be greater than the binding energy of deuterium; therefore any deuterium that was formed was immediately destroyed (a situation known as the deuterium bottleneck). Hence, the formation of helium-4 is delayed, until the universe becomes cool enough to form deuterium (at about T = 0.1 MeV [= 1 GK]), when there is a sudden burst of element formation. Shortly thereafter...the universe becomes too cool for any nuclear fusion to occur. At this point, the elemental abundances were fixed, and only change as some of the radioactive products of BBN (such as tritium) decayed...
Deuterium is in some ways the opposite of helium-4 in that while helium-4 is very stable and very difficult to destroy, deuterium is only marginally stable and easy to destroy. Because helium-4 is very stable, there is a strong tendency on the part of two deuterium nuclei to combine to form helium-4. The only reason BBN did not convert all of the deuterium in the universe to helium-4 is that the expansion of the universe cooled the universe, and cut this conversion short, before it could be completed. One consequence of this is that unlike helium-4, the amount of deuterium is very sensitive to initial conditions. The denser the universe is, the more deuterium gets converted to helium-4 before time runs out, and the less deuterium remains.
Deuterium is in some ways the opposite of helium-4 in that while helium-4 is very stable and very difficult to destroy, deuterium is only marginally stable and easy to destroy. Because helium-4 is very stable, there is a strong tendency on the part of two deuterium nuclei to combine to form helium-4. The only reason BBN did not convert all of the deuterium in the universe to helium-4 is that the expansion of the universe cooled the universe, and cut this conversion short, before it could be completed. One consequence of this is that unlike helium-4, the amount of deuterium is very sensitive to initial conditions. The denser the universe is, the more deuterium gets converted to helium-4 before time runs out, and the less deuterium remains.
According to direct observations of space, there are (relatively) high levels of surviving D; and (relatively) low levels of Li:

Thus, the following nuclear reactions occurred:

but not:

QUESTIONS:
Qualitatively, is the Lawson criterion applicable, i.e. the amount of fusion that occurred, when the primordial plasma was "singed" in BBN, was proportional, to the product, of baryon density during BBN, multiplied by the time of BBN, i.e.
? (I understand, that the temperature regime, is plausibly constrained, 300 MK < T < 1000 MK.)And so, if the baryon density was higher, then the time for fusion must have been lower ??
Could "inflation", or something similar, have "stretched out space", more swiftly than currently conceived, so that a hypothetically higher baryon density, e.g.
, would have had less time to "cook" ?

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MultiQuote
, that

; then, to be consistent with observations (of abundances) & calculations (of 
&
, i.e. comparing various scenarios, 

from the temperature data. If so, then "demanding" that the baryon density be ~20x higher, i.e. close to critical density, would "require":












