Entropy, neutrino physics, and the lithium problem: why are there stars with essentially no lithium due to serious lithium deficiency in certain spatial regions in the early universe?

The consequences of abnormally low lithium abundance in a nearby population II star (which is almost as old as the supposed population III stars) as represented by HE0107-5240 are that standard BBN theory is out of sync with observations. Analysis of the big bang nucleosynthesis may help explain the anomalously low value of lithium abundance in the star HE0107-5240, which by orthodox BBN, should not exist, as explained by Shigeyama et al. [1]. Introduction The dimensional identification of energy given by p, as well as variation in energy ∆E in a graviton, with p ∼ L · μ and ∆E ∼ L · μ, define how gravitons evolve in space time due to conditions which are related to the degree gravitons evolving in space time relate to the gravitational Lorenz violation. Note that L 6= 0 extends the standard model, as given by Jenkens [2], in which, if gravitons travel with a speed of v, L ∼ (v − c)/c. Bashinsky’s [3] analysis with neutrino-graviton interaction occurs as L 6= 0 becomes L→ 0. We are seeking to understand the regime where neutrino-graviton mixing may be taking place, allowing for stars like HE0107-5240. 1 Dispersion of neutrinos in early cosmology Marklund et al. [4] have estimated neutrino mass as mv = −gαβpp, where mv is neutrino mass, gαβ is for a metric, and p is four momentum. If space becomes abruptly flat at the onset of inflation, for a neutrino mass, as L 6= 0 approaches zero, gαβ approaches gαα (i.e. leading to flat space), then by Marklund et al. [4], there exits, assuming k is a four space wave number, the inequality ω F > (gαα/|g00|) · [k] + 2ωF (g00/|g00|)k. (1) It is suggested that neutrino-graviton interactions would allow a researcher to input values of k, k, gαα, and g00 when Eqn. (1) is true. Based on this, the neutrino has approximately 10 − 10 times the effective mass of a graviton.