Constraining Coupling Constants' Variation with Supernovae, Quasars, and GRBs

Abstract

Dirac, in 1937 proposed the variation of coupling constants derived from his large number hypothesis. Efforts have continued since then to constrain their variation by various methods. We briefly discuss several methods used for the purpose while focusing primarily on the use of supernovae type 1a, quasars, and gamma-ray bursts (GRBs) as cosmological probes for determining cosmological distances. Supernovae type Ia (SNeIa) are considered the best standard candles since their intrinsic luminosity can be determined precisely from their light curves. However, they have only been observed up to about redshift $z=2.3$, mostly at $z<1.5$. Quasars are the brightest non-transient cosmic sources in the Universe. They have been observed up to $z=7.5$. Certain types of quasars can be calibrated well enough for their use as standard candles but with a higher degree of uncertainty in their intrinsic luminosity than the SNeIa. GRBs are even brighter than quasars, observed up to $z=9.4$. Their radiation lasts from 10s of milliseconds to several minutes and, in rare cases, for a few hours. However, they are even more challenging to calibrate as standard candles than quasars. What if the standard candles' intrinsic luminosities are affected when the coupling constants become dynamic? This paper uses our earlier finding that the speed of light c, the gravitational constant G, the Planck constant h, and the Boltzmann constant k variations are correlated as $G\sim c^3\sim h^3\sim k^{3/2}$ with $(\dot{G}/G{)}_0=3(\dot{c}/c{)}_0=(\dot{h}/h{)}_0=1.5(\dot{k}/k{)}_0=5.4H_0=3.90(\pm 0.04)\times 10^{-10}y{r}^{-1}$ corroborates it with SNeIa, quasars, and GRBs observational data. Also, we show that this covarying coupling constant model may be better than the standard ΛCDM model for using quasars and GRBs as standard candles and predict the mass of the GRBs scales as $((1+z{)}^{1/3}-1)$.

arXiv comment18 pages, 5 figures. arXiv admin note: text overlap with arXiv:2202.12758

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