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

Dirac, in 1937, proposed the potential variation of coupling constants derived from his large numbers hypothesis. Efforts have continued since then to constrain their variation by various methods, including astrophysical and cosmological observations. We briefly discuss several methods used for the purpose while focusing primarily on the use of supernovae type 1a, quasars, and gamma-ray bursts 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 SNeIa. Gamma-ray bursts (GRBs) are even brighter than quasars, and they have been observed up to z = 9.4. They are sources of highly transient radiation lasting from tens of milliseconds to several minutes and, in rare cases, a few hours. However, they are even more challenging to calibrate as standard candles than quasars. Both quasars and GRBs use SNeIa for distance calibration. What if the standard candles' intrinsic luminosities are affected when the coupling constants become dynamic and depend on measured distances? Assuming it to be constant at all cosmic distances leads to the wrong constraint on the data-fitted model parameters. 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 vary in such a . . way that their variation is interrelated as G similar to c(3) similar to h(3) similar to k(3/2) with G/G = 3(.)c/c = 3.h/h = 1.5 k/k = 3.90(+/- 0.04) x 10(-10) yr(-1 )and corroborates it with SNeIa, quasars, and GRBs observational data. Additionally, we show that this covarying coupling constant model may be better than the standard lambda CDM model for using quasars and GRBs as standard candles and predict that the mass of the GRBs scales with z as (1 + z)(1/3 )- 1 . Noether's symmetry on the coupling constants is now transferred effectively to the constant in the function relating to their variation.