Examining Temporal Variation of the Fermi Coupling Constant using SNe Ia Light Curves

TL;DR

This study investigates the potential temporal variation of the Fermi coupling constant using Type Ia supernovae light curves across different redshifts, employing non-parametric methods to derive constraints independent of cosmological models.

Contribution

It introduces a novel approach to constrain $G_F$ variation by analyzing supernova light curves and applying Gaussian Process regression to avoid cosmological assumptions.

Findings

Suggests a small but finite variation of $G_F$ over time.

Sets a strong upper bound on the current fractional change of $G_F$.

Analyzes 1169 supernovae across redshifts 0 to 0.75.

Abstract

In standard model, the Fermi coupling constant, $G_F$, sets the strength of electroweak decay. We attempt an approach to constrain the temporal variation of the Fermi coupling constant $G_F$. To probe it, Type Ia supernovae (SNe Ia) light curves are being used as a source of reliable primordial nucleosynthesis events across the redshifts. We utilized studies suggesting that in the initial phase after the SNe Ia explosion, the electroweak decay of $^{56}Ni \rightarrow ^{56}Co \rightarrow ^{56}Fe$ is the key contributor to powering the SNe Ia light curve. We hence used the Pan-STARRS supernovae catalog having 1169 supernovae light curves in $g$, $r$, $i$, and $z$ spectral filters. The post-peak decrease in the apparent magnitude of light curves (in the rest frame of SNe) was related to the electroweak decay rate of primordial nucleosynthesis. Further, the decay rate relates to $G_F$. To keep the analysis independent of the cosmological model, we used the Hubble parameter measurement and a non-parametric statistical method, the Gaussian Process. Our study suggests a small yet finite temporal variation of $G_F$ and puts a strong upper bound on the present value of the fractional change in the Fermi coupling constant i.e; $\dfrac{\dot G_F}{G_F}\big\rvert_{z=0} \approx 10^{-11} yr^{-1}$ using datasets spread over a redshift range $0<z<0.75$.