Modelling Cosmic Rays Flux with Pierre Auger and Telescope Array Data in $\boldsymbol{f(R)}$ and $\boldsymbol{f(Q)}$ Theories of Gravity

TL;DR

This paper models cosmic ray flux using $f(R)$ and $f(Q)$ theories of gravity, analyzing how magnetic fields and redshift affect cosmic ray propagation and fitting the models to observational data from Pierre Auger and Telescope Array.

Contribution

It introduces a comparative analysis of $f(R)$ and $f(Q)$ gravity models for cosmic ray propagation, highlighting the $f(Q)$ model's superior fit to observational data.

Findings

$f(Q)$ model shows highest CR density enhancement.

$f(Q)$ model has lowest chi-squared when fitted to data.

Magnetic field and redshift significantly influence CR flux in these models.

Abstract

We investigate the effects of the magnetic field and the redshift on the propagation of galactic and extragalactic cosmic rays (CRs) in a modified theory of gravity (MTG) and an alternative theory of gravity (ATG) framework. For this purpose, we consider the $f(R)$ gravity and the $f(Q)$ gravity theories. We utilise these two MTG and ATG to compute the density enhancement factor of CRs as a function of the magnetic field and the redshift. For this work, we take the magnetic field strength from $1-100$ nG, while $0-2.5$ for the redshift. For each of these parameters, we take $100$ bins within their considered range for the computation. The enhancement parameter for the mixed composition of heavy nuclei up to Fe is also taken into account for this work. Further, we compute the $E^3$ magnified diffusive flux for $150$ sources separated by a distance $d_\text{s}$ for the different cosmological models. For the fitting with observational data from the Pierre Auger Observatory (PAO) and Telescope Array (TA), we parameterized some set that consists of the redshift $z$, the separation distances $d_\text{s}$ between the $150$ sources, and the maximum cutoff energy $E_{\text{max}}$. For each case, a residue plot and $\chi^2$ value are also added to check the goodness of fitting. A comparative analysis of considered models has been performed in each of the cases along with the $\Lambda$CDM model. The considered MTG and ATG models produce notable and fascinating outcomes, with the $f(Q)$ model showing the highest CR density enhancement and the lowest reduced chi-squared value when fitted to PAO and TA data of UHECRs flux. This research provides new perspectives on the connections between high-energy physics, astrophysics, and cosmology.