Mass Composition Studies of the Highest Energy Cosmic Rays

TL;DR

This paper discusses methods and findings related to determining the mass composition of the highest energy cosmic rays using atmospheric detection techniques, highlighting recent results from the Pierre Auger Observatory.

Contribution

It presents detailed analysis of the Pierre Auger elongation rate studies and explores combined surface and fluorescence detector data for mass composition insights.

Findings

Composition becomes lighter up to 2×10^{18} eV

Composition appears to become heavier above 2×10^{18} eV

Results depend heavily on high energy hadron interaction models

Abstract

The determination of the mass composition of the highest energy cosmic rays is one of the greatest challenges in cosmic ray experiments. The highest energy cosmic rays are only detected indirectly because of their very low flux. Using the atmosphere as a large target, Air Fluorescence Detectors are capable of tracing the evolution of the size of the Extensive Air Shower through the atmosphere (the shower longitudinal profile). The analysis of the characteristics of the detected longitudinal profiles is currently the most reliable way for extracting some information about the primary cosmic ray mass composition. In this proceeding, I will describe in some detail the Pierre Auger elongation rate studies, and I will show the potential for mass composition studies using the surface and the fluorescence detectors information as part of a single analysis. The interpretation of the current data with regard to mass composition, relies heavily on high energy hadron interaction models. Using standard hadron interaction models, the data suggest that the composition becomes lighter up to about 2 $\times$ 10$^{18}$ $eV$ and above that it becomes heavier again. This apparent change in the mass composition at 2 $\times$ 10$^{18}$ $eV$ seems to be correlated with a spectrum index change in the observed energy spectrum.