Validation of the neutron monitor yield function using data from AMS-02 experiment, 2011--2017

TL;DR

This study calibrates ground-based neutron monitors using AMS-02 space data from 2011 to 2017, verifying yield functions and recommending the Mi13 model for accurate cosmic-ray analysis.

Contribution

It validates and compares several neutron monitor yield functions using space-based spectra, recommending the Mi13 model for improved cosmic-ray and solar event analysis.

Findings

Mi13 yield function accurately models NM response to galactic cosmic rays.

Ma16 and CD00 overestimate sensitivity to low-rigidity cosmic rays.

Force-field approximation fits proton spectra within a few percent during low to moderate activity.

Abstract

The newly published spectra of protons and helium over time directly measured in space by the AMS-02 experiment for the period 2011--2017 provide a unique opportunity to calibrate ground-based neutron monitors (NMs). Here, calibration of several stable sealevel NMs (Inuvik, Apatity, Oulu, Newark, Moscow, Hermanus, Athens) was performed using these spectra. Four modern NM yield functions were verified: Mi13 (Mishev et al., 2013), Ma16 (Mangeard et al., 2016), CM12 (Caballero-Lopez & Moraal, 2012) and CD00 (Clem & Dorman, 2000), on the basis of the cosmic-ray spectra measured by AMS-02. The Mi13 yield function was found to realistically represent the NM response to galactic cosmic rays. CM12 yield function leads to a small skew in the solar cycle dependence of the scaling factor. In contrast, Ma16 and CD00 yield functions tend to overestimate the NM sensitivity to low-rigidity (<10 GV) cosmic rays. This effect may be important for an analysis of ground level enhancements, leading to a potential underestimate of fluxes of solar energetic particles as based on NM data. The Mi13 yield function is recommended for quantitative analyses of NM data, especially for ground-level enhancements. The validity the force-field approximation was studied, and it was found that it fits well the directly measured proton spectra, within a few % for periods of low to moderate activity and up to ~10% for active periods. The results of this work strengthen and validate the method of the cosmic-ray variability analysis based on the NM data and yield-function formalism, and improves its accuracy.