Estimating the flux of the 14.4 keV solar axions

Abstract

this paper we present a calculation of the expected flux of the mono-energetic 14.4 keV solar axions emitted by the M1 type nuclear transition of Fe-57 in the Sun. These axions can be detected, e.g., by inverse coherent Bragg-Prirnakoff conversion in single-crystal Teo(2) bolonteters. The ingredients of this calculation are i) the axion nucleon coupling, estimated in several popular axion models and ii)the nuclear spin matrix elements involving realistic shell model calculations with both proton and neutron excitations. For the benefit of the experiments we have also calculated the branching ratio involving axion and photon emission. We, find the solar axion flux on Earth to be Phi(a) = 0.703 x 10(9) cm(-2)s(-1) (10(7) GeV/f(a))(2) and the branching; ratio of axion to photon for the same model to be: omega(a)/omega(gamma) = 0.229 x 10(-15) approximate to 2 x 10(-16). (c) 2018 IOP Publishing Ltd and Sissa Medialab