Solar axion fluxes from 57Fe and 83Kr nuclear transitions differ by three orders of magnitude, yielding stronger constraints on |g_aN^eff × g_aγγ| and g_aγγ vs. m_a from Chandrayaan-2 XSM data for iron.
A Search For Solar Hadronic Axions Using Kr-83
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abstract
We introduce a new experimental method for solar hadronic axions search. It is suggested that these axions are created in the Sun during M1 transition between the first thermally excited level at 9.4 keV and the ground state in $^{83}Kr$. Our method is based on axion detection via resonant absorption process by the same nucleus in the laboratory. We use proportional gas counter filled with krypton to detect signals for axions. With this setup, target and detector are the same which increases the efficiency of the experiment. At present, an upper limit on hadronic axion mass of 5.5 keV at the 95% confidence level is obtained.
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Solar Axions from Nuclear Transitions
Solar axion fluxes from 57Fe and 83Kr nuclear transitions differ by three orders of magnitude, yielding stronger constraints on |g_aN^eff × g_aγγ| and g_aγγ vs. m_a from Chandrayaan-2 XSM data for iron.