Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung

By Pierluca Carenza, Tobias Fischer, Maurizio Giannotti, G. Guo, G. Mart'inez-Pinedo, A. Mirizzi. Journal of Cosmology and Astroparticle Physics, 2019

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The most efficient axion production mechanism in a supernova (SN) core is the nucleon-nucleon bremsstrahlung. This process has been often modeled at the level of the vacuum one-pion exchange (OPE) approximation. Starting from this naive recipe, we revise the calculation including systematically different effects, namely a non-vanishing mass for the exchanged pion, the contribution from the two-pions exchange, effective in-medium nucleon masses and multiple nucleon scatterings. Moreover, we allow for an arbitrary degree of nucleon degeneracy. A self consistent treatment of the axion emission rate including all these effects is currently missing. The aim of this work is to provide such an analysis. Furthermore, we demonstrate that the OPE potential with all the previous corrections gives rise to similar results as the on-shell T-matrix, and is \pagebreak therefore well justified for our and similar studies. We find that the axion emissivity is reduced by over an order of magnitude with respect to the basic OPE calculation, after all these effects are accounted for. The implications for the axion mass bound and the impact for the next generation experimental axion searches is also discussed.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ccc11b216638c65b255a6416b5a75622b8cf5a5c

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Citations in the corpus

The landscape of QCD axion models (2020, methodology): “However, even trapped axions may extract more energy than neutrinos from the young SN and couplings all the way to gan = gap ≈ 10−4 should be probably excluded [396].”
More axions from strings (2020, background): “The limit on DFSZ models from white dwarfs and red giants (“WD/RG”) is indicated for tanβ = 1 [75] , while the supernova-1987a limit on such models (“SN1987a”) spans the blurred region as tanβ varies (the corresponding constraint on KSVZ models is ma < 15 meV) [70].”
The Dark Photon (2020, unknown): “This limit yields, taking the most conservative estimate in (Carenza et al., 2019; Keil et al., 1997), α′aN ≤ 1.3× 10−18 .”