%0 Journal Article
%T Invisible neutrino decay in precision cosmology
%A Barenboim, G.
%A Chen, J. Z.
%A Hannestad, S.
%A Oldengott, I. M.
%A Tram, T.
%A Wong, Y. Y. Y.
%J Journal of Cosmology and Astroparticle Physics
%D 2021
%V 03
%N 3
%I Iop Publishing Ltd
%@ 1475-7516
%G English
%F Barenboim_etal2021
%O WOS:000636717400082
%O exported from refbase (https://references.ific.uv.es/refbase/show.php?record=4782), last updated on Tue, 27 Apr 2021 18:21:11 +0000
%X We revisit the topic of invisible neutrino decay in the precision cosmological context, via a first-principles approach to understanding the cosmic microwave background and large-scale structure phenomenology of such a non-standard physics scenario. Assuming an effective Lagrangian in which a heavier standard-model neutrino nu(H) couples to a lighter one nu(l) and a massless scalar particle phi via a Yukawa interaction, we derive from first principles the complete set of Boltzmann equations, at both the spatially homogeneous and the firstorder inhomogeneous levels, for the phase space densities of nu(H), nu(l), and phi in the presence of the relevant decay and inverse decay processes. With this set of equations in hand, we perform a critical survey of recent works on cosmological invisible neutrino decay in both limits of decay while nu(H) is ultra-relativistic and non-relativistic. Our two main findings are: (i) in the non-relativistic limit, the effective equations of motion used to describe perturbations in the neutrino-scalar system in the existing literature formally violate momentum conservation and gauge invariance, and (ii) in the ultra-relativistic limit, exponential damping of the anisotropic stress does not occur at the commonly-used rate Gamma(T) = (1/tau(0))( m(nu H)/E-nu H)(3), but at a rate similar to (1/ tau(0))(m(nu H)/E-nu H)(5). Both results are model-independent. The impact of the former finding on the cosmology of invisible neutrino decay is likely small. The latter, however, implies a significant revision of the cosmological limit on the neutrino lifetime tau(0) from tau(old)(0) greater than or similar to 1.2 x 10(9) s (m(nu H)/50 meV)(3) to tau(0) greater than or similar to (4 x 10(5) -> 4 x 10(6)) s (m(nu H)/50 meV)(5).
%K cosmological neutrinos
%K neutrino properties
%K CMBR theory
%K cosmological parameters from CMBR
%R 10.1088/1475-7516/2021/03/087
%U https://arxiv.org/abs/2011.01502
%U https://doi.org/10.1088/1475-7516/2021/03/087
%P 087-53pp