Abstract
We propose a new possibility of using the coherently enhanced neutrino pair emission to probe light-mediator interactions between electron and neutrinos. With typical momentum transfer at the atomic mathcal O(1 eV) scale, this process is extremely sensitive for the mediator mass range mathcal O(10^{-3} sim 10^4) eV. The sensitivity on the product of couplings with electron (g^e or y^e) and neutrinos (g^nu or y^nu ) can touch down to |y^e y^nu | < 10^{-9} sim 10^{-19} for a scalar mediator and |g^e g^nu | < 10^{-15} sim 10^{-26} for a vector one, with orders of improvement from the existing constraints.
Highlights
The beyond the Standard Model (SM) (BSM) neutrino interactions can appear as non-standard interactions (NSI) [26,27] and effective neutrino masses [28,29]
In this work we present a new possibility of using the radiative emission of neutrino pair (RENP) [76–79] to probe the BSM interactions mediated by a light mediator
The various existing constraints on the coupling constant can no longer improve once the light mediator mass decreases to become comparable with momentum transfer
Summary
The BSM neutrino interactions can appear as non-standard interactions (NSI) [26,27] and effective neutrino masses [28,29]. The presence of new light particles have impact in the early Universe by generating extra degrees of freedom [44,45] or delaying the neutrino freezeout [46,47]. Despite these ways of probing neutrino interactions, most of them involve large momentum transfer and cannot probe light mediators much below O(1 MeV). The most stringent bound comes from cooling of astrophysical sources [49,50] which are model dependent [51] Most of these can only indirectly constrain the coupling with either electron or neutrino, not both of them. In this work we present a new possibility of using the radiative emission of neutrino pair (RENP) [76–79] to probe the BSM interactions mediated by a light mediator. We summarize the most prominent results and features in 5
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