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SN1987A constraints to BSM models with extra neutral bosons near the trapping regime: $U(1)_{L_μ-L_τ}$ model as an illustrative example (2401.16023v2)

Published 29 Jan 2024 in hep-ph

Abstract: New physics beyond the Standard Model (BSM) with an extra neutral boson can be constrained from the observation of SN1987A, since the production of this neutral boson in a supernova (SN) could accelerate the SN cooling and potentially lead to a period of the neutrino burst incompatible with the observation. The constraint to the model is formulated by the condition $L_{\rm NB}\leq 3\times 10{52}$ erg/s according to G. Raffelt with $L_{\rm NB}$ the luminosity of BSM neutral boson. Computing the above luminosity in the large coupling case, the so-called trapping regime, is non-trivial since the luminosity is a competition between the large production rate and the efficient absorption or decay rate of the neutral boson. We illustrate such a subtlety using $U(1){L\mu-L_\tau}$ model as an example where the $Z{\prime}$ luminosity, $L_{Z{\prime}}$, from the neutrinosphere is calculated. We calculate $Z'$ production, absorption, and decay rates through pair-coalescence, semi-Compton, loop-bremsstrahlung from proton-neutron scattering, and their inverse processes in a benchmark SN simulation with muons. We point out that, as the coupling constant $g_{Z'}$ increases, $L_{Z{\prime}}$ shall be approaching a constant plateau value for a given $m_{Z'}$ instead of monotonically decreasing down to zero as obtained in the previous literature. We demonstrate that this plateau phenomenon can be understood by physical arguments and justified by numerical calculations. With a different result on $L_{Z{\prime}}$ from the previous one, we discuss impacts on the constraints to $U(1){L\mu-L_\tau}$ parameter space by SN1987A. The implication of our result to the similar constraint on a generic BSM model with an extra neutral boson is also discussed.

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  35. There is a caveat worth mentioning as αZ′subscript𝛼superscript𝑍′\alpha_{Z^{\prime}}italic_α start_POSTSUBSCRIPT italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT end_POSTSUBSCRIPT approaches or even surpasses α𝛼\alphaitalic_α. In such a case, the interaction rate for Z′⁢μ−→Z′⁢μ−→superscript𝑍′superscript𝜇superscript𝑍′superscript𝜇Z^{\prime}\mu^{-}\to Z^{\prime}\mu^{-}italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT italic_μ start_POSTSUPERSCRIPT - end_POSTSUPERSCRIPT → italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT italic_μ start_POSTSUPERSCRIPT - end_POSTSUPERSCRIPT is comparable or even faster than that of Z′⁢μ−→γ⁢μ−→superscript𝑍′superscript𝜇𝛾superscript𝜇Z^{\prime}\mu^{-}\to\gamma\mu^{-}italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT italic_μ start_POSTSUPERSCRIPT - end_POSTSUPERSCRIPT → italic_γ italic_μ start_POSTSUPERSCRIPT - end_POSTSUPERSCRIPT. Hence the former process should be considered for the propagation of Z′superscript𝑍′Z^{\prime}italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT in addition to those reabsorption processes considered in Fig. 3. Consequently the Z′superscript𝑍′Z^{\prime}italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT trajectory inside the neutrinosphere is no longer a straight line. We shall not consider such a scenario in this work. Thus one should disregard constrained regions with gZ′>0.1subscript𝑔superscript𝑍′0.1g_{Z^{\prime}}>0.1italic_g start_POSTSUBSCRIPT italic_Z start_POSTSUPERSCRIPT ′ end_POSTSUPERSCRIPT end_POSTSUBSCRIPT > 0.1.
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