Abstract
We present the supernova constraints on an axion-photon-dark photon coupling, which can be the leading coupling to dark sector models and can also lead to dramatic changes to axion cosmology. We show that the supernova bound on this coupling has two unusual features. One occurs because the scattering that leads to the trapping regime converts axions and dark photons into each other. Thus, if one of the two new particles is sufficiently massive, both production and scattering become suppressed and the bounds from bulk emission and trapped (area) emission both weaken exponentially and do not intersection The other unusual feature occurs because for light dark photons, longitudinal modes couple more weakly than transverse modes do. Since the longitudinal mode is more weakly coupled, it can still cause excessive cooling even if the transverse mode is trapped. Thus, the supernova constraints for massive dark photons look like two independent supernova bounds super-imposed on top of each other.
Highlights
Plane intersect at large masses, leading to a closed region that can be excluded by cooling considerations
We present the supernova constraints on an axion-photon-dark photon coupling, which can be the leading coupling to dark sector models and can lead to dramatic changes to axion cosmology
We study the supernovae cooling constraint on the axion-photon-darkphoton coupling, and show that this model leads to two new qualitative features in supernovae that can play a role in non-minimal scenarios where there are more than one new degree of freedom
Summary
The core collapse supernova SN1987A has provided, and continues to provide, valuable constraints on new physics. We must compute the emissivity for each process that can produce axions and dark photons in the supernova To find these emissivites, we take the interaction rate per unit volume for that process and weigh it by the energy carried away by the axion and dark photon in the final state [53],. Upon integration of each emissivity over the volume of the supernova, we find that the annihilation is the dominant process, with plasmon decay being a significant contribution for lower masses These emissivities are summed into a total emissivity and integrated over the volume of the supernova to give the total luminosity of axions and dark photons. This total luminosity is applied to the constraint in eq (2.1) for various axion and dark photon masses and is shown in the lower line in figure 5
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