Rate of dark photon emission from electron positron annihilation in massive stars. (arXiv:1904.10567v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Rrapaj_E/0/1/0/all/0/1">Ermal Rrapaj</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sieverding_A/0/1/0/all/0/1">Andre Sieverding</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Qian_Y/0/1/0/all/0/1">Yong-Zhong Qian</a>
We calculate the rate of production of dark photons from electron-positron
pair annihilation in hot and dense matter characteristic of supernova
progenitors. Given the non-linear dependence of the emission rate on the dark
photon mass and current astrophysical constraints on the dark photon parameter
space, we focus on the mass range of 1–10 MeV. For the conditions under
consideration both mixing with the in-medium photon and plasma effects on the
electron dispersion relation are non-negligible and are explored in detail. We
perform our calculations to the leading order in the fine-structure constant.
Transverse and longitudinal photon modes are treated separately given their
different dispersion relations. We consider the implications for the evolution
of massive stars when dark photons decay either into particles of the standard
model or of the dark sector.
We calculate the rate of production of dark photons from electron-positron
pair annihilation in hot and dense matter characteristic of supernova
progenitors. Given the non-linear dependence of the emission rate on the dark
photon mass and current astrophysical constraints on the dark photon parameter
space, we focus on the mass range of 1–10 MeV. For the conditions under
consideration both mixing with the in-medium photon and plasma effects on the
electron dispersion relation are non-negligible and are explored in detail. We
perform our calculations to the leading order in the fine-structure constant.
Transverse and longitudinal photon modes are treated separately given their
different dispersion relations. We consider the implications for the evolution
of massive stars when dark photons decay either into particles of the standard
model or of the dark sector.
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