Dark QED from inflation
Abstract One contribution to any dark sector’s abundance comes from its gravitational production during inflation. If the dark sector is weakly coupled to the inflaton and the Standard Model, this can be its only production mechanism. For non-interacting dark sectors, such as a free massive fermion...
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2021
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oai:doaj.org-article:880b357fc5fc4b33953145da19ca3ce52021-11-21T12:41:32ZDark QED from inflation10.1007/JHEP11(2021)1061029-8479https://doaj.org/article/880b357fc5fc4b33953145da19ca3ce52021-11-01T00:00:00Zhttps://doi.org/10.1007/JHEP11(2021)106https://doaj.org/toc/1029-8479Abstract One contribution to any dark sector’s abundance comes from its gravitational production during inflation. If the dark sector is weakly coupled to the inflaton and the Standard Model, this can be its only production mechanism. For non-interacting dark sectors, such as a free massive fermion or a free massive vector field, this mechanism has been studied extensively. In this paper we show, via the example of dark massive QED, that the presence of interactions can result in a vastly different mass for the dark matter (DM) particle, which may well coincide with the range probed by upcoming experiments. In the context of dark QED we study the evolution of the energy density in the dark sector after inflation. Inflation produces a cold vector condensate consisting of an enormous number of bosons, which via interesting processes — Schwinger pair production, strong field electromagnetic cascades, and plasma dynamics — transfers its energy to a small number of “dark electrons” and triggers thermalization of the dark sector. The resulting dark electron DM mass range is from 50 MeV to 30 TeV, far different from both the 10 −5 eV mass of the massive photon dark matter in the absence of dark electrons, and from the 109 GeV dark electron mass in the absence of dark photons. This can significantly impact the search strategies for dark QED and, more generally, theories with a self-interacting DM sector. In the presence of kinetic mixing, a dark electron in this mass range can be searched for with upcoming direct detection experiments, such as SENSEI-100g and OSCURA.Asimina ArvanitakiSavas DimopoulosMarios GalanisDavide RaccoOlivier SimonJedidiah O. ThompsonSpringerOpenarticleBeyond Standard ModelCosmology of Theories beyond the SMNonperturbative EffectsNuclear and particle physics. Atomic energy. RadioactivityQC770-798ENJournal of High Energy Physics, Vol 2021, Iss 11, Pp 1-86 (2021) |
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DOAJ |
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DOAJ |
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EN |
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Beyond Standard Model Cosmology of Theories beyond the SM Nonperturbative Effects Nuclear and particle physics. Atomic energy. Radioactivity QC770-798 |
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Beyond Standard Model Cosmology of Theories beyond the SM Nonperturbative Effects Nuclear and particle physics. Atomic energy. Radioactivity QC770-798 Asimina Arvanitaki Savas Dimopoulos Marios Galanis Davide Racco Olivier Simon Jedidiah O. Thompson Dark QED from inflation |
| description |
Abstract One contribution to any dark sector’s abundance comes from its gravitational production during inflation. If the dark sector is weakly coupled to the inflaton and the Standard Model, this can be its only production mechanism. For non-interacting dark sectors, such as a free massive fermion or a free massive vector field, this mechanism has been studied extensively. In this paper we show, via the example of dark massive QED, that the presence of interactions can result in a vastly different mass for the dark matter (DM) particle, which may well coincide with the range probed by upcoming experiments. In the context of dark QED we study the evolution of the energy density in the dark sector after inflation. Inflation produces a cold vector condensate consisting of an enormous number of bosons, which via interesting processes — Schwinger pair production, strong field electromagnetic cascades, and plasma dynamics — transfers its energy to a small number of “dark electrons” and triggers thermalization of the dark sector. The resulting dark electron DM mass range is from 50 MeV to 30 TeV, far different from both the 10 −5 eV mass of the massive photon dark matter in the absence of dark electrons, and from the 109 GeV dark electron mass in the absence of dark photons. This can significantly impact the search strategies for dark QED and, more generally, theories with a self-interacting DM sector. In the presence of kinetic mixing, a dark electron in this mass range can be searched for with upcoming direct detection experiments, such as SENSEI-100g and OSCURA. |
| format |
article |
| author |
Asimina Arvanitaki Savas Dimopoulos Marios Galanis Davide Racco Olivier Simon Jedidiah O. Thompson |
| author_facet |
Asimina Arvanitaki Savas Dimopoulos Marios Galanis Davide Racco Olivier Simon Jedidiah O. Thompson |
| author_sort |
Asimina Arvanitaki |
| title |
Dark QED from inflation |
| title_short |
Dark QED from inflation |
| title_full |
Dark QED from inflation |
| title_fullStr |
Dark QED from inflation |
| title_full_unstemmed |
Dark QED from inflation |
| title_sort |
dark qed from inflation |
| publisher |
SpringerOpen |
| publishDate |
2021 |
| url |
https://doaj.org/article/880b357fc5fc4b33953145da19ca3ce5 |
| work_keys_str_mv |
AT asiminaarvanitaki darkqedfrominflation AT savasdimopoulos darkqedfrominflation AT mariosgalanis darkqedfrominflation AT davideracco darkqedfrominflation AT oliviersimon darkqedfrominflation AT jedidiahothompson darkqedfrominflation |
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