Supernova bounds on axionlike particles coupled with nucleons and electrons
We investigate the potential of type II supernovae (SNe) to constrain axionlike particles (ALPs) coupled simultaneously to nucleons and electrons. ALPs coupled to nucleons can be efficiently produced in the SN core via nucleon-nucleon bremsstrahlung and, for a wide range of parameters, leave the SN...
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| Main Authors: | , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
16 August 2021
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| In: |
Physical review
Year: 2021, Volume: 104, Issue: 4, Pages: 1-13 |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.104.043016 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1103/PhysRevD.104.043016 Verlag, lizenzpflichtig, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.104.043016 
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| Author Notes: | Francesca Calore, Pierluca Carenza, Maurizio Giannotti, Joerg Jaeckel, Giuseppe Lucente, and Alessandro Mirizzi |
| Summary: | We investigate the potential of type II supernovae (SNe) to constrain axionlike particles (ALPs) coupled simultaneously to nucleons and electrons. ALPs coupled to nucleons can be efficiently produced in the SN core via nucleon-nucleon bremsstrahlung and, for a wide range of parameters, leave the SN unhindered, producing a large ALP flux. For masses exceeding 1 MeV, these ALPs would decay into electron-positron pairs, generating a positron flux. In the case of Galactic SNe, the annihilation of the created positrons with the electrons present in the Galaxy would contribute to the 511 keV annihilation line. Using the spectrometer on integral observation of this line allows us to exclude a wide range of the axion-electron coupling, 10−19≲gae≲10−11, for gap∼10−9. Additionally, ALPs from extra-galactic SNe decaying into electron-positron pairs would yield a contribution to the cosmic x-ray background. In this case, we constrain the ALP-electron coupling down to gae∼10−20. |
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| Item Description: | Gesehen am 22.10.2021 |
| Physical Description: | Online Resource |
| ISSN: | 2470-0029 |
| DOI: | 10.1103/PhysRevD.104.043016 |