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PreprintarXiv licencearXiv

Neutron Star Bounds on Muonic Fifth Forces from Picometer to Meter Scales

  • Damiano F. G. Fiorillo
  • Alessandro Lella
  • Georg G. Raffelt
  • Nudzeim Selimovic
  • Edoardo Vitagliano
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Abstract

Testing muonic fifth forces is difficult because muons are scarce in ordinary matter. However, they are abundant in neutron stars. We show that this population responds coherently to electromagnetic fluctuations induced by proton and electron collisions, emitting the fifth-force mediator and cooling the star. This energy loss constrains gXμ≲ 10−13 for scalars with mϕ≲ 100 keV and vectors with 10−5 eV≲ mV≲ 100 keV, far more strongly than SN 1987A cooling. Vector forces at smaller mV deplete muons, suppressing the coherent response. Cooling from incoherent muon scattering still constrains gV μ≲ 2.5× 10−12 for 1.3× 10−7 eV≲ mV≲ 10−5 eV. Together, these bounds provide the most sensitive probes of muonic interactions across a broad range of parameters.

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Cite

BibTeXRIS
BibTeX
@misc{fiorillo2026neutron,
  title = {{Neutron Star Bounds on Muonic Fifth Forces from Picometer to Meter Scales}},
  author = {Damiano F. G. Fiorillo and Alessandro Lella and Georg G. Raffelt and Nudzeim Selimovic and Edoardo Vitagliano},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2605.24094},
  eprint = {2605.24094},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2605.24094},
}
RIS
TY  - UNPB
TI  - Neutron Star Bounds on Muonic Fifth Forces from Picometer to Meter Scales
AU  - Damiano F. G. Fiorillo
AU  - Alessandro Lella
AU  - Georg G. Raffelt
AU  - Nudzeim Selimovic
AU  - Edoardo Vitagliano
PY  - 2026
DA  - 2026/10/08
PB  - arXiv
DO  - 10.48550/arxiv.2605.24094
UR  - https://arxiv.org/abs/2605.24094
AB  - Testing muonic fifth forces is difficult because muons are scarce in ordinary matter. However, they are abundant in neutron stars. We show that this population responds coherently to electromagnetic fluctuations induced by proton and electron collisions, emitting the fifth-force mediator and cooling the star. This energy loss constrains g_Xμ≲ 10^−13 for scalars with m_ϕ≲ 100 keV and vectors with 10^−5 eV≲ m_V≲ 100 keV, far more strongly than SN 1987A cooling. Vector forces at smaller m_V deplete muons, suppressing the coherent response. Cooling from incoherent muon scattering still constrains g_V μ≲ 2.5× 10^−12 for 1.3× 10^−7 eV≲ m_V≲ 10^−5 eV. Together, these bounds provide the most sensitive probes of muonic interactions across a broad range of parameters.
ER  -