{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/muonic-boson-limits-supernova-redux","title":"Muonic Boson Limits: Supernova Redux","arxiv_id":"2109.03244","date":"2021-09-07","proceeding":null,"authors":["Andrea Caputo","Georg Raffelt","Edoardo Vitagliano"],"abstract":"We derive supernova (SN) bounds on muon-philic bosons, taking advantage of the recent emergence of muonic SN models. Our main innovations are to consider scalars $\\phi$ in addition to pseudoscalars $a$ and to include systematically the generic two-photon coupling $G_{\\gamma\\gamma}$ implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound $G_{\\gamma\\gamma}<0.67\\times10^{-10}~{\\rm GeV}^{-1}$ derived for axion-like particles carries over to the muonic Yukawa couplings as $g_a<3.1\\times10^{-9}$ and $g_\\phi< 4.6\\times10^{-9}$ for $m_{a,\\phi}\\lesssim 100$ keV, so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN1987A $\\gamma$ rays and the diffuse cosmic $\\gamma$-ray background. The latter allows at most $10^{-4}$ of a typical total SN energy of $E_{\\rm SN}\\simeq3\\times10^{53}$erg to show up as $\\gamma$ rays, for $m_{a,\\phi}\\gtrsim 100$keV implying $g_a \\lesssim 0.9\\times10^{-10}$ and $g_\\phi \\lesssim 0.4\\times10^{-10}$. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match $L_\\nu$ for $g_{a,\\phi}\\simeq 10^{-4}$. However, the $2\\gamma$ decay is so fast that all the energy is dumped into the surrounding progenitor-star matter, whereas at most $10^{-2}E_{\\rm SN}$ may show up in the explosion. To suppress boson emission below this level we need yet larger couplings, $g_{a}\\gtrsim 2\\times10^{-3}$ and $g_{\\phi}\\gtrsim 4\\times10^{-3}$. Muonic scalars can explain the muon magnetic-moment anomaly for $g_{\\phi}\\simeq 0.4\\times10^{-3}$, a value hard to reconcile with SN physics despite the uncertainty of the explosion-energy bound. For generic axion-like particles, this argument covers the \"cosmological triangle\" in the $G_{a\\gamma\\gamma}$--$m_a$ parameter space.","url_abs":"https://arxiv.org/abs/2109.03244v2","url_pdf":"https://arxiv.org/pdf/2109.03244v2.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"muonic-boson-limits-supernova-redux","repo_url":"https://github.com/marie-lecroq/alp-fluence-calculation","is_official":0,"mentioned_in_paper":0,"mentioned_in_github":1,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}