Muonic Boson Limits: Supernova Redux
Fuente:
arXiv
Guardado en:
| Autores principales: | , , |
|---|---|
| Formato: | Preprint |
| Publicado: |
2021
|
| Materias: | |
| Acceso en línea: | |
| Etiquetas: |
Agregar Etiqueta
Sin Etiquetas, Sea el primero en etiquetar este registro!
|
| _version_ | 1866910098250530816 |
|---|---|
| author | Caputo, Andrea Raffelt, Georg Vitagliano, Edoardo |
| author_facet | Caputo, Andrea Raffelt, Georg Vitagliano, Edoardo |
| contents | 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 $ϕ$ in addition to pseudoscalars $a$ and to include systematically the generic two-photon coupling $G_{γγ}$ implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound $G_{γγ}<0.67\times10^{-10}~{\rm GeV}^{-1}$ derived for axion-like particles carries over to the muonic Yukawa couplings as $g_a<3.1\times10^{-9}$ and $g_ϕ< 4.6\times10^{-9}$ for $m_{a,ϕ}\lesssim 100$ keV, so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN1987A $γ$ rays and the diffuse cosmic $γ$-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 $γ$ rays, for $m_{a,ϕ}\gtrsim 100$keV implying $g_a \lesssim 0.9\times10^{-10}$ and $g_ϕ\lesssim 0.4\times10^{-10}$. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match $L_ν$ for $g_{a,ϕ}\simeq 10^{-4}$. However, the $2γ$ 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 $g_ϕ\gtrsim 4\times10^{-3}$. Muonic scalars can explain the muon magnetic-moment anomaly for $g_ϕ\simeq 0.4\times10^{-3}$, 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 $G_{aγγ}$--$m_a$ parameter space. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2109_03244 |
| institution | arXiv |
| publishDate | 2021 |
| record_format | arxiv |
| spellingShingle | Muonic Boson Limits: Supernova Redux Caputo, Andrea Raffelt, Georg Vitagliano, Edoardo High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena High Energy Physics - Experiment 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 $ϕ$ in addition to pseudoscalars $a$ and to include systematically the generic two-photon coupling $G_{γγ}$ implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound $G_{γγ}<0.67\times10^{-10}~{\rm GeV}^{-1}$ derived for axion-like particles carries over to the muonic Yukawa couplings as $g_a<3.1\times10^{-9}$ and $g_ϕ< 4.6\times10^{-9}$ for $m_{a,ϕ}\lesssim 100$ keV, so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN1987A $γ$ rays and the diffuse cosmic $γ$-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 $γ$ rays, for $m_{a,ϕ}\gtrsim 100$keV implying $g_a \lesssim 0.9\times10^{-10}$ and $g_ϕ\lesssim 0.4\times10^{-10}$. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match $L_ν$ for $g_{a,ϕ}\simeq 10^{-4}$. However, the $2γ$ 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 $g_ϕ\gtrsim 4\times10^{-3}$. Muonic scalars can explain the muon magnetic-moment anomaly for $g_ϕ\simeq 0.4\times10^{-3}$, 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 $G_{aγγ}$--$m_a$ parameter space. |
| title | Muonic Boson Limits: Supernova Redux |
| topic | High Energy Physics - Phenomenology Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena High Energy Physics - Experiment |
| url | https://arxiv.org/abs/2109.03244 |