APS : Cooling the Shock: New Supernova Constraints on Dark Photons

Caputo, Andrea; Raffelt, Georg; Janka, Hans-Thomas; Yun, Seokhoon

doi:10.1103/PhysRevLett.134.151002

Article
Report number	arXiv:2502.01731
Title	Cooling the Shock: New Supernova Constraints on Dark Photons
Related title	Dark Photons can Prevent Core-Collapse Supernova Explosions
Author(s)	Caputo, Andrea (CERN ; U. Rome La Sapienza (main)) ; Janka, Hans-Thomas (Garching, Max Planck Inst.) ; Raffelt, Georg (Garching, Max Planck Inst.) ; Yun, Seokhoon (IBS, Daejeon, CTPU)
Publication	2025-04-16
Imprint	2025-02-03
Number of pages	9
Note	Version published in PRL
In:	Phys. Rev. Lett. 134 (2025) 151002
DOI	10.1103/PhysRevLett.134.151002 (publication)
Subject category	astro-ph.HE ; Astrophysics and Astronomy ; hep-ph ; Particle Physics - Phenomenology
Abstract	During the accretion phase of a core-collapse supernova (SN), dark-photon (DP) cooling can be largest in the gain layer below the stalled shock wave. In this way, it could counter-act the usual shock rejuvenation by neutrino energy deposition and thus prevent the explosion. This peculiar energy-loss profile derives from the resonant nature of DP production. The largest cooling and thus strongest constraints obtain for DP masses of 0.1-0.4 MeV, a range corresponding to the photon plasma mass in the gain region. Electron-capture SNe, once observationally unambiguously identified, could provide strong bounds even down to nearly 0.01 MeV. For a coupling strength so small that neutrino-driven explosions are expected to survive, the DP cooling of the core is too small to modify the neutrino signal, i.e., our new argument supersedes the traditional SN1987A cooling bound.
Copyright/License	preprint: © 2025 The author(s) (License: arXiv nonexclusive-distrib 1.0) publication: © 2025 The author(s) (License: CC BY 4.0), sponsored by SCOAP³

$Numerical results for SN explosion model s18.88-LS220, 1D counterpart of 3D models in \cite{Bollig:2020phc}. \textbf{Left:} Time evolution of the plasma frequency at the position of the gain radius (red) and shock radius (blue). When a horizontal dashed line for a given DP mass falls between the red and blue curves, then transverse DPs are resonantly produced in the gain layer. \textbf{Right:} Differential DP luminosity as a function of radius 0.2~s pb for $m_{\gamma'}=0.3\,\rm MeV$ and $\varepsilon \simeq 10^{-8}$, the SN1987A cooling limit. {\em Green~curve} for longitudinal DPs, {\em blue} for transverse modes, showing a resonance near 80~km. The {\em orange and red curves} are neutrino cooling and heating. The vertical dashed lines indicate the gain radius $r_\mathrm{gain}$ and shock radius $r_\mathrm{shock}$.$ $Numerical results for SN explosion model s18.88-LS220, 1D counterpart of 3D models in \cite{Bollig:2020phc}. \textbf{Left:} Time evolution of the plasma frequency at the position of the gain radius (red) and shock radius (blue). When a horizontal dashed line for a given DP mass falls between the red and blue curves, then transverse DPs are resonantly produced in the gain layer. \textbf{Right:} Differential DP luminosity as a function of radius 0.2~s pb for $m_{\gamma'}=0.3\,\rm MeV$ and $\varepsilon \simeq 10^{-8}$, the SN1987A cooling limit. {\em Green~curve} for longitudinal DPs, {\em blue} for transverse modes, showing a resonance near 80~km. The {\em orange and red curves} are neutrino cooling and heating. The vertical dashed lines indicate the gain radius $r_\mathrm{gain}$ and shock radius $r_\mathrm{shock}$.$ $SN related DP constraints, all computed in the same SN model; for references see main text. {\em Solid red:} Above this line, DP cooling prevents shock revival by neutrino heating (this work) using $\xi_{\gamma'/\nu} = 0.2$. {\em Dot-dashed red:} same for the ECSN-like model, but with $\xi_{\gamma'/\nu} = 0.5$. {\em Blue dashed:} DP luminosity dominates before shock revival for comparison. {\em Black line and shaded gray region:} excessive PNS cooling excluded by SN1987A. {\em Orange:} excessive diffuse $\gamma$-ray flux from DP decay emitted by all cosmic SNe. {\em Magenta:} $\gamma$-ray limits from SN1987A. {\em Green:} excessive energy deposition in low-E SNe, causing excessive explosion energies. {\em Brown:} DP-induced fireball formation. {\em Dashed black:} above this line, DPs are thermally overproduced before matter-radiation equality in standard cosmology.$ Show more plots

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Zapis kreiran 2025-02-06, zadnja izmjena 2025-05-18

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