Axions produced in supernovae generate a diffuse gamma-ray signal through conversion in magnetic fields, yielding competitive constraints on the axion-photon coupling from COMPTEL, EGRET, and Fermi-LAT data plus forecasts for future MeV telescopes.
Reduction of Weak Interaction Rates in Neutron Stars by Nucleon Spin Fluctuations: Degenerate Case
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abstract
Nucleon spin fluctuations in a dense medium reduce the ``naive'' values of weak interaction rates (neutrino opacities, neutrino emissivities). We extend previous studies of this effect to the degenerate case which is appropriate for neutron stars a few ten seconds after formation. If neutron-neutron interactions by a one-pion exchange potential are the dominant cause of neutron spin fluctuations, a perturbative calculation of weak interaction rates is justified for $T\alt 3m/(4\pi\alpha_\pi^2)\approx 1 MeV$, where $m$ is the neutron mass and $\alpha_\pi\approx15$ the pion fine-structure constant. At higher temperatures, the application of Landau's theory of Fermi liquids is no longer justified, i.e. the neutrons cannot be viewed as simple quasiparticles in any obvious sense.
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UNVERDICTED 2representative citing papers
Collective nucleon scattering in neutron-star matter suppresses the effective absorption of ultralight bosons at the long wavelengths relevant for superradiance, weakening the link between stellar cooling bounds and superradiant instability rates.
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Lights, Camera, Axion: Tracing Axions from Supernovae in the Diffuse $\gamma$-ray Sky
Axions produced in supernovae generate a diffuse gamma-ray signal through conversion in magnetic fields, yielding competitive constraints on the axion-photon coupling from COMPTEL, EGRET, and Fermi-LAT data plus forecasts for future MeV telescopes.
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Stellar Superradiance and Low-Energy Absorption in Dense Nuclear Media
Collective nucleon scattering in neutron-star matter suppresses the effective absorption of ultralight bosons at the long wavelengths relevant for superradiance, weakening the link between stellar cooling bounds and superradiant instability rates.