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.
Particle Physics from Stars
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abstract
Low-mass particles such as neutrinos, axions, other Nambu-Goldstone bosons and gravitons are produced in the hot and dense interior of stars. Therefore, astrophysical arguments constrain the properties of these particles in ways which are often complementary to cosmological arguments and to laboratory experiments. This review provides an update on the most important stellar-evolution limits and discusses them in the context of other information from cosmology and laboratory experiments.
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Supernova models yield coupling limits g_a ≲ 0.9×10^{-10} and g_φ ≲ 0.4×10^{-10} for masses above 100 keV from gamma-ray observations, plus stronger trapping-regime limits from explosion energy, that are difficult to reconcile with a muon g-2 explanation.
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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.
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Muonic Boson Limits: Supernova Redux
Supernova models yield coupling limits g_a ≲ 0.9×10^{-10} and g_φ ≲ 0.4×10^{-10} for masses above 100 keV from gamma-ray observations, plus stronger trapping-regime limits from explosion energy, that are difficult to reconcile with a muon g-2 explanation.