Axion Mass Limits from Cooling Neutron Stars

(2) University of Toledo; (3)Montana State Univ.); Hideyuki Umeda(1); Ken'ichi Nomoto(1) ((1) Research Center for the Early Universe; Letao Qin(3); Naoki Iwamoto(2); Sachiko Tsuruta(3); University of Tokyo

Axion Mass Limits from Cooling Neutron Stars

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arxiv astro-ph/9806337 v1 pith:VM674ZXY submitted 1998-06-25 astro-ph

Hideyuki Umeda(1) , Naoki Iwamoto(2) , Sachiko Tsuruta(3) , Letao Qin(3) , Ken'ichi Nomoto(1) ((1) Research Center for the Early Universe , University of Tokyo , (2) University of Toledo , (3)Montana State Univ.) This is my paper · ORCID

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abstract

The thermal evolution of a neutron star is studied by including the energy loss due to axion emission. Two axion models and three types of neutron-star matter equation of state are used with the effects of nucleon superfluidity properly taken into account. In comparison with the observational data of PSR0656+14 from ROSAT, the upper limits on the axion mass are found to be $m_a < 0.06 - 0.3$ eV and 0.08$ -$ 0.8 eV for the KSVZ and DFSZ axion models, respectively, with the soft equation of state giving the most stringent limits.

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Testing selectively enhanced QCD axions couplings as an explanation of the RX J1856.5-3754 hard X-ray excess
hep-ph 2026-07 conditional novelty 6.0 of 10

An 18 µeV selectively enhanced QCD axion reproduces the total 2-8 keV flux of RX J1856.5-3754 in unpaired bremsstrahlung, but not the spectral shape; KSVZ axions fall short.

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