Axion cyclotron emissivity of magnetized white dwarfs and neutron stars

Details Axion cyclotron emissivity of magnetized white dwarfs and neutron stars Axion cyclotron emissivity of magnetized white dwarfs and neutron stars

1997-01-12

arxiv.org/abs/astro-ph/9701056v2

Phys.Rev.D56:1313-1319,1997

Astronomy and Astrophysics

Astrophysics

11 pages, 4 ps figures, revtex. Minor additions and correction of typos. Accepted for publication in Phys. Rev. D

Scientific paper

10.1103/PhysRevD.56.1313

The energy loss rate of a magnetized electron gas emitting axions a due to the process $e^- \to e^- +a$ is derived for arbitrary magnetic field strength B. Requiring that for a strongly magnetized neutron star the axion luminosity is smaller than the neutrino luminosity we obtain the bound $g_{ae}\lsim 10^{-10}$ for the axion electron coupling constant. This limit is considerably weaker than the bound derived earlier by Borisov and Grishina using the same method. Applying a similar argument to magnetic white dwarf stars results in the more stringent bound $g_{ae}\lsim 9x10^{-13} (T/10^7 K)^{5/4} (B/10^{10} G)^{-2}$ where T is the internal temperature of the white dwarf.

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