Axion cyclotron emissivity of magnetized white dwarfs and neutron stars

Simple item page
dc.creatorKachelriess, M.
dc.creatorWilke, C.
dc.creatorWunner, G.
dc.date1997-01-12
dc.date1997-04-08
dc.date.accessioned2026-07-07T10:31:44Z
dc.date.available2026-07-07T10:31:44Z
dc.descriptionThe 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.
dc.description11 pages, 4 ps figures, revtex. Minor additions and correction of typos. Accepted for publication in Phys. Rev. D
dc.identifierhttps://arxiv.org/abs/astro-ph/9701056
dc.identifierhttp://arxiv.org/abs/astro-ph/9701056
dc.identifierPhys.Rev.D56:1313-1319,1997
dc.identifierdoi:10.1103/PhysRevD.56.1313
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/178516
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.titleAxion cyclotron emissivity of magnetized white dwarfs and neutron stars
dc.typetext

Files

Collections

arXiv