Physics
Scientific paper
Aug 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phrvd..40..942r&link_type=abstract
Physical Review D (Particles and Fields), Volume 40, Issue 4, 15 August 1989, pp.942-947
Physics
21
Radiative Transfer, Scattering, Elementary Particle Processes, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages
Scientific paper
We investigate the effects of massive pseudoscalar particles χ on stellar evolution, focusing on the case where these new states interact only with electrons. If the effective fine-structure constant αx is sufficiently small, they escape freely and rob stellar interiors of energy; if it is so large that they scatter or decay in the star, they contribute to the radiative energy transfer. In this case, their thermal number density must be suppressed by a Boltzmann factor e-mx/T in order to avoid excessive heat transport. We derive general expressions for the energy transport by massive bosons and calculate all relevant contributions to the opacity in the limit mx>>T. In order to avoid either excessive energy loss or excessive energy transport in the Sun, we exclude the parameter range -19+0.32mx-4.5 lnmx<~lnαx<~2.3 -0.32mx+0.5 lnmx, where the particle mass mx is in units of keV. More restrictive constraints are derived from the observed properties of horizontal-branch stars. This excludes a recent suggestion that the presence of a γχ channel accounts for the anomalous decay width of orthopositronium. We stress the importance of numerical studies of both horizontal-branch stars and red giants.
Starkman Glenn D.
~Raffelt Georg G.
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