SOLAR NEUTRINO PHYSICS: SENSITIVITY TO LIGHT DARK MATTER PARTICLES

被引：16

作者：

Lopes, Ilidio ^{[1
,2
]}

Silk, Joseph ^{[3
,4
,5
]}

机构：

[1] Univ Tecn Lisboa, Inst Super Tecn, Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal

[2] Univ Evora, Dept Fis, Escola Ciencia & Tecnol, Colegio Luis Antonio Verney, P-7002554 Evora, Portugal

[3] Univ Paris 06, UMR CNRS 7095, Inst Astrophys Paris, F-75014 Paris, France

[4] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[5] Univ Oxford, Beecroft Inst Particle Astrophys & Cosmol, Oxford OX1 3RH, England

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 752卷 / 02期

关键词：

dark matter; elementary particles; stars: evolution; stars: interiors; Sun: interior; HELIOSEISMOLOGY; MODELS; EVOLUTION; STARS; PROBE; I;

D O I：

10.1088/0004-637X/752/2/129

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Neutrinos are produced in several neutrino nuclear reactions of the proton-proton chain and carbon-nitrogen-oxygen cycle that take place at different radii of the Sun's core. Hence, measurements of solar neutrino fluxes provide a precise determination of the local temperature. The accumulation of non-annihilating light dark matter particles (with masses between 5 GeV and 16 GeV) in the Sun produces a change in the local solar structure, namely, a decrease in the central temperature of a few percent. This variation depends on the properties of the dark matter particles, such as the mass of the particle and its spin-independent scattering cross-section on baryon-nuclei, specifically, the scattering with helium, oxygen, and nitrogen among other heavy elements. This temperature effect can be measured in almost all solar neutrino fluxes. In particular, by comparing the neutrino fluxes generated by stellar models with current observations, namely B-8 neutrino fluxes, we find that non-annihilating dark matter particles with a mass smaller than 10 GeV and a spin-independent scattering cross-section with heavy baryon-nuclei larger than 3 x 10(-37) cm(-2) produce a variation in the B-8 neutrino fluxes that would be in conflict with current measurements.

引用

页数：7

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