SOLAR CONSTRAINTS ON ASYMMETRIC DARK MATTER

Here, we constrain [eta]ADM by investigating the impact of such a type of dark matter on the evolution of the Sun, namely, the flux of solar neutrinos and helioseismology. We find that dark matter particles with a mass smaller than 15 GeV, a spin-independent scattering cross section on baryons of th...

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Published inThe Astrophysical journal Vol. 757; no. 2; pp. 1 - 8
Main Authors Lopes, Ilidio, Silk, Joseph
Format Journal Article
LanguageEnglish
Published United States American Astronomical Society 01.10.2012
Subjects
ANNIHILATION
ANTIBARYONS
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ASYMMETRY
Baryons
COSMOLOGY
CROSS SECTIONS
Dark matter
Density
Flux
GEV RANGE
Helioseismology
NONLUMINOUS MATTER
P WAVES
S WAVES
Sciences of the Universe
SOLAR NEUTRINOS
SPIN
STAR EVOLUTION
SUN
UNIVERSE
WEAK INTERACTIONS
elementary particles
High Energy Physics - Phenomenology
Sun: interior
stars: interiors
stars: evolution
Astrophysics - Galaxy Astrophysics
High Energy Physics - Experiment
dark matter
Astrophysics - Cosmology and Extragalactic Astrophysics
Astrophysics - Solar and Stellar Astrophysics
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Summary:Here, we constrain [eta]ADM by investigating the impact of such a type of dark matter on the evolution of the Sun, namely, the flux of solar neutrinos and helioseismology. We find that dark matter particles with a mass smaller than 15 GeV, a spin-independent scattering cross section on baryons of the order of a picobam, and an [eta]-asymmetry with a value in the interval 10 super(-12)-10 super(-1), would induce a change in solar neutrino fluxes in disagreement with current neutrino flux measurements. This result is also confirmed by helioseismology data. A natural consequence of this model is suppressed annihilation, thereby reducing the tension between indirect and direct dark matter detection experiments, but the model also allows a greatly enhanced annihilation cross section. All the cosmological [eta]ADM scenarios that we discuss have a relic dark matter density [Omega]h super(2) and baryon asymmetry [eta] sub(B) in agreement with the current WMAP measured values, [Omega] sub(DM)h super(2) = 0.1109 + or - 0.0056 and [eta] sub(B) = 0.88 x 10 super(-10).
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ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/757/2/130