Neutrino constraints on inelastic dark matter after CDMS II results

Journal Article · Tue Jun 15 00:00:00 EDT 2010 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PHYSREVD.81.123519· OSTI ID:21408052

Jing, Shu ^[1]; Pengfei, Yin; Shouhua, Zhu ^[2]

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1. Institute for the Physics and Mathematics of the Universe, University of Tokyo, Chiba 277-8568 (Japan)
2. Institute of Theoretical Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871 (China)

We discuss the neutrino constraints from solar and terrestrial dark matter (DM) annihilations in the inelastic dark matter (iDM) scenario after the recent CDMS II results. To reconcile the DAMA/LIBRA data with constraints from all other direct experiments, the iDM needs to be light (m{sub {chi}}<100 GeV) and have a large DM-nucleon cross section ({sigma}{sub n{approx}}10{sup -4} pb in the spin-independent (SI) scattering and {sigma}{sub n{approx}}10 pb in the spin-dependent (SD) scattering). The dominant contribution to the iDM capture in the Sun is from scattering off Fe/Al in the SI/SD case. Current bounds from Super-Kamiokande exclude the hard DM annihilation channels, such as W{sup +}W{sup -}, ZZ, tt, and {tau}{sup +{tau}-}. For soft channels such as bb and cc, the limits are loose, but could be tested or further constrained by future IceCube plus DeepCore. For neutrino constraints from the DM annihilation in the Earth, due to the weaker gravitational effect of the Earth and inelastic capture condition, the constraint exists only for small mass splitting {delta}<40 keV and m{sub {chi}}{approx}(10,50) GeV even in the {tau}{sup +{tau}-} channel.

• OSTI ID: 21408052
• Journal Information: Physical Review. D, Particles Fields, Vol. 81, Issue 12; Other Information: DOI: 10.1103/PhysRevD.81.123519; (c) 2010 The American Physical Society; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
ANNIHILATION
CAPTURE
CROSS SECTIONS
GEV RANGE 10-100
KEV RANGE 10-100
MASS
NEUTRINOS
NONLUMINOUS MATTER
NUCLEONS
SCATTERING
SOLAR NEUTRINOS
SPIN
SUN
ANGULAR MOMENTUM
BARYONS
ELEMENTARY PARTICLES
ENERGY RANGE
FERMIONS
GEV RANGE
HADRONS
INTERACTIONS
KEV RANGE
LEPTONS
MAIN SEQUENCE STARS
MASSLESS PARTICLES
MATTER
PARTICLE INTERACTIONS
PARTICLE PROPERTIES
RADIATIONS
SOLAR PARTICLES
SOLAR RADIATION
STARS
STELLAR RADIATION