Neutrino fluxes from constrained minimal supersymmetric standard model lightest supersymmetric particle annihilations in the Sun
2010 (English)In: Physical Review D. Particles and fields, ISSN 0556-2821, E-ISSN 1089-4918, Vol. 81, no 8, 85004- p.Article in journal (Refereed) Published
We evaluate the neutrino fluxes to be expected from neutralino lightest supersymmetric particle (LSP) annihilations inside the Sun, within the minimal supersymmetric extension of the standard model with supersymmetry-breaking scalar and gaugino masses constrained to be universal at the grand unified theory scale [the constrained minimal supersymmetric standard model (CMSSM)]. We find that there are large regions of typical CMSSM (m(1/2), m(0)) planes where the LSP density inside the Sun is not in equilibrium, so that the annihilation rate may be far below the capture rate. We show that neutrino fluxes are dependent on the solar model at the 20% level, and adopt the AGSS09 model of Serenelli et al. for our detailed studies. We find that there are large regions of the CMSSM (m(1/2), m(0)) planes where the capture rate is not dominated by spin-dependent LSP-proton scattering, e. g., at large m(1/2) along the CMSSM coannihilation strip. We calculate neutrino fluxes above various threshold energies for points along the coannihilation/rapid-annihilation and focus-point strips where the CMSSM yields the correct cosmological relic density for tan beta = 10 and 55 for mu > 0, exploring their sensitivities to uncertainties in the spin-dependent and-independent scattering matrix elements. We also present detailed neutrino spectra for four benchmark models that illustrate generic possibilities within the CMSSM. Scanning the cosmologically favored parts of the parameter space of the CMSSM, we find that the IceCube/DeepCore detector can probe at best only parts of this parameter space, notably the focus-point region and possibly also at the low-mass tip of the coannihilation strip.
Place, publisher, year, edition, pages
2010. Vol. 81, no 8, 85004- p.
IdentifiersURN: urn:nbn:se:su:diva-50675DOI: 10.1103/PhysRevD.81.085004ISI: 000277205000121OAI: oai:DiVA.org:su-50675DiVA: diva2:382332
authorCount :42010-12-302010-12-302010-12-30Bibliographically approved