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BABAR Collaboration(Lees, J. P. et al), Martinez-Vidal, F., & Oyanguren, A. (2011). Branching fraction measurements of the color-suppressed decays B-bar(0) to D((*)0)pi(0), D((*)0)eta, D((*)0)omega, and D((*)0)eta ' and measurement of the polarization in the decay B-bar(0) -> D((*)0)omega. Phys. Rev. D, 84(11), 112007–25pp.
Abstract: We report updated branching fraction measurements of the color-suppressed decays (B) over bar (0) -> D(0)pi(0), D*(0)pi(0), D(0)eta, D*(0)eta, D(0)omega, D*(0)omega, D(0)eta', and D*(0)eta'. We measure the branching fractions (x 10(-4)): B((B) over bar (0) -> D(0)pi(0)) = 2.69 +/- 0.09 +/- 0.13, B((B) over bar (0) -> D(0)pi(0)) = 3.05 +/- 0.14 +/- 0.28, B((B) over bar (0) -> D(0)eta) = 2.53 +/- 0.09 +/- 0.11, B((B) over bar (0) -> D(0)eta) = 2.69 +/- 0.14 +/- 0.23, B((B) over bar (0) -> D(0)eta) = 2.57 +/- 0.11 +/- 0.14, B((B) over bar (0) -> D*(0)omega) = 4.55 +/- 0.24 +/- 0.39, B((B) over bar (0) -> D*(0)omega) = 1.48 +/- 0.13 +/- 0.07, and B((B) over bar (0) -> D*(0)eta') = 1.49 +/- 0.22 +/- 0.15. We also present the first measurement of the longitudinal polarization fraction of the decay channel D*(0)omega, f(L) = (66.5 +/- 4.7 +/- 1.5)%. In the above, the first uncertainty is statistical and the second is systematic. The results are based on a sample of (454 +/- 5) x 10(6) B (B) over bar pairs collected at the Gamma(4S) resonance, with the BABAR detector at the PEP-II storage rings at SLAC. The measurements are the most precise determinations of these quantities from a single experiment. They are compared to theoretical predictions obtained by factorization, Soft Collinear Effective Theory (SCET) and perturbative QCD (pQCD). We find that the presence of final state interactions is favored and the measurements are in better agreement with SCET than with pQCD.
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Fornengo, N., Lineros, R. A., Regis, M., & Taoso, M. (2011). Possibility of a Dark Matter Interpretation for the Excess in Isotropic Radio Emission Reported by ARCADE. Phys. Rev. Lett., 107(27), 271302–5pp.
Abstract: The ARCADE 2 Collaboration has recently measured an isotropic radio emission which is significantly brighter than the expected contributions from known extra-galactic sources. The simplest explanation of such excess involves a "new'' population of unresolved sources which become the most numerous at very low (observationally unreached) brightness. We investigate this scenario in terms of synchrotron radiation induced by weakly interacting massive particle (WIMP) annihilations or decays in extra-galactic halos. Intriguingly, for light-mass WIMPs with a thermal annihilation cross section, the level of expected radio emission matches the ARCADE observations.
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Krauss, M. B., Ota, T., Porod, W., & Winter, W. (2011). Neutrino mass from higher than d=5 effective operators in supersymmetry, and its test at the LHC. Phys. Rev. D, 84(11). Retrieved July 15, 2024, from http://dx.doi.org/10.1103/PhysRevD.84.115023
Abstract: We discuss neutrino masses from higher than d = 5 effective operators in a supersymmetric framework, where we explicitly demonstrate which operators could be the leading contribution to neutrino mass in the minimal supersymmetric standard model and next to minimal supersymmetric standard model. As an example, we focus on the d = 7 operator LLH(u)H(u)H(d)H(u), for which we systematically derive all tree-level decompositions. We argue that many of these lead to a linear or inverse seesaw scenario with two extra neutral fermions, where the lepton number violating term is naturally suppressed by a heavy mass scale when the extra mediators are integrated out. We choose one example, for which we discuss possible implementations of the neutrino flavor structure. In addition, we show that the heavy mediators, in this case SU(2) doublet fermions, may indeed be observable at the LHC, since they can be produced by Drell-Yan processes and lead to displaced vertices when they decay. However, the direct observation of lepton number violating processes is on the edge at LHC.
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Serenelli, A. M., Haxton, W. C., & Pena-Garay, C. (2011). Solar Models With Accretion. I. Application To The Solar Abundance Problem. Astrophys. J., 743(1), 24–20pp.
Abstract: We generate new standard solar models using newly analyzed nuclear fusion cross sections and present results for helioseismic quantities and solar neutrino fluxes. The status of the solar abundance problem is discussed. We investigate whether nonstandard solar models with accretion from the protoplanetary disk might alleviate this problem. We examine a broad range of models, analyzing metal-enriched and metal-depleted accretion and three scenarios for the timing of accretion. Only partial solutions are found. Formetal-rich accreted material (Z(ac) greater than or similar to 0.018) there exist combinations of accreted mass and metallicity that bring the depth of the convective zone into agreement with the helioseismic value. For the surface helium abundance, the helioseismic value is reproduced if metal-poor or metal-free accretion is assumed (Z(ac) less than or similar to 0.09). In both cases a few percent of the solar mass must be accreted. Precise values depend on when accretion takes place. We do not find a simultaneous solution to both problems but speculate that changing the hydrogen-to-helium mass ratio in the accreted material may lead to more satisfactory solutions. We also show that, with current data, solar neutrinos are already a very competitive source of information about the solar core and can help constraining possible accretion histories. Even without helioseismic constraints, solar neutrinos rule out the possibility that more than 0.02 M(circle dot) from the protoplanetary disk were accreted after the Sun settled on the main sequence. Finally, we discuss how measurements of neutrinos from the CN cycle could shed light on the interaction between the early Sun and its protoplanetary disk.
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Agarwalla, S. K., Blennow, M., Fernandez-Martinez, E., & Mena, O. (2011). Neutrino probes of the nature of light dark matter. J. Cosmol. Astropart. Phys., 09(9), 004–19pp.
Abstract: Dark matter particles gravitationally trapped inside the Sun may annihilate into Standard Model particles, producing a flux of neutrinos. The prospects of detecting these neutrinos in future multi-kt neutrino detectors designed for other physics searches are explored here. We study the capabilities of a 34/100 kt liquid argon detector and a 100 kt magnetized iron calorimeter detector. These detectors are expected to determine the energy and the direction of the incoming neutrino with unprecedented precision allowing for tests of the dark matter nature at very low dark matter masses, in the range of 10-25 GeV. By suppressing the atmospheric background with angular cuts, these techniques would be sensitive to dark matter-nucleon spin-dependent cross sections at the fb level, reaching down to a few ab for the most favorable annihilation channels and detector technology.
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