213 research outputs found

    Dark matter assisted Dirac leptogenesis and neutrino mass

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    We propose a minimal extension of the standard model with U(1)_{B-L} \times Z_{2} symmetry. In this model by assuming that the neutrinos are Dirac (i.e. BLB-L is an exact symmetry), we found a simultaneous solution for non zero neutrino masses and dark matter content of the universe. The observed baryon asymmetry of the universe is also explained using Dirac Leptogenesis, which is assisted by a dark sector, gauged under a U(1)_D symmetry. The latter symmetry of the dark sector is broken at a TeV scale and thereby giving mass to a neutral gauge boson Z_D. The standard model Z-boson mixes with the gauge boson Z_D at one loop level and thus paves a way to detect the dark matter through spin independent elastic scattering at terrestrial laboratories.Comment: 12 pages, 10 figures. Accepted for publication in Nuclear Physics

    keV Warm Dark Matter via the Supersymmetric Higgs Portal

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    Warm dark matter (WDM) may resolve the possible conflict between observed galaxy halos and the halos produced in cold dark matter (CDM) simulations. Here we present an extension of MSSM to include WDM by adding a gauge singlet fermion, \bar{\chi}, with a portal-like coupling to the MSSM Higgs doublets. This model has the property that the dark matter is {\it necessarily warm}. In the case where M_{\bar{\chi}} is mainly due to electroweak symmetry breaking, the \bar{\chi} mass is completely determined by its relic density and the reheating temperature, T_R. For 10^2 GeV < T_{R} < 10^{5} GeV$, the range allowed by \bar{chi} production via thermal Higgs annihilation, the \bar{\chi} mass is in the range 0.3-4 keV, precisely the range required for WDM. The primordial phase-space density, Q, can directly account for that observed in dwarf spheroidal galaxies, Q \approx 5 x 10^{6}(eV/cm^3)/(km/s)^3,, when the reheating temperature is in the range T_R \approx 10-100 TeV, in which case M_{\bar{\chi}} \approx 0.45 keV. The free-streaming length is in the range 0.3-4 Mpc, which can be small enough to alleviate the problems of overproduction of galaxy substructure and low angular momentum of CDM simulations.Comment: 6 pages LaTeX, Significantly expanded discussion. To be published in Physical Review

    Predictive model for dark matter, dark energy, neutrino masses and leptogenesis at the TeV scale

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    We propose a new mechanism of TeV scale leptogenesis where the chemical potential of right-handed electron is passed on to the BLB-L asymmetry of the Universe in the presence of sphalerons. The model has the virtue that the origin of neutrino masses are independent of the scale of leptogenesis. As a result, the model could be extended to explain {\it dark matter, dark energy, neutrino masses and leptogenesis at the TeV scale}. The most attractive feature of this model is that it predicts a few hundred GeV triplet Higgs scalar that can be tested at LHC or ILC.Comment: 5 pages (revtex), double column, 2 eps figures, journal version. To appear in Phys. ReV.

    TeV scale model for neutrino masses, dark matter and leptogenesis

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    We present a TeV scale model for leptogenesis where the origin of neutrino masses are independent of the scale of leptogenesis. As a result, the model could be extended to explain {\it dark matter, neutrino masses and leptogenesis at the TeV scale}. The most attractive feature of this model is that it predicts a few hundred GeV triplet Higgs scalar that can be tested at LHC or ILC.Comment: 4 pages, contribution to International workshop on theoretical high energy physics (IWTHEP), Roorkee, 200

    Gravitino production in an inflationary Universe and implications for leptogenesis

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    Models of leptogenesis are constrained by the low reheat temperature at the end of reheating associated with the gravitino bound. However a detailed view of reheating, in which the maximum temperature during reheating, \Tmax, can be orders of magnitude higher than the reheat temperature, allows for the production of heavy Majorana neutrinos needed for leptogenesis. But then one must also consider the possibility of enhanced gravitino production in such scenarios. In this article we consider gravitino production during reheating, its dependence on \Tmax, and its relevance for leptogenesis. Earlier analytical studies of the gravitino abundance have only considered gravitino production in the post-reheating radiation dominated era. We find that the gravitino abundance generated during reheating is comparable to that generated after reheating. This lowers the upper bound on the reheat temperature by a factor of 4/3.Comment: Journal version, minor change in title, 13 pages (revtex), 2 eps figure

    Gauged BLB-L symmetry and baryogenesis via leptogenesis at TeV scale

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    It is shown that the requirement of preservation of baryon asymmetry does not rule out a scale for leptogenesis as low as 10 TeV. The conclusions are compatible with see-saw mechanism if for example the pivot mass scale for neutrinos is 102\approx 10^{-2} that of the charged leptons. We explore the parameter space m~1\tilde{m}_1-M1M_1 of relevant light and heavy neutrino masses by solving Boltzmann equations. A viable scenario for obtaining baryogenesis in this way is presented in the context of gauged BLB-L symmetry.Comment: 15 pages, 4 figures, references added, match with journal versio

    Cosmic Ray Anomalies and Dark Matter Annihilation to Muons via a Higgs Portal Hidden Sector

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    Annihilating dark matter (DM) models based on a scalar hidden sector with Higgs portal-like couplings to the Standard Model are considered as a possible explanation for recently observed cosmic ray excesses. Two versions of the model are studied, one with non-thermal DM as the origin of the boost factor and one with Sommerfeld enhancement. In the case of non-thermal DM, four hidden sector scalars which transform under a U(1)_{X} symmetry are added. The heaviest scalars decouple and later decay to DM scalars, so providing the boost factor necessary to explain the present DM annihilation rate. The mass of the annihilating scalars is limited to < 600 GeV for the model to remain perturbative. U(1)_{X} breaking to Z_2 at the electroweak transition mixes light O(100) MeV hidden sector scalars with the Higgs. The DM scalars annihilate to these light scalars, which subsequently decay to two mu^{+} mu^{-} pairs via Higgs mixing, so generating a positron excess without antiprotons. Decay to \mu^{+}\mu^{-} rather than e^{+}e^{-} is necessary to ensure a fast enough light scalar decay rate to evade light scalar domination at nucleosynthesis. In the version with Sommerfeld enhancement only three new scalars are necessary. TeV scale DM masses can be accomodated, allowing both the higher energy electron plus positron excess and the lower energy PAMELA positron excess to be explained. DM annihilates to two \mu^{+}\mu^{-} pairs as in the non-thermal model. This annihilation mode may be favoured by recent observations of the electron plus positron excess by FERMI and HESS.Comment: 24 pages, 4 figures. Expanded discussion, conclusions unchanged. Version to be published in Physical Review
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