Layers of the LapDance Scholarship

Barwick, Emily Moran

doi:10.17077/etd.hmg26wee

Cited by 3 publications

(7 citation statements)

References 15 publications

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“…[29], the positron flux, Φ e + , is also presented. Rescaling the given result, we found that Φ e + from the Wino-like CDM is comparable to the currently measured flux by the HEAT experiment [31] even for m χ ≃ 100 GeV. Therefore, we believe our scenario is not seriously constrained by the present data, but could give a very prominent signal in the future.…”

Section: )supporting

confidence: 78%

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Wino cold dark matter from anomaly mediated SUSY breaking

2000

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The cosmological moduli problem is discussed in the framework of sequestered sector/anomaly-mediated supersymmetry (SUSY) breaking. In this scheme, the gravitino mass (corresponding to the moduli masses) is naturally 10 − 100 TeV, and hence the lifetime of the moduli fields can be shorter than ∼ 1 sec. As a result, the cosmological moduli fields should decay before big-bang nucleosynthesis starts. Furthermore, in the anomaly-mediated scenario, the lightest superparticle (LSP) is the Wino-like neutralino. Although the large annihilation cross section means the thermal relic density of the Wino LSP is too small to be the dominant component of cold dark matter (CDM), moduli decays can produce Winos in sufficient abundance to constitute CDM. If Winos are indeed the dark matter, it will be highly advantageous from the point of view of detection. If the halo density is dominated by the Wino-like LSP, the detection rate of Wino CDM in Ge detectors can be as large as 0.1 − 0.01 event/kg/day, which is within the reach of the future CDM detection with Ge detector. Furthermore, there is a significant positron signal from pair annihilation of Winos in our galaxy which should give a spectacular signal at AMS. *

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Section: )supporting

confidence: 78%

“…#9 In fact, Ref [32]. suggests a distortion in the positron spectrum measured by the HEAT experiment[31]. Positrons from the Wino CDM may be the source of this distortion.…”

mentioning

confidence: 99%

Wino cold dark matter from anomaly mediated SUSY breaking

2000

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“…As upper limits of neutrino fluxes by several experiments, AMANDA-II limits [51,52], limit on tau neutrinos by the PAO [53], ANITA-lite limit [54] are shown. As estimated or projected sensitivities, sensitivity of 3 years observation by IceCube [55], sensitivity of 5 years observation by the PAO [56], ARIANNA sensitivity [57], and full-ANITA sensitivity [54] are also shown. As diffuse neutrino spectra from energetic sources, a maximal neutrino flux from active galactic nuclei including neutrino oscillation [58] and neutrino spectrum from GRBs calculated in Ref.…”

Section: Neutrino Fluxesmentioning

confidence: 99%

Cosmogenic neutrinos as a probe of the transition from Galactic to extragalactic cosmic rays

Takami

Murase

Nagataki

et al. 2009

Astroparticle Physics

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There are two promising scenarios that explain the ankle, which is a dip in the spectrum of cosmic rays at ∼ 10 19 eV. A scenario interprets the ankle as the transition from Galactic to extragalactic cosmic rays (ankle-transition scenario), while the other is that the dip caused by pair production on the cosmic microwave background radiation (proton-dip scenario). In this paper, we consider whether cosmogenic neutrinos can be a clue to judge which scenario is favored. We calculated the fluxes of cosmogenic neutrinos following these scenarios with plausible physical parameter sets, and found several important features as follows. First of all, the neutrino flux at ∼ 10 20 eV becomes much higher in the ankle-transition scenario as long as the maximum energy of the cosmic rays at sources is sufficiently high. On the other hand, the neutrino spectrum has a characteristic peak at ∼ 10 16 eV in the protondip scenario on the condition that extragalactic protons significantly contribute to the observed cosmic rays down to 10 17 eV. Thus, we conclude cosmogenic neutrinos should give us a clue to judge which scenario is favored, unless these features are masked by the neutrino background coming from possible, powerful neutrino sources such as AGNs and GRBs. We also found an interesting feature that the neutrino flux at ∼ 10 18 eV depends only on the cosmological evolution of the cosmic ray sources. That means cosmogenic neutrinos with the energy bring us information on the cosmological evolution of the sources of ultra-high energy cosmic rays. Finally, we compare the fluxes of cosmogenic neutrinos with the expected sensitivity curves of several neutrino detectors, and conclude the detection of cosmogenic neutrinos in the near future is promising.2

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“…The decay to these scalar bosons may occur at a faster rate [64] than that to photons and may therefore have astrophysical and cosmological implications [65]. This will be the subject of another working group [9]; so we only focus on the implications of the magnetic moment in one of the subsequent sections.…”

Section: Neutrino Electromagnetic Dipole Moments and Neutrino Decaymentioning

confidence: 99%

“…We expect this overview to be supplemented by other excellent existing reviews of the subject in the literature. Regarding more references and the more experimental aspects of the topics under study, we refer to the other working group reports, the Solar and Atmospheric Experiments [5], the Reactor [6], the Neutrino Factory and Beta Beam Experiments and Development [7], the Neutrinoless Double Beta Decay and Direct Searches for Neutrino Mass [8] and the Neutrino Astrophysics and Cosmology [9] WGs. In particular, we have not discussed theoretical models for neutrino masses except giving a broad outline of ideas and getting beyond it only when there is a need to make some phenomenological point.…”

Section: Introductionmentioning

confidence: 99%

Theory of Neutrinos: a White Paper

Mohapatra¹,

Antusch²,

Babu³

et al. 2006

157

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During 2004, four divisions of the American Physical Society commissioned a study of neutrino physics to take stock of where the field is at the moment and where it is going in the near and far future. Several working groups looked at various aspects of this vast field. The summary was published as a main report entitled "The Neutrino Matrix" accompanied by short 50 page versions of the report of each working group. Theoretical research in this field has been quite extensive and touches many areas and the short 50 page report [1] provided only a brief summary and overview of few of the important points. The theory discussion group felt that it may be of value to the community to publish the entire study as a white paper and the result is the current article. After a brief overview of the present knowledge of neutrino masses and mixing and some popular ways to probe the new physics implied by recent data, the white paper summarizes what can be learned about physics beyond the Standard Model from the various proposed neutrino experiments. It also comments on the impact of the experiments on our understanding of the origin of the matter-antimatter asymmetry of the Universe and the basic nature of neutrino interactions as well as the existence of possible additional neutrinos. Extensive references to original literature are provided.

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Layers of the LapDance Scholarship

Cited by 3 publications

References 15 publications

Wino cold dark matter from anomaly mediated SUSY breaking

Wino cold dark matter from anomaly mediated SUSY breaking

Cosmogenic neutrinos as a probe of the transition from Galactic to extragalactic cosmic rays

Theory of Neutrinos: a White Paper

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