<i>In situ</i>determination of Earth matter density in a neutrino factory

Minakata, Hisakazu; Uchinami, Shoichi

doi:10.1103/physrevd.75.073013

Cited by 30 publications

(25 citation statements)

References 58 publications

(83 reference statements)

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“…For small values of sin 2 2θ 13 , however, the solar term cannot be easily extracted because of the disappearance channel contamination in the non-magnetized detector. For the superbeam, the performance is similar to that the neutrino factory, and to predictions from past studies [37,47]. Precise numbers at different confidence levels are found in Table 4, assuming that sin 2 2θ 13 = 10 −2 .…”

Section: Measurement Of the Earth's Core Densitysupporting

confidence: 77%

Requirements for a new detector at the South Pole receiving an accelerator neutrino beam

Tang

Winter

2012

J. High Energ. Phys.

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There are recent considerations to increase the photomultiplier density in the IceCube detector array beyond that of DeepCore, which will lead to a lower detector energy threshold and a relatively huge fiducial mass for the neutrino detection. This initiative is known as "Precision IceCube Next Generation Upgrade" (PINGU). We discuss the possibility to send a neutrino beam from one of the major accelerator laboratories in the Northern hemisphere to such a detector. Such an experiment would be unique in the sense that it would be the only neutrino beam where the baseline crosses the Earth's outer core. We study the detector requirements for a beta beam, a neutrino factory beam, and a superbeam, where we consider the cases of both small θ 13 and large θ 13 , as suggested by the recent T2K and Double Chooz results. We illustrate that a flavor-clean beta beam best suits the requirements of such a detector, in particular, that PINGU may replace a magic baseline detector for small values of θ 13 -even in the absence of any energy resolution capability. For large θ 13 , however, a single-baseline beta beam experiment cannot compete if it is constrained by the CERN-SPS. For a neutrino factory, because of the missing charge identification possibility in the detector, a very good energy resolution is required. If this can be achieved, especially a low energy neutrino factory, which does not suffer from the tau contamination, may be an interesting option for large θ 13 . For the superbeam, where we consider the LBNE beam as a reference, electron neutrino flavor identification and statistics are two of the primary limitations. Finally, we demonstrate that in principle the neutrino factory and superbeam options may measure the density of the Earth's core at a sub percent level for sin 2 2θ 13 0.01. a this work if the large increase of statistics by this relatively huge detector mass may compensate for the loss of statistics from the long baseline. More specifically, consider a beta beam, neutrino factory beam, and a superbeam, and establish the detector requirements for each of these beam classes for small and large θ 13 . Sec. 4 discusses our detector parameterization. These requirements may serve as guidance for the optimization of the detector, if it were intended to receive a neutrino beam. Our primary focus is the optimization with respect to the most often used performance indicators, including the θ 13 , mass hierarchy (MH), and CP violation (CPV) discovery reaches as a function of (true) θ 13 and δ CP . Note that the neutrino oscillation physics using such a long core-crossing baseline is quite unique because of the "parametric enhancement" [22, 23] of the oscillation probability; for a detailed discussion, see Sec. 2. Conversely, the density of the Earth's core can be probed with such a neutrino beam [24], which we study in Sec. 7. Earlier works studying a neutrino beam to the South Pole include Refs. [25,26].As far as the different beam classes are concerned, we distinguish setups for small θ 13 , where only an uppe...

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Section: Measurement Of the Earth's Core Densitysupporting

confidence: 77%

Requirements for a new detector at the South Pole receiving an accelerator neutrino beam

Tang

Winter

2012

J. High Energ. Phys.

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“…By looking into the expressions of 9 We note that a different type of the confusion theorem was derived in [27] which involves θ 13 and NSI parameters in production and in propagation processes that obey a special relationship. 10 If we take the setting with only ε ee as NSI, it can be regarded as uncertainty in the matter density and it is known that neutrino factory has a great sensitivity to it [47,48]. However, in our current setting the issue of matter density uncertainty is much more severe and universal; It produces uncertainties in determining all the NSI elements.…”

Section: B Strategy For Parameter Determinationmentioning

confidence: 96%

Perturbation theory of neutrino oscillation with nonstandard neutrino interactions

Kikuchi

Minakata

Uchinami

2009

J. High Energy Phys.

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102

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We discuss various physics aspects of neutrino oscillation with non-standard interactions (NSI). We formulate a perturbative framework by taking ∆m 2 21 /∆m 2 31 , s 13 , and the NSI elements ε αβ (α, β = e, µ, τ ) as small expansion parameters of the same order ǫ. Within the ǫ perturbation theory we obtain the S matrix elements and the neutrino oscillation probability formula to second order (third order in ν e related channels) in ǫ. The formula allows us to estimate size of the contribution of any particular NSI element ε αβ to the oscillation probability in arbitrary channels, and gives a global bird-eye view of the neutrino oscillation phenomena with NSI. Based on the second-order formula we discuss how all the conventional lepton mixing as well as NSI parameters can be determined. Our results shows that while θ 13 , δ, and the NSI elements in ν e sector can in principle be determined, complete measurement of the NSI parameters in the ν µ − ν τ sector is not possible by the rate only analysis. The discussion for parameter determination and the analysis based on the matter perturbation theory indicate that the parameter degeneracy prevails with the NSI parameters. In addition, a new solar-atmospheric variable exchange degeneracy is found. Some general properties of neutrino oscillation with and without NSI are also illuminated.

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“…In addition, there are many other applications of this baseline, see, e.g., Refs. [23,[45][46][47], for non-standard physics, see, e.g., Refs. [24,48].…”

Section: θ 13 Discovered In Phase I+iimentioning

confidence: 99%

Neutrino factory in stages: Low energy, high energy, off-axis

Tang

Winter

2010

Phys. Rev. D

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We discuss neutrino oscillation physics with a neutrino factory in stages, including the possibility of upgrading the muon energy within the same program. We point out that a detector designed for the low energy neutrino factory may be used off-axis in a high energy neutrino factory beam. We include the re-optimization of the experiment depending on the value of θ 13 found. As upgrade options, we consider muon energy, additional baselines, a detector mass upgrade, an off-axis detector, and the platinum (muon to electron neutrino) channels. In addition, we test the impact of Daya Bay data on the optimization. We find that for large θ 13 (θ 13 discovered by the next generation of experiments), a low energy neutrino factory might be the most plausible minimal version to test the unknown parameters. However, if a higher muon energy is needed for new physics searches, a high energy version including an off-axis detector may be an interesting alternative. For small θ 13 (θ 13 not discovered by the next generation), a plausible program could start with a low energy neutrino factory, followed by energy upgrade, and then baseline or detector mass upgrade, depending on the outcome of the earlier phases.

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In situdetermination of Earth matter density in a neutrino factory

Cited by 30 publications

References 58 publications

Requirements for a new detector at the South Pole receiving an accelerator neutrino beam

Requirements for a new detector at the South Pole receiving an accelerator neutrino beam

Perturbation theory of neutrino oscillation with nonstandard neutrino interactions

Neutrino factory in stages: Low energy, high energy, off-axis

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