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Abstract
We consider tomography of the Earth's interior using the neutrino pair beam which has recently been proposed. The beam produces a large amount of neutrino and antineutrino pairs from the circulating partially stripped ions and provides the possibility to measure precisely the energy spectrum of neutrino oscillation probability together with a sufficiently large detector. It is shown that the pair beam gives a better sensitivity to probe the Earth's crust compared with the neutrino sources at present. In addition we present a method to reconstruct a matter density profile by means of the analytic formula of the oscillation probability in which the matter effect is included perturbatively to the second order.
Highlights
Our understanding of neutrino has improved greatly since the end of the last century
This letter is organized as follows: In section 2 we briefly review the neutrino oscillation in matter and present the analytic formula of the oscillation probability based on the perturbation of the matter effect, which will be used to reconstruct the density profile ρ(x)
The tomography by the neutrino pair beam under consideration relies on the oscillation probability of νe → νe as explained in the previous section, and we are faced with this problem
Summary
Our understanding of neutrino has improved greatly since the end of the last century. By measuring the absorption rates of neutrinos passing through the object from different angles, the image of the object can be reconstructed This is similar to the computed tomography using x-rays, which enables us to probe inside solids without destruction. The second one is inherent in the tomography using the oscillation between flavor neutrinos It has been shown [49, 50, 51] that the flavor oscillation probability with the density profile ρ(x) is the same as that with ρ(L − x) where x = 0 or L is the production or detection position, if only two flavors of neutrinos are considered. It has been, proposed that the difficulty can be avoided by using the transition probability of mass eigenstate to flavor eigenstate, which can be realized for the solar and supernova neutrinos [54, 32].
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