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Phys. Rev. D 67, 093004 (2003) [28 pages]

Prospects of very long baseline neutrino oscillation experiments with the KEK-JAERI high intensity proton accelerator

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Mayumi Aoki1,*, K. Hagiwara1, Y. Hayato2,†, T. Kobayashi2,‡, T. Nakaya3,§, K. Nishikawa3,**, and N. Okamura4,††
1Theory Group, KEK, Tsukuba, Ibaraki 305-0801, Japan
2Institute of Particle and Nuclear Studies, High Energy Accelerator Research Org. (KEK), Tsukuba, Ibaraki 305-0801, Japan
3Department of Physics, Kyoto University, Kyoto 606-8502, Japan
4IPPAP, Physics Department, Virginia Tech., Blacksburg, Virginia 24061

Received 27 December 2001; revised 19 February 2003; published 20 May 2003

We study the physics potential of very long baseline neutrino-oscillation experiments with a high intensity proton accelerator which will be completed by the year 2007 in Tokai-village, as a joint project of KEK and JAERI (Japan Atomic Energy Research Institute). The 50 GeV proton synchrotron at J-PARC (Japan Proton Accelerator Research Complex) will deliver neutrino beams in the range of a few GeV with an intensity about two orders of magnitude higher than the present KEK beam for the K2K experiment. As a sequel to the proposed J-PARC–to–Super-Kamiokande experiment, we study the impact of experiments with a 100 kton-level detector and a baseline length of a few-thousand km. The pulsed narrow-band νμ beams allow us to measure the νμνe transition probability and the νμ survival probability through counting experiments at a large water-Čerenkov detector. We study the sensitivity of such experiments to the neutrino mass hierarchy, the mass-squared differences, the three angles, and one CP phase of the three-generation lepton-flavor-mixing matrix. We find that experiments at a distance between 1000 and 2000 km can determine the sign of the larger mass-squared difference (m32-m12) if the mixing between νe and ν3 (the heaviest-or-lightest neutrino) is not too small: 4|Ue3|2(1-|Ue3|2)0.03. The CP phase can be constrained if the |Ue3| element is sufficiently large: 4|Ue3|2(1-|Ue3|2)0.06, and if the smaller mass-squared difference (m22-m12) and the Ue2 element are in the preferred range of the large-mixing-angle solution of the solar-neutrino deficit. The magnitude |m32-m12| and the matrix element Uμ3 can be precisely measured, but we find little sensitivity to m22-m12 and the matrix element Ue2.

© 2003 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevD.67.093004
DOI:
10.1103/PhysRevD.67.093004
PACS:
14.60.Lm, 14.60.Pq

*Email address: mayumi.aoki@kek.jp

Email address: hayato@neutrino.kek.jp

Email address: takashi.kobayashi@kek.jp

§Email address: nakaya@scphys.kyoto-u.ac.jp

**Email address: nishikaw@neutrino.kek.jp

††Email address: nokamura@vt.edu