Constraints on Neutrino Oscillations Using 1258 Days of Super-Kamiokande Solar Neutrino Data

Fukuda, Seisuke; Fukuda, Y.; Ishitsuka, M.; Itow, Y.; Kajita, T.; Kameda, J.; Kaneyuki, K.; Kobayashi, Kazuyoshi; Koshio, Y.; Miura, M.; Moriyama, S.; Nakahata, M.; Nakayama, S.; Okada, Atsushi; Sakurai, N.; Shiozawa, M.; Suzuki, Y.; Takeuchi, Hideki; Takeuchi, Y.; Toshito, T.; Totsuka, Y.; Yamada, Shoichi; Desai, S.; Earl, M.; Kearns, E.; Messier, M. D.; Scholberg, K.; Stone, J. L.; Sulak, L.; Walter, C. W.; Goldhaber, M.; Barszczak, T.; Casper, D.; Gajewski, W.; Kropp, W. R.; Mine, S.; Liu, D. W.; Price, L. R.; Smy, M. B.; Sobel, H. W.; Vagins, M. R.; Ganezer, K. S.; Keig, W. E.; Ellsworth, R. W.; Tasaka, S.; Kibayashi, A.; Learned, J. G.; Matsuno, S.; Takemori, D.; Hayato, Y.; Ishii, T.; Kobayashi, T.; Nakamura, K.; Obayashi, Y.; Oyama, Y.; Sakai, Akito; Sakuda, M.; Kohama, M.; Inagaki, T.; Nakaya, T.; Nishikawa, K.; Haines, T. J.; Blaufuss, E.; Dazeley, S.; Lee, K. B.; Svoboda, R.; Goodman, J. A.; Guillian, G.; Sullivan, G. W.; Turčan, D.; Habig, A.; Hill, J.; Jung, C. K.; Martens, K.; Malek, M.; Mauger, C.; McGrew, C.; Sharkey, E.; Viren, B.; Yanagisawa, C.; Mitsuda, C.; Miyano, K.; Saji, C.; Shibata, Tadashi; Kajiyama, Yuji; Nagashima, Y.; Nitta, K.; Takita, M.; Yoshida, Masato; Kim, H. I.; Kim, S. B.; Yoo, J.; Okazawa, H.; Ishizuka, T.; Etoh, M.; Gando, Y.; Hasegawa, T.; Inoue, K.; Ishihara, K.; Maruyama, T.; Shirai, J.; Suzuki, A.; Koshiba, M.; Hatakeyama, Yutaka; Ichikawa, Yasumasa; Koike, Masafumi; Nishijima, K.; Fujiyasu, H.; Ishino, H.; Morii, M.; Watanabe, Y.; Golebiewska, Urszula; Kiełczewska, D.; Boyd, S.; Stachyra, A. L.; Wilkes, R. J.; Young, K. K.

doi:10.1103/physrevlett.86.5656

Cited by 600 publications

(195 citation statements)

References 21 publications

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“…This is due to the severe inadequacies in the SM as it fails to explain many experimentally observed phenomena and address some theoretical questions. One such observed phenomena is the tiny but non-zero neutrino masses and large neutrino mixing [1][2][3][4][5]. Due to the absence of right handed neutrinos, one can not write down a Dirac mass term for the neutrinos whereas the Majorana mass term for the neutrinos are disallowed by the gauge structure of SM.…”

Section: Introductionmentioning

confidence: 99%

Neutrinoless double beta decay in type I+II seesaw models

Borah

Dasgupta

2015

J. High Energ. Phys.

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We study neutrinoless double beta decay in left-right symmetric extension of the standard model with type I and type II seesaw origin of neutrino masses. Due to the enhanced gauge symmetry as well as extended scalar sector, there are several new physics sources of neutrinoless double beta decay in this model. Ignoring the left-right gauge boson mixing and heavy-light neutrino mixing, we first compute the contributions to neutrinoless double beta decay for type I and type II dominant seesaw separately and compare with the standard light neutrino contributions. We then repeat the exercise by considering the presence of both type I and type II seesaw, having non-negligible contributions to light neutrino masses and show the difference in results from individual seesaw cases. Assuming the new gauge bosons and scalars to be around a TeV, we constrain different parameters of the model including both heavy and light neutrino masses from the requirement of keeping the new physics contribution to neutrinoless double beta decay amplitude below the upper limit set by the GERDA experiment and also satisfying bounds from lepton flavor violation, cosmology and colliders.

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Section: Introductionmentioning

confidence: 99%

Neutrinoless double beta decay in type I+II seesaw models

Borah

Dasgupta

2015

J. High Energ. Phys.

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“…Neutrino that is produced in a flavour eigenstate, which is some linear superposition of mass eigenstates, can latter be measured as being of a different flavour, due to different mass eigenstates acquiring a different phase during propagation. In particular, oscillations of atmospheric neutrinos suggest a squared mass difference of |∆m 2 23 | = |m 2 3 − m 2 2 | =∼ 2.5 × 10 −3 eV 2 [20,21], while solar neutrino observations, together with results from the KamLAND reactor neutrino experiment, point towards ∆m 2 12 = m 2 2 − m 2 1 =∼ 5 × 10 −5 eV 2 [22,23]. Note that in the former case, the sign of the difference is not know, while in the latter it is.…”

Section: Introductionmentioning

confidence: 99%

Detecting neutrino mass difference with cosmology

Slosar

2006

Phys. Rev. D

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Cosmological parameter estimation exercises usually make the approximation that the three standard neutrinos have degenerate mass, which is at odds with recent terrestrial measurements of the difference in the square of neutrino masses. In this paper we examine whether the use of this approximation is justified for the cosmic microwave background (CMB) spectrum, matter power spectrum and the CMB lensing potential power spectrum. We find that, assuming δm 2 23 ∼ 2.5 × 10 −3 eV 2 in agreement with recent Earth based measurements of atmospheric neutrino oscillations, the correction due to non-degeneracy is of the order of precision of present numerical codes and undetectable for the foreseeable future for the CMB and matter power spectra. An ambitious experiment that could reconstruct the lensing potential power spectrum to the cosmic variance limit up to ℓ ∼ 1000 will have to take the effect into account in order to avoid biases. The degeneracies with other parameters, however, will make the detection of the neutrino mass difference impossible. We also show that relaxing the bound on the neutrino mass difference will also increase the error-bar on the sum of neutrino masses by a factor of up to a few. For exotic models with significantly non-degenerate neutrinos the corrections due to non-degeneracy could become important for all the cosmological probes discussed here.

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“…The recent neutrino experiments MINOS [7], T2K [8], Double ChooZ [9], Daya-Bay [10] and RENO [11] have not only confirmed the earlier observations of tiny neutrino masses, but also measured the neutrino parameters more precisely. The 3σ global fit values of neutrino oscillation parameters that have appeared in the recent analysis of [12] and [13] are shown in table 1.…”

Section: Introductionmentioning

confidence: 99%

“…Observations of non-zero neutrino masses and mixing [1][2][3][4][5][6] has been one of the most compelling evidences of the existence of beyond standard model (BSM) physics. Although the recently observed Higgs boson is believed to be responsible for the masses of all the known fundamental particles, it can not account for observed neutrino masses due to the absence of any renormalizable couplings between the Higgs and neutrino fields.…”

Section: Introductionmentioning

confidence: 99%

Charged lepton flavour violcxmation and neutrinoless double beta decay in left-right symmetric models with type I+II seesaw

Borah

Dasgupta

2016

J. High Energ. Phys.

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We study the new physics contributions to neutrinoless double beta decay (0νββ) half-life and lepton flavour violation (LFV) amplitude within the framework of the minimal left-right symmetric model (MLRSM). Considering all possible new physics contributions to 0νββ and charged lepton flavour violation µ → eγ, µ → 3e in MLRSM, we constrain the parameter space of the model from the requirement of satisfying existing experimental bounds. Assuming the breaking scale of the left-right symmetry to be O(1) TeV accessible at ongoing and near future collider experiments, we consider the most general type I+II seesaw mechanism for the origin of tiny neutrino masses. Choosing the relative contribution of the type II seesaw term allows us to calculate the right handed neutrino mass matrix as well as Dirac neutrino mass matrix as a function of the model parameters, required for the calculation of 0νββ and LFV amplitudes. We show that such a general type I+II seesaw structure results in more allowed parameter space compared to individual type I or type II seesaw cases considered in earlier works. In particular, we show that the doubly charged scalar masses M ∆ are allowed to be smaller than the heaviest right handed neutrino mass M N from the present experimental bounds in these scenarios which is in contrast to earlier results with individual type I or type II seesaw showing M ∆ > M N .

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Constraints on Neutrino Oscillations Using 1258 Days of Super-Kamiokande Solar Neutrino Data

Cited by 600 publications

References 21 publications

Neutrinoless double beta decay in type I+II seesaw models

Neutrinoless double beta decay in type I+II seesaw models

Detecting neutrino mass difference with cosmology

Charged lepton flavour violcxmation and neutrinoless double beta decay in left-right symmetric models with type I+II seesaw

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