Testing the LMA solution with solar neutrinos independently of solar models

Barger, V.; Marfatia, Danny; Whisnant, K.

doi:10.1016/j.physletb.2005.04.073

Cited by 21 publications

(15 citation statements)

References 54 publications

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“…A non-zero θ x improves the fit to the intermediate-energy solar neutrinos (compared to the twoneutrino case), at the expense of a slightly worse fit to the low and high-energy solar neutrinos [52].…”

Section: Solar Neutrinosmentioning

confidence: 96%

Confronting mass-varying neutrinos with MiniBooNE

2006

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We study the proposal that mass-varying neutrinos could provide an explanation for the LSND signal forν µ →ν e oscillations. We first point out that all positive oscillation signals occur in matter and that three active mass-varying neutrinos are insufficient to describe all existing neutrino data including LSND. We then examine the possibility that a model with four mass-varying neutrinos (three active and one sterile) can explain the LSND effect and remain consistent with all other neutrino data. We find that such models with a 3 + 1 mass structure in the neutrino sector may explain the LSND data and a null MiniBooNE result for 0.10 < ∼ sin 2 2θ x < ∼ 0.30. Predictions of the model include a null result at Double-CHOOZ, but positive signals for underground reactor experiments and for ν µ → ν e oscillations in long-baseline experiments.

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Section: Solar Neutrinosmentioning

confidence: 96%

Confronting mass-varying neutrinos with MiniBooNE

2006

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“…The NSI matter effects on the pp spectrum are negligible [46] and therefore not included. Because the NSI propagation corrections to the LMA-MSW model [41,[47][48][49] for P ee will be small corrections to small effects below 2 MeV [13] and our CC semi-leptonic source NSI do not enter the matter effects, and, as with the pp spectral shape, we do not include the remaining matter contributions from the ν -e forward scattering process in this paper 6 .…”

Section: A Estimate Of Matter Effects On the ν E Survival Probabilitymentioning

confidence: 99%

sin2 θ W estimate and bounds on nonstandard interactions at source and detector in the solar neutrino low-energy regime

Khan

McKay

2017

J. High Energ. Phys.

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Abstract:We explore the implications of the Borexino experiment's real time measurements of the lowest energy part of the neutrino spectrum from the primary pp fusion process up to 0.420 MeV through the 7 Be decay at 0.862 MeV to the pep reaction at 1.44 MeV. We exploit the fact that at such low energies, the large mixing angle solution to the MikheyevSmirnov-Wolfenstein matter effects in the sun are small for 7 Be and pep and negligible for pp. Consequently, the neutrinos produced in the sun change their flavor almost entirely through vacuum oscillations during propagation from the sun's surface and through possible nonstandard interactions acting at the solar source and Borexino detector. We combine the different NSI effects at source and detector in a single framework and use the current Borexino data to bound NSI non-universal and flavor-changing parameters at energies below the reach of reactor neutrino experiments. We also study the implication of the current data for the weak-mixing angle at this "low-energy frontier" data from the Borexino experiment, where it is expected to be slightly larger than its value at the Z mass. We find sin 2 θ W = 0.224 ± 0.016, the lowest energy-scale estimate to date. Looking to the future, we use projected sensitivities to solar neutrinos in next generation dedicated solar experiments and direct dark matter detection experiments and find a potential factor five improvement in determination of the weak-mixing angle and up to an order of magnitude improvement in probing the NSI parameters space.

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“…the third row mixing matrix elements. Black line is U τ 1 , red is U τ 2 and blue is U τ 3 ; Here, we use an adiabatic MSW effect to reproduce solar neutrino signals, with the choice of N e = 100(/N A /cm 3 ) as electron density in the central region of the Sun [97]. Of course, this model does not predict a signal for LSND and MiniBooNE.…”

Section: Model Construction 531 Bimaximal Modelmentioning

confidence: 99%

“…The trick is that, the eigenvalue difference cancels at the leading order contribution, and the second-order term becomes the leading term, like the seesaw mechanism that generates neutrino mass. short baseline experiments (left is LSND, right is for MiniBooNE), KamLAND (with data points from [83]), atmospheric neutrinos, and solar neutrinos (with data points from [97]). …”

Section: Bicycle Modelmentioning

confidence: 99%

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

Katori

2008

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school was successful since I relied 100% on your support. For FINeSSE, you taught me everything step by step because I didn't know anything. For Lorentz violation, even though it was a spin-off subject for me and you, but you were so generous, supportive, and patient.And for MiniBooNE, the CCQE work couldn't have been done without your ideas. I am really proud of the amount of work I present in this thesis; it is the evidence of what a good work relationship we have. Finally I want to apologize for my bad English and for how you always had to correct it, including in this thesis. This acknowledgments section is the only one place in all my writings for which you didn't correct my English! Thank you Rex.My first three years were supported by the people in Indiana.I wish to give sincere appreciation to Chris Cox and Nikodem Pop lawski, I think it was my fate to see you from the very first day in US. I had a hard time (as you know), but because of your help, I not only survived, but also changed my style to be more suitable in this country. No one ever was so influential for me as Chris, I think. And Niko, before Thank you for sharing good times with me. I also want to thank Hans-Otto Mayer, Jack Doskow, and Gerard Visser for your help and inspiration for the work on FINeSSE. Thank you everyone.My friends from the classroom, it is a very strange feeling that now all we are going somewhere to do something, but we have known each other more than six years! Liliana Cabellero, you changed shy Teppei...to an emotional salsa dancer! If the dancing is my mother of energy, then Lily is founding mother of energetic Teppei. Muchas gracias. Leah Welty and Jason Rieger are the first real American students I met. When you described Chicago, I didn't understand very much, but now, yeah, I love this city and want to stay here more. Heechang Na, thank you for talking with me every time I stopped by your office, v because you are so kind and welcome and easy to talk with! Haiyang "Ocean" Yan, I am proud that I nicknamed you. I think you are a very good physicist. Thank you for teaching me a lot about Chinese history and physics. I always enjoyed it. Masaki (& Shizuka) Ishitsuka is the first Japanese fellow I met at Indiana even though I left Bloomington before you came. I always enjoyed talking about neutrinos with you, your view of physics is very unique and interesting to me. Thank you. Yun-Chan, Tony, George, Jay, Helber, Jorge, Shinya... I had so much fun in Indiana because of you. Thank you very much.One of the reasons I wanted to be a physicist is that physicists make friends all over the world so easily. I met many friends at conferences, summer schools, etc. Thank you to everyone who called me a crazy Japanese, even uploading my stupidities on YouTube.

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Testing the LMA solution with solar neutrinos independently of solar models

Cited by 21 publications

References 54 publications

Confronting mass-varying neutrinos with MiniBooNE

Confronting mass-varying neutrinos with MiniBooNE

sin2 θ W estimate and bounds on nonstandard interactions at source and detector in the solar neutrino low-energy regime

A Measurement of the muon neutrino charged current quasielastic interaction and a test of Lorentz violation with the MiniBooNE experiment

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