Perturbing neutrino oscillations around the solar resonance
Abstract
Atmospheric neutrinos at low energies, $$E \lesssim 500$$ MeV, are known to be a rich source of information on lepton mixing parameters. We formulate a simple perturbative framework to elucidate the characteristic features of neutrino oscillation at around the solar-scale enhancement due to the matter effect. The clearest message that we could extract from our perturbation theory is that CP violation in the appearance oscillation probability is large, a factor of $$\sim 10$$ times larger than CP violation at around the atmospheric-scale oscillation maximum. The underlying mechanism for this is that one of the suppression factors on the CP phase-dependent terms due to the smallness of $$\Delta m^2_{21} / \Delta m^2_{31}$$ is dynamically lifted by the solar-scale enhancement. Our framework has a unique feature as a perturbation theory in which a large $$\Delta m^2_{31}$$ term outside the key 1-2 sector for the solar-scale resonance does not yield sizable corrections. On the contrary, the larger the $$\Delta m^2_{31}$$, the smaller the higher-order corrections.
- Authors:
-
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States). Theoretical Physics Dept.; Northwestern Univ., Evanston, IL (United States). Dept. of Physics and Astronomy; Colegio de Física Fundamental e Interdisciplinaria de las Américas (COFI), San Juan (Puerto Rico)
- Virginia Tech, Blacksburg, VA (United States). Dept. of Physics, Center for Neutrino Physics; Univ. of Tokyo, Kashiwa, Chiba (Japan). Inst. for Cosmic Ray Research, Research Center for Cosmic Neutrinos
- Publication Date:
- Research Org.:
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
- OSTI Identifier:
- 1545096
- Report Number(s):
- arXiv:1904.07853; FERMILAB-PUB-19-149-T; NUHEP-TH/19-05
Journal ID: ISSN 2050-3911; 1730033
- Grant/Contract Number:
- AC02-07CH11359
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Progress of Theoretical and Experimental Physics
- Additional Journal Information:
- Journal Volume: 2019; Journal Issue: 7; Journal ID: ISSN 2050-3911
- Publisher:
- Physical Society of Japan
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
Citation Formats
Martinez-Soler, Ivan, and Minakata, Hisakazu. Perturbing neutrino oscillations around the solar resonance. United States: N. p., 2019.
Web. doi:10.1093/ptep/ptz067.
Martinez-Soler, Ivan, & Minakata, Hisakazu. Perturbing neutrino oscillations around the solar resonance. United States. doi:10.1093/ptep/ptz067.
Martinez-Soler, Ivan, and Minakata, Hisakazu. Mon .
"Perturbing neutrino oscillations around the solar resonance". United States. doi:10.1093/ptep/ptz067. https://www.osti.gov/servlets/purl/1545096.
@article{osti_1545096,
title = {Perturbing neutrino oscillations around the solar resonance},
author = {Martinez-Soler, Ivan and Minakata, Hisakazu},
abstractNote = {Atmospheric neutrinos at low energies, $E \lesssim 500$ MeV, are known to be a rich source of information on lepton mixing parameters. We formulate a simple perturbative framework to elucidate the characteristic features of neutrino oscillation at around the solar-scale enhancement due to the matter effect. The clearest message that we could extract from our perturbation theory is that CP violation in the appearance oscillation probability is large, a factor of $\sim 10$ times larger than CP violation at around the atmospheric-scale oscillation maximum. The underlying mechanism for this is that one of the suppression factors on the CP phase-dependent terms due to the smallness of $\Delta m^2_{21} / \Delta m^2_{31}$ is dynamically lifted by the solar-scale enhancement. Our framework has a unique feature as a perturbation theory in which a large $\Delta m^2_{31}$ term outside the key 1-2 sector for the solar-scale resonance does not yield sizable corrections. On the contrary, the larger the $\Delta m^2_{31}$, the smaller the higher-order corrections.},
doi = {10.1093/ptep/ptz067},
journal = {Progress of Theoretical and Experimental Physics},
number = 7,
volume = 2019,
place = {United States},
year = {2019},
month = {7}
}
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Fig. 1: The bi-probability diagrams in $P$($ν$μ → $ν$e) − $P$($\bar{v}$μ → $\bar{v}$e) space are presented for the solar-scale enhanced region (large ellipses), $E$ = 0.1 GeV and $L$ = 2000 km, and for the NO$ν$A setting (small ellipses), $E$ = 2 GeV and $L$ = 810 km. The bluemore »
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