${{\mathit \nu}}$ CHARGE

INSPIRE   PDGID:
S066CHR
$\mathit e$ = electron charge is the unit of values listed below.
VALUE ($\mathit e$) CL% DOCUMENT ID TECN  COMMENT
$\bf{<4 \times 10^{-35}}$ 95 1
CAPRINI
2005
COSM charge neutral universe
• • We do not use the following data for averages, fits, limits, etc. • •
$<2.24 \times 10^{-13}$ 90 2
AALBERS
2023A
 LZ Solar ${{\mathit \nu}}$ spectrum
$<1.5 \times 10^{-13}$ 90 3
ATZORI-CORONA
2023
FIT solar neutrinos
$<3.3 \times 10^{-12}$ 90 4
BONET
2022A
 CONU nuclear reactor
$<5.4 \times 10^{-12}$ 90 5
ABE
2020E
 XMAS solar neutrinos
$1.7 - 2.3 \times 10^{-12}$ 68 6
KHAN
2020
spectral fit of XENON1T
$<3 \times 10^{-8}$ 95 7
DELLA-VALLE
2016
LASR magnetic dichroism
$<2.1 \times 10^{-12}$ 90 8
CHEN
2014A
 TEXO nuclear reactor
$<1.5 \times 10^{-12}$ 90 9
STUDENIKIN
2014
nuclear reactor
$<3.7 \times 10^{-12}$ 90 10
GNINENKO
2007
RVUE nuclear reactor
$<2 \times 10^{-14}$ 11
RAFFELT
1999
ASTR red giant luminosity
$<6 \times 10^{-14}$ 12
RAFFELT
1999
ASTR solar cooling
$<4 \times 10^{-4}$ 13
BABU
1994
RVUE BEBC beam dump
$<3 \times 10^{-4}$ 14
DAVIDSON
1991
RVUE SLAC ${{\mathit e}^{-}}$ beam dump
$<2 \times 10^{-15}$ 15
BARBIELLINI
1987
ASTR SN 1987A
$<1 \times 10^{-13}$ 16
BERNSTEIN
1963
ASTR solar energy losses
1  CAPRINI 2005 limit derived from the lack of a charge asymmetry in the universe. Limit assumes that charge asymmetries between particles are not anti-correlated.
2  AALBERS 2023A utilize the first 60 days of data collected by the LZ dark matter search to place a limit on the electric charge of solar neutrinos. Low energy electron-recoil events are utilized. This LZ-collaboration analysis supersedes that of the external authors in ATZORI-CORONA 2023 because of a more complete treatment of experiment uncertainties.
3  ATZORI-CORONA 2023 use LUX-ZEPLIN dark matter search data published by AALBERS 2023 to place a limit on neutrino millicharge.
4  BONET 2022A use data collected by four low-threshold ${}^{}\mathrm {Ge}$ detectors, placed 17.1 m from one of the cores of the nuclear reactors at Brokdorf to derive this limit. A spectral analysis is performed on reactor on and off data.
5  ABE 2020E obtains this result by assuming that the low-energy excess events in the XMASS detector are produced by neutrino millicharge which is common for all three neutrino flavors.
6  KHAN 2020 performed a constrained spectral fit analysis of the excess observed in the electron recoil energy spectrum by the XENON1T experiment. This range of neutrino millicharge values is one of the possible interpretations of these excess events. For the individual flavor constraints at 90$\%$ C.L. see the original reference.
7  DELLA-VALLE 2016 obtain a limit on the charge of neutrinos valid for masses of less than 10 meV. For heavier neutrinos the limit increases as a power of mass, reaching $10^{-6}$ $\mathit e$ for $\mathit m$ = 100 meV.
8  CHEN 2014A use the Multi-Configuration RRPA method to analyze reactor ${{\overline{\mathit \nu}}_{{{e}}}}$ scattering on ${}^{}\mathrm {Ge}$ atoms with 300 eV recoil energy threshold to obtain this limit.
9  STUDENIKIN 2014 uses the limit on ${{\mathit \mu}_{{{\nu}}}}$ from BEDA 2013 and the 2.8 keV threshold of the electron recoil energy to obtain this limit.
10  GNINENKO 2007 use limit on ${{\overline{\mathit \nu}}_{{{e}}}}$ magnetic moment from LI 2003B to derive this result. The limit is considerably weaker than the limits on the charge of ${{\mathit \nu}_{{{e}}}}$ and ${{\overline{\mathit \nu}}_{{{e}}}}$ from various astrophysics considerations.
11  This RAFFELT 1999 limit applies to all neutrino flavors which are light enough ($<5~$keV) to be emitted from globular-cluster red giants.
12  This RAFFELT 1999 limit is derived from the helioseismological limit on a new energy-loss channel of the Sun, and applies to all neutrino flavors which are light enough ($<1~$keV) to be emitted from the sun.
13  BABU 1994 use COOPER-SARKAR 1992 limit on ${{\mathit \nu}}$ magnetic moment to derive quoted result. It applies to ${{\mathit \nu}_{{{\tau}}}}$.
14  DAVIDSON 1991 use data from early SLAC electron beam dump experiment to derive charge limit as a function of neutrino mass. It applies to ${{\mathit \nu}_{{{\tau}}}}$.
15  Exact BARBIELLINI 1987 limit depends on assumptions about the intergalactic or galactic magnetic fields and about the direct distance and time through the field. It applies to$~{{\mathit \nu}_{{{e}}}}$.
16  The limit applies to all flavors.
Conservation Laws:
ELECTRIC CHARGE ($\mathit Q$)
References