| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $<3 \times 10^{-8}$ |
95 |
1 |
|
LASR |
| $<2.1 \times 10^{-12}$ |
90 |
2 |
|
TEXO |
| $<1.5 \times 10^{-12}$ |
90 |
3 |
|
|
| $<3.7 \times 10^{-12}$ |
90 |
4 |
|
RVUE |
| $<2 \times 10^{-14}$ |
|
5 |
|
ASTR |
| $<6 \times 10^{-14}$ |
|
6 |
|
ASTR |
| $<4 \times 10^{-4}$ |
|
7 |
|
RVUE |
| $<3 \times 10^{-4}$ |
|
8 |
|
RVUE |
| $<2 \times 10^{-15}$ |
|
9 |
|
ASTR |
| $<1 \times 10^{-13}$ |
|
10 |
|
ASTR |
|
1
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.
|
|
2
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.
|
|
3
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.
|
|
4
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.
|
|
5
This RAFFELT 1999 limit applies to all neutrino flavors which are light enough ($<5~$keV) to be emitted from globular-cluster red giants.
|
|
6
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.
|
|
7
BABU 1994 use COOPER-SARKAR 1992 limit on ${{\mathit \nu}}$ magnetic moment to derive quoted result. It applies to ${{\mathit \nu}_{{\tau}}}$.
|
|
8
DAVIDSON 1991 use data from early SLAC electron beam dump experiment to derive charge limit as a function of neutrino mass. It applies to ${{\mathit \nu}_{{\tau}}}$.
|
|
9
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$~{{\mathit \nu}_{{e}}}$.
|
|
10
The limit applies to all flavors.
|
