| $\bf{<1 \times 10^{-21}}$ |
1 |
|
| • • • We do not use the following data for averages, fits, limits, etc. • • • |
| $<3.2 \times 10^{-20}$ |
2 |
|
| $<0.8 \times 10^{-21}$ |
|
|
| $<1.0 \times 10^{-21}$ |
1 |
|
|
1
BRESSI 2011 uses the method of DYLLA 1973 but finds serious errors in that experiment that greatly reduce its accuracy. The BRESSI 2011 limit assumes that ${{\mathit n}}$ $\rightarrow$ ${{\mathit p}}{{\mathit e}^{-}}{{\mathit \nu}_{{e}}}$ conserves charge. Thus the limit applies equally to the charge of the neutron.
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2
SENGUPTA 2000 uses the difference between the observed rate of of rotational energy loss by the binary pulsar PSR B1913+16 and the rate predicted by general relativity to set this limit. See the paper for assumptions.
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