Constraints on neutrino nonstandard interactions from COHERENT, PandaX-4T and XENONnT

We investigate constraints on neutrino nonstandard interactions (NSIs) in the effective field theory framework, using data from the first measurement of solar <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mrow><a:mmultiscripts><a:mrow><a:mi mathvariant="normal">B</a:mi></a:mrow><a:mprescripts/><a:none/><a:mrow><a:mn>8</a:mn></a:mrow></a:mmultiscripts></a:mrow></a:math> neutrinos via coherent elastic neutrino-nucleus scattering (<d:math xmlns:d="http://www.w3.org/1998/Math/MathML" display="inline"><d:mrow><d:mi>CE</d:mi><d:mi>ν</d:mi><d:mi>NS</d:mi></d:mrow></d:math>) in the PandaX-4T and XENONnT experiments and data from the COHERENT experiment. The impacts of neutrino NSIs on the <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mrow><f:mi>CE</f:mi><f:mi>ν</f:mi><f:mi>NS</f:mi></f:mrow></f:math> cross section and the matter effect in the propagation of solar neutrinos are included, while we obtain that the expected number of <h:math xmlns:h="http://www.w3.org/1998/Math/MathML" display="inline"><h:mrow><h:mi>CE</h:mi><h:mi>ν</h:mi><h:mi>NS</h:mi></h:mrow></h:math> events is more sensitive to neutrino NSIs appearing in the cross section. Due to relatively large statistical uncertainties, the sensitivities of the PandaX-4T and XENONnT experiments to the neutrino NSIs are currently limited, compared to the COHERENT experiment. Besides, we find that since the central value of the measured <j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"><j:mrow><j:mi>CE</j:mi><j:mi>ν</j:mi><j:mi>NS</j:mi></j:mrow></j:math> counts significantly differs from the Standard Model prediction, the sensitivity of PandaX-4T experiment is even more restricted compared to XENONnT. However, the measurements of PandaX-4T and XENONnT are uniquely sensitive to the neutrino NSIs for the <l:math xmlns:l="http://www.w3.org/1998/Math/MathML" display="inline"><l:mi>τ</l:mi></l:math> flavor due to oscillation feature of the solar <n:math xmlns:n="http://www.w3.org/1998/Math/MathML" display="inline"><n:mrow><n:mmultiscripts><n:mrow><n:mi mathvariant="normal">B</n:mi></n:mrow><n:mprescripts/><n:none/><n:mrow><n:mn>8</n:mn></n:mrow></n:mmultiscripts></n:mrow></n:math> neutrinos. We also assess how the experimental central value, exposure, and systematic uncertainties will affect the constraints on neutrino NSIs from various <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:mrow><q:mi>CE</q:mi><q:mi>ν</q:mi><q:mi>NS</q:mi></q:mrow></q:math> measurements in the future.