Solar Neutrino Detection Sensitivity in DARWIN via Electron Scattering

2 Sep 2021, 17:10
50m
Talk in parallel session Neutrino physics and astrophysics Discussion Panel Neutrinos 8

Speaker

Shayne Reichard

Description

The proposed liquid xenon observatory DARWIN will exhibit sensitivity to solar neutrinos via elastic electron scattering. In this channel, DARWIN will have the potential to measure the fluxes of five solar neutrino components: $pp$, $^7$Be, $^{13}$N, $^{15}$O and $pep$. The precision of the $^{13}$N, $^{15}$O and $pep$ components is hindered by the double-beta decay of $^{136}$Xe and, thus, would benefit from a depleted target. A high-statistics observation of $pp$ neutrinos would allow for measurements of the electroweak mixing angle, $\sin^2\theta_w$, and the electron-type neutrino survival probability, $P_{ee}$, in the electron recoil energy region from a few keV up to 200 keV for the first time, with relative precision of 5% and 4%, respectively, with 10 live years of data and a 30 tonne fiducial volume. An observation of $pp$ and $^7$Be neutrinos would constrain the neutrino-inferred solar luminosity to 0.2%. A combination of all flux measurements would distinguish between the high- (GS98) and low-metallicity (AGS09) solar models with 2.1-2.5$\sigma$ significance, independent of external measurements from other experiments or a measurement of $^8$B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, it is demonstrated that with a depleted target DARWIN may be sensitive to the neutrino capture process of $^{131}$Xe.

Reference to paper (DOI or arXiv) 10.1140/epjc/s10052-020-08602-7

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