https://doi.org/10.1140/epjc/s10052-020-08602-7
Regular Article - Experimental Physics
Solar neutrino detection sensitivity in DARWIN via electron scattering
1
Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, 10691, Stockholm, SE, Sweden
2
Department of Physics and Astronomy, University of Bologna and INFN-Bologna, 40126, Bologna, Italy
3
LPNHE, Université Pierre et Marie Curie, Université Paris Diderot, CNRS/IN2P3, 75252, Paris, France
4
Institut für Physik & Exzellenzcluster PRISMA+, Johannes Gutenberg-Universität Mainz, 55099, Mainz, Germany
5
Institut für Kernphysik, Westfälische Wilhelms-Universität Münster, 48149, Münster, Germany
6
LIBPhys, Department of Physics, University of Coimbra, 3004-516, Coimbra, Portugal
7
Nikhef and the University of Amsterdam, Science Park, 1098XG, Amsterdam, The Netherlands
8
Vinca Institute of Nuclear Science, University of Belgrade, Mihajla Petrovica Alasa 12-14, Belgrade, Serbia
9
Physics Department, Columbia University, 10027, New York, NY, USA
10
Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 7610001, Rehovot, Israel
11
New York University Abu Dhabi, Abu Dhabi, United Arab Emirates
12
Institute for Data Processing and Electronics (IPE), Karlsruhe Institute of Technology (KIT), 76344, Eggenstein-Leopoldshafen, Germany
13
Physik-Institut, University of Zurich, 8057, Zurich, Switzerland
14
Physikalisches Institut, Universität Freiburg, 79104, Freiburg, Germany
15
Université Paris-Saclay, CNRS/IN2P3, IJCLab, 91405, Orsay, France
16
Department of Physics, Applied Physics and Astronomy, Rensselaer Polytechnic Institute, 12180, Troy, NY, USA
17
Max-Planck-Institut für Kernphysik, 69117, Heidelberg, Germany
18
Department of Physics and Astronomy, Purdue University, 47907, West Lafayette, IN, USA
19
Institute for Astroparticle Physics (IAP), Karlsruhe Institute of Technology (KIT), 76344, Eggenstein-Leopoldshafen, Germany
20
SUBATECH, IMT Atlantique, CNRS/IN2P3, Université de Nantes, 44307, Nantes, France
21
Institute of Experimental Particle Physics (ETP), Karlsruhe Institute of Technology (KIT), 76344, Eggenstein-Leopoldshafen, Germany
22
Department of Physics and Chemistry, University of L’Aquila, 67100, L’Aquila, Italy
23
INFN-Laboratori Nazionali del Gran Sasso and Gran Sasso Science Institute, 67100, L’Aquila, Italy
24
Physikalisches Institut, Ruprecht-Karls-Universität Heidelberg, Heidelberg, Germany
25
INFN-Laboratori Nazionali del Gran Sasso and Gran Sasso Science Institute, 67100, L’Aquila, Italy
26
Department of Physics and Kavli Institute for Cosmological Physics, University of Chicago, 60637, Chicago, IL, USA
27
Institute for Technical Physics (ITEP), Karlsruhe Institute of Technology (KIT), 76344, Eggenstein-Leopoldshafen, Germany
28
The Origins Project Foundation, 85020, Phoenix, AZ, USA
29
Department of Physics, University of California, 92093, San Diego, CA, USA
30
School of Physics, The University of Melbourne, 3010, Melbourne, VIC, Australia
31
Department of Physics, University of Alabama, 35487, Tuscaloosa, AL, USA
32
Department of Physics and Astronomy, Rice University, 77005, Houston, TX, USA
33
Department of Physics, Imperial Centre for Inference and Cosmology, Imperial College London, SW7 2AZ, London, UK
34
Institute for Nuclear and Particle Physics, TU Dresden, 01069, Dresden, Germany
Received:
5
June
2020
Accepted:
28
October
2020
Published online:
8
December
2020
We detail the sensitivity of the proposed liquid xenon DARWIN observatory to solar neutrinos via elastic electron scattering. We find that DARWIN will have the potential to measure the fluxes of five solar neutrino components: pp, Be,
N,
O and pep. The precision of the
N,
O and pep components is hindered by the double-beta decay of
Xe and, thus, would benefit from a depleted target. A high-statistics observation of pp neutrinos would allow us to infer the values of the electroweak mixing angle,
, and the electron-type neutrino survival probability,
, 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
Be neutrinos would constrain the neutrino-inferred solar luminosity down 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
significance, independent of external measurements from other experiments or a measurement of
B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, we demonstrate that with a depleted target DARWIN may be sensitive to the neutrino capture process of
Xe.
© The Author(s) 2020
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