Sensitivity to neutrinos from the solar CNO cycle in Borexino

Abstract

<jats:title>Abstract</jats:title><jats:p>Neutrinos emitted in the carbon, nitrogen, oxygen (CNO) fusion cycle in the Sun are a sub-dominant, yet crucial component of solar neutrinos whose flux has not been measured yet. The Borexino experiment at the Laboratori Nazionali del Gran Sasso (Italy) has a unique opportunity to detect them directly thanks to the detector’s radiopurity and the precise understanding of the detector backgrounds. We discuss the sensitivity of Borexino to CNO neutrinos, which is based on the strategies we adopted to constrain the rates of the two most relevant background sources, <jats:inline-formula><jats:alternatives><jats:tex-math>$$pep$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mi>pep</mml:mi> </mml:mrow> </mml:math></jats:alternatives></jats:inline-formula> neutrinos from the solar <jats:italic>pp</jats:italic>-chain and <jats:inline-formula><jats:alternatives><jats:tex-math>$$^{210}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mrow /> <mml:mn>210</mml:mn> </mml:msup> </mml:math></jats:alternatives></jats:inline-formula>Bi beta decays originating in the intrinsic contamination of the liquid scintillator with <jats:inline-formula><jats:alternatives><jats:tex-math>$$^{210}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mrow /> <mml:mn>210</mml:mn> </mml:msup> </mml:math></jats:alternatives></jats:inline-formula>Pb. Assuming the CNO flux predicted by the high-metallicity Standard Solar Model and an exposure of 1000 days <jats:inline-formula><jats:alternatives><jats:tex-math>$$\times $$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mo>×</mml:mo> </mml:math></jats:alternatives></jats:inline-formula> 71.3 t, Borexino has a median sensitivity to CNO neutrino higher than 3 <jats:inline-formula><jats:alternatives><jats:tex-math>$$\sigma $$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>σ</mml:mi> </mml:math></jats:alternatives></jats:inline-formula>. With the same hypothesis the expected experimental uncertainty on the CNO neutrino flux is 23%, provided the uncertainty on the independent estimate of the <jats:inline-formula><jats:alternatives><jats:tex-math>$$^{210}\text {Bi}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mn>210</mml:mn> </mml:msup> <mml:mtext>Bi</mml:mtext> </mml:mrow> </mml:math></jats:alternatives></jats:inline-formula> interaction rate is 1.5 <jats:inline-formula><jats:alternatives><jats:tex-math>$$\hbox {cpd}/100~\hbox {ton}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:mtext>cpd</mml:mtext> <mml:mo>/</mml:mo> <mml:mn>100</mml:mn> <mml:mspace /> <mml:mtext>ton</mml:mtext> </mml:mrow> </mml:math></jats:alternatives></jats:inline-formula> . Finally, we evaluated the expected uncertainty of the C and N abundances and the expected discrimination significance between the high and low metallicity Standard Solar Models (HZ and LZ) with future more precise measurement of the CNO solar neutrino flux.</jats:p>