CN-Cycle Solar Neutrinos and Sun's Primordial Core Metalicity

TL;DR

This paper explores using solar neutrino measurements from the CN cycle and pp chain to determine the Sun's primordial core metal abundances of carbon and nitrogen, testing solar interior models and photospheric data.

Contribution

It proposes a novel method to measure the Sun's core C and N abundances using neutrino fluxes, reducing model dependence and improving understanding of solar composition.

Findings

Potential to measure core C and N at about 9% precision

Neutrino fluxes can be calibrated with existing experiments like Super-Kamiokande and SNO

The method offers a cross-check on photospheric abundance determinations.

Abstract

We argue that it may be possible to exploit neutrinos from the CN cycle and pp chain to determine the primordial solar core abundances of C and N at an interesting level of precision. Such a measurement would allow a comparison of the Sun's deep interior composition with it surface, testing a key assumption of the standard solar model (SSM), a homogeneous zero-age Sun. It would also provide a cross-check on recent photospheric abundance determinations that have altered the once excellent agreement between the SSM and helioseismology. As further motivation, we discuss a speculative possibility in which photospheric abundance/helioseismology puzzle is connected with the solar-system metal differentiation that accompanied formation of the gaseous giant planets. The theoretical relationship between core C and N and the 13N and 15O solar neutrino fluxes can be made more precise (and more general) by making use of the Super-Kamiokande and SNO 8B neutrino capture rates, which calibrate the temperature of the solar core. The primordial C and N abundances can then be obtained from these neutrino fluxes and from a product of nuclear rates, with little residual solar model dependence. We describe some of the recent experimental advances that could allow this comparison to be made (theoretically) at about the 9% level, and note that this uncertainty may be reduced further due to ongoing work on the S-factor for 14N(p,gamma). The envisioned measurement might be possible in deep, large-volume detectors using organic scintillator, e.g., Borexino or SNO+