Big Bang Nucleosynthesis and the Helium Isotope Ratio

TL;DR

This paper proposes using combined measurements of primordial deuterium and helium isotope ratios to more reliably test for physics beyond the standard model during Big Bang Nucleosynthesis, highlighting current limitations and future observational strategies.

Contribution

It introduces a new method combining deuterium and helium isotope data to constrain the effective number of neutrino species, improving the reliability of BBN tests against systematic uncertainties.

Findings

Current Neff estimate supports the standard model.

Pre-solar helium isotope ratio uncertainty affects primordial value assumptions.

Future measurements could significantly tighten constraints on new physics.

Abstract

The conventional approach to search for departures from the standard model of physics during Big Bang Nucleosynthesis involves a careful, and subtle measurement of the mass fraction of baryons consisting of helium. Recent measurements of this quantity tentatively support new physics beyond the standard model but, historically, this method has suffered from hidden systematic uncertainties. In this letter, I show that a combined measurement of the primordial deuterium abundance and the primordial helium isotope ratio has the potential to provide a complementary and reliable probe of new physics beyond the standard model. Using the recent determination of the primordial deuterium abundance and assuming that the measured pre-solar 3He/4He meteoritic abundance reflects the primordial value, a bound can be placed on the effective number of neutrino species, Neff(BBN) = 3.01 (+0.95 -0.76, with 95 per cent confidence). Although this value of Neff supports the standard model, it is presently unclear if the pre-solar 3He/4He ratio reflects the primordial value. New astrophysical measurements of the helium isotope ratio in near-pristine environments, together with updated calculations and experimental values of several important nuclear reactions (some of which are already being attempted), will lead to much improved limits on possible departures from the standard model. To this end, I describe an analysis strategy to measure the 3He I flux emitted from nearby low metallicity H II regions. The proposed technique can be attempted with the next generation of large telescopes, and will be easier to realize in metal-poor H II regions with quiescent kinematics.