Absolute Determination of the 22Na(p,g) Reaction Rate in Novae

TL;DR

This study precisely measured key resonance strengths of the 22Na(p,g) reaction, significantly refining the reaction rate and predicting a reduced abundance of 22Na in nova ejecta, aiding gamma-ray detection efforts.

Contribution

It provides the first absolute measurements of resonance strengths in the 22Na(p,g) reaction, reducing uncertainties in nova nucleosynthesis models.

Findings

Resonance strengths at 213, 288, 454, and 610 keV are 2.4 to 3.2 times stronger than previous estimates.

Upper limits established for resonances at 198, 209, and 232 keV.

Predicted 22Na abundance in novae is reduced by factors of 1.5 to 2.

Abstract

Gamma-ray telescopes in orbit around the Earth are searching for evidence of the elusive radionuclide 22Na produced in novae. Previously published uncertainties in the dominant destructive reaction, 22Na(p,g)23Mg, indicated new measurements in the proton energy range of 150 to 300 keV were needed to constrain predictions. We have measured the resonance strengths, energies, and branches directly and absolutely by using protons from the University of Washington accelerator with a specially designed beamline, which included beam rastering and cold vacuum protection of the 22Na implanted targets. The targets, fabricated at TRIUMF-ISAC, displayed minimal degradation over a ~ 20 C bombardment as a result of protective layers. We avoided the need to know the stopping power, and hence the target composition, by extracting resonance strengths from excitation functions integrated over proton energy. Our measurements revealed that resonance strengths for E_p = 213, 288, 454, and 610 keV are stronger by factors of 2.4 to 3.2 than previously reported. Upper limits have been placed on proposed resonances at 198-, 209-, and 232-keV. We have re-evaluated the 22Na(p,g) reaction rate, and our measurements indicate the resonance at 213 keV makes the most significant contribution to 22Na destruction in novae. Hydrodynamic simulations including our rate indicate that the expected abundance of 22Na ejecta from a classical nova is reduced by factors between 1.5 and 2, depending on the mass of the white-dwarf star hosting the nova explosion.