M. B. Bennett

Classical-NOVA CONTRIBUTION to the Milky Way's ²⁶Al abundance: exit channel of the key ²⁵Al(p,γ) ²⁶Si resonance.

Classical novae are expected to contribute to the 1809-keV Galactic γ-ray emission by producing its precursor 26Al, but the yield depends on the thermonuclear rate of the unmeasured 25Al(p,γ)26Si reaction. Using the β decay of 26P to populate the key J(π)=3(+) resonance in this reaction, we report the first evidence for the observation of its exit channel via a 1741.6±0.6(stat)±0.3(syst)  keV primary γ ray, where the uncertainties are statistical and systematic, respectively. By combining the measured γ-ray energy and intensity with other experimental data on 26Si, we find the center-of-mass energy and strength of the resonance to be E(r)=414.9±0.6(stat)±0.3(syst)±0.6(lit.)  keV and ωγ=23±6(stat)(-10)(+11)(lit.)  meV, respectively, where the last uncertainties are from adopted literature data. We use hydrodynamic nova simulations to model 26Al production showing that these measurements effectively eliminate the dominant experimental nuclear-physics uncertainty and we estimate that novae may contribute up to 30% of the Galactic 26Al.

Revalidation of the isobaric multiplet mass equation for the A = 20 quintet

An unexpected breakdown of the isobaric multiplet mass equation in the A = 20, T = 2 quintet was recently reported, presenting a challenge to modern theories of nuclear structure. In the present work, the excitation energy of the lowest T = 2 state in Na-20 has been measured to be 6498.4 +/- 0.2stat ± 0.4syst keV by using the superallowed 0+ → 0+ beta decay of Mg-20 to access it and an array of high-purity germanium detectors to detect its gamma-ray deexcitation. This value differs by 27 keV (1.9 standard deviations) from the recommended value of 6525 ± 14 keV and is a factor of 28 more precise. The isobaric multiplet mass equation is shown to be revalidated when the new value is adopted.

Isobaric multiplet mass equation in the A = 31 , T = 3 / 2 quartets

The observed mass excesses of analog nuclear states with the same mass number

Beta-delayed gamma decay of 26P: Possible evidence of a proton halo

A

Isospin Mixing Reveals P 30 (p,γ) S 31 Resonance Influencing Nova Nucleosynthesis

and isospin

Confirmation of the isomeric state in P 26

T

Observation of Doppler broadening in β -delayed proton- γ decay

can be used to test the isobaric multiplet mass equation (IMME), which has, in most cases, been validated to a high degree of precision. A recent measurement [Kankainen et al., Phys. Rev. C 93 041304(R) (2016)] of the ground-state mass of

Isospin mixing reveals 30P(p, γ)31S resonance influencing nova nucleosynthesis

^{31}

Observation of Doppler broadening inβ-delayed proton-γdecay

Cl led to a substantial breakdown of the IMME for the lowest

Observation of Doppler broadening in

A = 31, T = 3/2