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Updated: Mar 23, 2026

Atomic Scale Structural Studies of Macromolecular Assemblies by Solid-state Nuclear Magnetic Resonance Spectroscopy
Published on: September 17, 2017
Isospin Mixing Reveals ^{30}P(p,γ)^{31}S Resonance Influencing Nova Nucleosynthesis
M B Bennett1,2,3, C Wrede1,2, B A Brown1,2
1Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
The rate of the ^{30}P(p,γ)^{31}S reaction, crucial for nova nucleosynthesis, is now constrained. A key resonance state in ^{31}S was identified, improving models of stellar evolution and presolar grains.
Area of Science:
- Nuclear astrophysics
- Stellar nucleosynthesis
- Nova astrophysics
Background:
- The ^{30}P(p,γ)^{31}S reaction rate is vital for understanding ONe nova nucleosynthesis.
- Accurate modeling requires knowledge of ^{31}S proton capture resonance states, which are currently unconstrained due to spin and parity uncertainties.
Purpose of the Study:
- To experimentally determine the properties of key resonance states in ^{31}S.
- To improve the accuracy of the ^{30}P(p,γ)^{31}S reaction rate for nova models.
Main Methods:
- Utilized the beta decay of ^{31}Cl to observe beta-delayed gamma decay.
- Identified a ^{31}S state at E_{x}=6390.2(7) keV, corresponding to a resonance energy E_{r}=259.3(8) keV.
Main Results:
- Observed a ^{31}S state within the Gamow window for nova temperatures.
- Determined an unambiguous spin and parity of 3/2^{+} for this state through isospin mixing with the isobaric analog state.
Conclusions:
- The identified 3/2^{+} resonance is crucial for constraining the ^{30}P(p,γ)^{31}S reaction rate.
- This finding will enhance the calibration of nova thermometers and the identification of presolar nova grains.
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