Experimentally well-constrained masses of ${}^{27}$P and ${}^{27}$S: Implications for studies of explosive binary systems

Abstract

The mass of ${}^{27}$P was predicted to impact the X-ray burst (XRB) model predictions of burst light curves and the composition of the burst ashes. To address the uncertainties and inconsistencies in the reported ${}^{27}$P masses in literature, a wealth of information has been extracted from the $\beta$-decay spectroscopy of the drip-line nucleus ${}^{27}$S. We determine the most precise mass excess of ${}^{27}$P to date to be $-659(9)$~keV, which is 63~keV (2.3$\sigma$) higher than the AME2016 recommended value of $-722(26)$~keV. The experimentally unknown mass excess of ${}^{27}$S was estimated to be 17030(400)~keV in AME2016, and we constrain this mass to be 17678(77)~keV based on the measured $\beta$-delayed two-proton energy. In the temperature region of $(0.06-0.3)$~GK, the ${}^{26}$Si$(p,\gamma {)}^{27}$P reaction rate determined in this work is significantly lower than the rate recommended in the reaction rate libraries, up to two orders of magnitude around 0.1~GK. The impact of these newly determined masses and well-constrained rate on the modeling of the explosive astrophysical scenarios has been explored by hydrodynamic nova and post-processing XRB models. No substantial change was found in the nova contribution to the synthesis of galactic ${}^{26}$Al or in the XRB energy generation rate, but we found that the calculated abundances of ${}^{26}$Al and ${}^{26}$Si at the last stage of XRB are increased by a factor of 2.4. We also conclude that ${}^{27}$S is not a significant waiting point in the rapid proton capture process.

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• Recent progress in configuration-interaction shell model
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• Extension of the particle x-ray coincidence technique: The lifetimes and branching ratios apparatus
• Urca Nuclide Production in Type-I X-ray Bursts and Implications for Nuclear Physics Studies