학술논문
Experimentally well-constrained masses of $^{27}$P and $^{27}$S: Implications for studies of explosive binary systems
Document Type
Working Paper
Author
Sun, L. J.; Xu, X. X.; Hou, S. Q.; Lin, C. J.; José, J.; Lee, J.; He, J. J.; Li, Z. H.; Wang, J. S.; Yuan, C. X.; Herwig, F.; Keegans, J.; Budner, T.; Wang, D. X.; Wu, H. Y.; Liang, P. F.; Yang, Y. Y.; Lam, Y. H.; Ma, P.; Duan, F. F.; Gao, Z. H.; Hu, Q.; Bai, Z.; Ma, J. B.; Wang, J. G.; Zhong, F. P.; Wu, C. G.; Luo, D. W.; Jiang, Y.; Liu, Y.; Hou, D. S.; Li, R.; Ma, N. R.; Ma, W. H.; Shi, G. Z.; Yu, G. M.; Patel, D.; Jin, S. Y.; Wang, Y. F.; Yu, Y. C.; Zhou, Q. W.; Wang, P.; Hu, L. Y.; Wang, X.; Zang, H. L.; Li, P. J.; Zhao, Q. Q.; Yang, L.; Wen, P. W.; Yang, F.; Jia, H. M.; Zhang, G. L.; Pan, M.; Wang, X. Y.; Sun, H. H.; Hu, Z. G.; Chen, R. F.; Liu, M. L.; Yang, W. Q.; Zhao, Y. M.; Zhang, H. Q.
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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.