<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>β</mml:mi></mml:mrow></mml:math>-decay of the neutron-rich nucleus<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">N</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>18</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>

Li, Z. H.; Ye, Y. L.; Hua, H.; Jiang, D. X.; Zhang, Y. M.; Fang, Xu; Hu, Qiang; Zhang, G. L.; Chen, Z. Q.; Zheng, Tao; Wu, Chengwen; Lou, J. L.; Li, X. Q.; Pang, Dan; Wang, S.; Li, Chen; Xu, H. S.; Sun, Zhi Yu; Duan, L.-M.; Hu, Zhiyun; Hu, R. J.; Xu, H. G.; Mao, Ruishi; Wang, Ying; Yuan, Xiaohui; Gao, Hong; Wu, L. J.; Huiquan, Qi; Huang, T. H.; Fu, Fang; Fu, Jia; Gao, Q.; Ding, Xilun; Han, J. L.; Zhang, X. Y.

doi:10.1103/physrevc.72.064327

Cited by 51 publications

(83 citation statements)

References 16 publications

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“…As an illustration of three-body force effects on the symmetry energy, we quote in the following results of a study [121] using the MDI energy density functional [43]. The latter has been used extensively in both simulating heavy-ion reactions [58,122,123] and studying properties of neutron stars [124,125,126,127,128,129]. It is developed from a modified Gogny-type interaction within the Hartree-Fock approach [43].…”

Section: The Role Of the Spin-isospin Dependence Of Three-body Forcesmentioning

confidence: 99%

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Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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Section: The Role Of the Spin-isospin Dependence Of Three-body Forcesmentioning

confidence: 99%

“…[380]. The rectangular region (solid black lines) of I ⋆ = [1.29 − 1.62] × 10 45 g cm 2 and R = [11.5 − 13.6] km represents the constraints on I and R from analyzing heavy ion collision data [122,123,124,125]. As explained in Ref.…”

Section: Symmetry Energy Effects On the Moment Of Inertia Of Slowly Rmentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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“…Nuclear symmetry energy E sym (ρ) and the equation of state (EOS) of pure neutron matter (PNM) E PNM (ρ) have profound impact on many important physics problems in nuclear physics and astrophysics [1][2][3][4][5] as well as some issues in new physics beyond the standard model [6][7][8][9][10]. For instance, the density dependence of the symmetry energy or neutron matter EOS at subsaturation densities is intimately related to the neutron skin thickness of finite nuclei [11][12][13][14][15][16][17][18][19][20][21][22][23], the properties of neutron star crust [23][24][25][26], the cluster formations in nuclear matter at low densities [27][28][29][30][31], and the isospin diffusion in heavy ion collisions at Fermi energies [32][33][34][35].…”

Section: Introductionmentioning

confidence: 99%

Pairing effects on neutron matter equation of state and symmetry energy at subsaturation densities

Zhang

Chen

2019

Phys. Rev. C

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Within the framework of BCS theory and Skyrme-Hartree-Fock model, we employ various microscopic pairing gaps and effective pairing interactions to study pairing effects on the equation of state (EOS) of neutron matter and the symmetry energy at subsaturation densities. We find pairing effects may have considerable contributions to the EOS of neutron matter at very low densities ( 0.02 fm −3 ), while only have a small impact on the symmetry energy at subsatruation densities. In addition, the reliability of the parabolic approximation for the isospin asymmetry dependence of nuclear matter EOS with pairing correlations included is also discussed. *

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“…After passing through the 25-μm kapton foil, which separated the vacuum of the beam line from the air, and a stack of aluminum degraders, the neutron-rich ions were finally transported into the target chamber filled with low-temperature nitrogen and implanted in a 1500-μm-thick double-side Si strip detector (DSSD) of 50 mm×50 mm. The experiment was performed in the continuous beam mode, which has a higher beam efficiency compared to the traditional beam-on/off mode [20,21]. By correlating the implanted nuclei with their subsequent β-particles within the same pixel or adjacent pixels of the DSSD, the β-decay properties of the implanted nuclei could be measured with much less disturbance from other unstable nuclei and the random background [22].…”

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confidence: 99%