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Suitable resolution for EOS tables in neutron star investigation
Houyuan Chen, Dehua Wen, Na Zhang
Published:   , doi: 10.1088/1674-1137/43/5/054108
Inasmuch as the hydrostatic structure of interior neutron stars uniquely depends on the equation of state (EOS), the inverse constraints on EOS from astrophysical observation have been important methods to reveal the properties of the high-density matter. Up to date, most of EOSs for neutron-star matter are given in tabulations, but these numeric tables could be quite different in resolution. To guarantee both the accuracy and efficiency in computing Tolman-Oppenheimer-Volkoff (TOV) equation, a concise standard for generating EOS tables with suitable resolution is investigated in this work. It is shown that the EOS tables with 50 points logarithmic-uniformly located at supra-nuclear density segment [\begin{document}$ \rho_{0}, 10 \rho_{0} $\end{document}], where \begin{document}$ \rho_{0} $\end{document} is the nuclear saturation density) would correspond to the interpolation-induced errors at ~0.02% for the gravitational mass \begin{document}$ M $\end{document} and ~0.2% for the tidal deformability \begin{document}$ \Lambda $\end{document}.
Spectral hardenings of cosmic ray protons and helium nuclei in supernova remnant shocks
Wen-Hui Lin, Bi-Wen Bao, Ze-Jun Jiang, Li Zhang
Published:   , doi: 10.1088/1674-1137/43/5/053103
Observed hardenings of spectra for cosmic ray protons and helium nuclei are studied in the frame of the model of non-linear diffusive shock acceleration of supernova remnants (SNRs). In this model, the injected particles with energies below the spectral " knee” are assumed to be described by two populations with different spectral indexes around 200 GeV: the high-energy population is dominated by the particles with energies above 200 GeV released upstream of the shock of SNR, and the low-energy population is attributed to the particles with energies below 200 GeV released downstream of the shock of SNR. In this case, the spectral hardenings of cosmic ray protons and helium nuclei observed by PAMELA, AMS-02, and CREAM experiments can be reproduced.
Possibilities for synthesis of new neutron deficient isotopes of superheavy nuclei
Xiao-Jun Bao
Published:   , doi: 10.1088/1674-1137/43/5/054105
In order to search the optimal projectile-target combination to produce new neutron deficient isotopes of superheavy nuclei (SHN), the dependence of the evaporation residue cross section (ERCS) to synthesize SHN on the mass asymmetry and the isospin of colliding nuclei are analysed within the dinuclear system (DNS) concept. Predicted ERCSs for the production of new neutron deficient isotopes of SHN were found to be quite large with 36S projectile, and it is found that the production cross sections of SHN decrease slowly with the charged numbers of compound nuclei due to the increases in survival probability which \begin{document}$ W_{{\rm sur}} $\end{document} are not canceled by the decreasing \begin{document}$ P_{{\rm CN}} $\end{document}.
Quark-antiquark scattering phase shift and meson spectral function in pion superfluid
Tao Xia, Jin Hu, Shijun Mao
Published:   , doi: 10.1088/1674-1137/43/5/054103
We study the quark-antiquark scattering phase shift and meson spectral function in the pion superfluid described by the Nambu-Jona-Lasinio model. The meson mixing in the pion superfluid changes dramatically the full scattering phase shift and broadens strongly the spectral function of some of the collective modes.
The monopole effects, core excitations and ${\beta}$ decay in the A=130 hole nuclei near 132Sn
Han-Kui Wang, Zhi-Hong Li, Cen-Xi Yuan, Zhi-Qiang Chen, Ning Wang, Wei Qin, Yi-Qi He
Published:   , doi: 10.1088/1674-1137/43/5/054101
The proton and neutron cross-shell excitations across the Z=50 shell are investigated in the southwest quadrant of 132Sn by large-scale shell-model calculations with the extended pairing plus multipole-multipole force. The model space allows proton (neutron) core excitations, and both the low-lying and the high-energy states for 130In are wholly well described by comparison with the experimental data. The monopole effects between proton orbit \begin{document}$ g_{9/2} $\end{document} and neutron orbit \begin{document}$ g_{7/2} $\end{document} are studied as the new monopole correction that reproduces the first 1+ level in 130In perfectly. The energy interval of proton (neutron) core excitations in 130In lies in the energy of 4.5−6.5 (2.0−4.1) MeV, and the high energy yrast states are predicted as neutron core excitations. The \begin{document}$ \beta $\end{document} decays are calculated among the A=130 nuclei of 130In, 130Sn and 130Cd.