2019 Vol. 43, No. 7
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2019, 43(7): 073101. doi: 10.1088/1674-1137/43/7/073101
Abstract:
The diphoton invariant mass distribution from the interference between\begin{document}$gg\to H \to \gamma\gamma$\end{document} ![]()
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\begin{document}$gg\to \gamma\gamma$\end{document} ![]()
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\begin{document}$M_H$\end{document} ![]()
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\begin{document}$A_{\rm{int}}$\end{document} ![]()
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\begin{document}$M_H$\end{document} ![]()
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\begin{document}$\int^{M_H}_{M_H-5~\rm{GeV}} -\int_{M_H}^{M_H+5~\rm{GeV}}$\end{document} ![]()
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\begin{document}$A_{\rm{int}}$\end{document} ![]()
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\begin{document}$H\gamma\gamma$\end{document} ![]()
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\begin{document}$A_{\rm{int}}$\end{document} ![]()
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\begin{document}$H\gamma\gamma$\end{document} ![]()
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\begin{document}$A_{\rm{int}}$\end{document} ![]()
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\begin{document}$A_{\rm{int}}$\end{document} ![]()
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\begin{document}$H\gamma\gamma$\end{document} ![]()
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\begin{document}$Hgg$\end{document} ![]()
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The diphoton invariant mass distribution from the interference between
2019, 43(7): 073102. doi: 10.1088/1674-1137/43/7/073102
Abstract:
The doubly weak transition\begin{document}$b\to dd{\bar s}$\end{document} ![]()
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\begin{document}$\smash{\overline B}^0\to K^+\pi^-$\end{document} ![]()
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\begin{document}$\smash{\overline B}^0\to K^+\pi^-$\end{document} ![]()
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The doubly weak transition
2019, 43(7): 073103. doi: 10.1088/1674-1137/43/7/073103
Abstract:
\begin{document}$\bar B_s^0\to (D^0,\bar D^0) \pi^+\pi^-$\end{document} ![]()
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\begin{document}$b\to c \bar us$\end{document} ![]()
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\begin{document}$b \to u\bar cs$\end{document} ![]()
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\begin{document}$D_{\rm CP}$\end{document} ![]()
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\begin{document}$\gamma$\end{document} ![]()
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\begin{document}$\pi^+\pi^-$\end{document} ![]()
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\begin{document}$f_0(500)$\end{document} ![]()
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\begin{document}$f_0(980),f_0(1500),f_0(1790)$\end{document} ![]()
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\begin{document}$\bar B_s^0\to (D^0,\bar D^0) (\pi^+\pi^-)_S$\end{document} ![]()
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\begin{document}$10^{-6}$\end{document} ![]()
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\begin{document}$\bar B_s^0\to D_{\rm CP} (\pi^+\pi^-)_S$\end{document} ![]()
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\begin{document}$\gamma$\end{document} ![]()
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2019, 43(7): 074101. doi: 10.1088/1674-1137/43/7/074101
Abstract:
The chiral order-parameter σ field and its higher-order cumulants of fluctuations are calculated within the functional renormalization group approach by adopting the local potential approximation in this study. The influence of glue dynamics on fluctuations of the σ field is investigated, and we find that they are weakly affected. This is in sharp contrast to the baryon number fluctuations, which are sensitive to the glue dynamics and involve information on the color confinement. The implications of our calculated results are discussed from the viewpoint of the theoretical and experimental efforts in the search for the QCD critical end point.
The chiral order-parameter σ field and its higher-order cumulants of fluctuations are calculated within the functional renormalization group approach by adopting the local potential approximation in this study. The influence of glue dynamics on fluctuations of the σ field is investigated, and we find that they are weakly affected. This is in sharp contrast to the baryon number fluctuations, which are sensitive to the glue dynamics and involve information on the color confinement. The implications of our calculated results are discussed from the viewpoint of the theoretical and experimental efforts in the search for the QCD critical end point.
2019, 43(7): 074102. doi: 10.1088/1674-1137/43/7/074102
Abstract:
Spontaneous fission (SF) with a new formula based on a liquid drop model is proposed and used in the calculation of the SF half-lives of heavy and superheavy nuclei (Z = 90–120). The predicted half-lives are in agreement with the experimental SF half-lives. The half-lives of\begin{document}$ \alpha $\end{document} ![]()
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Spontaneous fission (SF) with a new formula based on a liquid drop model is proposed and used in the calculation of the SF half-lives of heavy and superheavy nuclei (Z = 90–120). The predicted half-lives are in agreement with the experimental SF half-lives. The half-lives of
2019, 43(7): 074103. doi: 10.1088/1674-1137/43/7/074103
Abstract:
The cross sections for 59, 60Ca, recently measured in the 345 A MeV\begin{document}$^{70}{\rm{Zn}}+^{9}{\rm{Be}}$\end{document} ![]()
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\begin{document}$^{66, 70}{\rm{Ca}}$\end{document} ![]()
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\begin{document}$^{70, 80}{\rm{Zn}}+^{9}{\rm{Be}}$\end{document} ![]()
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\begin{document}$^{66, 70}{\rm{Ca}}$\end{document} ![]()
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\begin{document}$^{80}{\rm{Zn}}+^{9}{\rm{Be}}$\end{document} ![]()
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\begin{document}$^{66, 70}{\rm{Ca}}$\end{document} ![]()
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The cross sections for 59, 60Ca, recently measured in the 345 A MeV
2019, 43(7): 074104. doi: 10.1088/1674-1137/43/7/074104
Abstract:
The radial basis function (RBF) approach is a powerful tool to improve nuclear mass predictions. By combining the RBF approach with the latest relativistic continuum Hartree-Bogoliubov (RCHB) model, the local systematic deviations between the RCHB mass predictions and the experimental data are eliminated, and the root-mean-square (rms) mass deviation is significantly reduced from 7.923 MeV to 0.386 MeV. However, systematic deviations between the RBF improved mass predictions and the experimental data remain for nuclei with four different odd-even parities, i.e. (even Z, even N), (even Z, odd N), (odd Z, even N), and (odd Z, odd N). They can be reduced by separately training RBF for the four groups of nuclei, and the resulting rms deviation decreases to 0.229 MeV. It is found that the RBF approach can describe the deformation effects neglected in the present RCHB mass calculations, and also improves the description of the shell effect and the pairing effect.
The radial basis function (RBF) approach is a powerful tool to improve nuclear mass predictions. By combining the RBF approach with the latest relativistic continuum Hartree-Bogoliubov (RCHB) model, the local systematic deviations between the RCHB mass predictions and the experimental data are eliminated, and the root-mean-square (rms) mass deviation is significantly reduced from 7.923 MeV to 0.386 MeV. However, systematic deviations between the RBF improved mass predictions and the experimental data remain for nuclei with four different odd-even parities, i.e. (even Z, even N), (even Z, odd N), (odd Z, even N), and (odd Z, odd N). They can be reduced by separately training RBF for the four groups of nuclei, and the resulting rms deviation decreases to 0.229 MeV. It is found that the RBF approach can describe the deformation effects neglected in the present RCHB mass calculations, and also improves the description of the shell effect and the pairing effect.
2019, 43(7): 074105. doi: 10.1088/1674-1137/43/7/074105
Abstract:
We investigate the squeezed back-to-back correlations (BBC) of\begin{document}$ K^+ $\end{document} ![]()
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\begin{document}$ K^- $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 200 $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 62.4 $\end{document} ![]()
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\begin{document}$ K^+ $\end{document} ![]()
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\begin{document}$ K^- $\end{document} ![]()
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\begin{document}$ K^+ $\end{document} ![]()
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\begin{document}$ K^- $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 200 $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 62.4 $\end{document} ![]()
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\begin{document}$ K^+ $\end{document} ![]()
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\begin{document}$ K^- $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 200 $\end{document} ![]()
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\begin{document}$ \sqrt{s_{NN}} = 62.4 $\end{document} ![]()
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We investigate the squeezed back-to-back correlations (BBC) of
2019, 43(7): 074106. doi: 10.1088/1674-1137/43/7/074106
Abstract:
The competition of isovector and isoscalar pairing in A=18 and 20 even-even N≈Z nuclei is analyzed in the framework of the mean-field plus the dynamic quadurpole-quadurpole, pairing and particle-hole interactions, whose Hamiltonian is diagonalized in the basis\begin{document}${ U}(24) \supset ({ U}(6)\supset {{SU}}(3)\supset {{SO}}(3)) \otimes ({ U}(4)\supset{ {SU}}_S(2)\otimes {{SU}}_T(2)) $\end{document} ![]()
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The competition of isovector and isoscalar pairing in A=18 and 20 even-even N≈Z nuclei is analyzed in the framework of the mean-field plus the dynamic quadurpole-quadurpole, pairing and particle-hole interactions, whose Hamiltonian is diagonalized in the basis
2019, 43(7): 074107. doi: 10.1088/1674-1137/43/7/074107
Abstract:
The restoration of pseudo-spin symmetry (PSS) along the\begin{document}$ N = 32 $\end{document} ![]()
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\begin{document}$ N =34 $\end{document} ![]()
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\begin{document}$ (\pi2s_{1/2},\pi1d_{3/2}) $\end{document} ![]()
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The restoration of pseudo-spin symmetry (PSS) along the
2019, 43(7): 075001. doi: 10.1088/1674-1137/43/7/075001
Abstract:
The Large High Altitude Air Shower Observatory (LHAASO) is a composite cosmic ray observatory consisting of three detector arrays: kilometer square array (KM2A), which includes the electromagnetic detector array and muon detector array, water Cherenkov detector array (WCDA) and wide field-of-view Cherenkov telescope array (WFCTA). One of the main scientific objectives of LHAASO is to precisely measure the cosmic rays energy spectrum of individual components from\begin{document}$ 10^{14} $\end{document} ![]()
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\begin{document}$ 10^{18} $\end{document} ![]()
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\begin{document}$ 900 \rm\ m^{2}Sr $\end{document} ![]()
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\begin{document}$ 1800 \rm\ m^{2}Sr $\end{document} ![]()
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The Large High Altitude Air Shower Observatory (LHAASO) is a composite cosmic ray observatory consisting of three detector arrays: kilometer square array (KM2A), which includes the electromagnetic detector array and muon detector array, water Cherenkov detector array (WCDA) and wide field-of-view Cherenkov telescope array (WFCTA). One of the main scientific objectives of LHAASO is to precisely measure the cosmic rays energy spectrum of individual components from
2019, 43(7): 075002. doi: 10.1088/1674-1137/43/7/075002
Abstract:
The muonic component of the extensive air showers (EAS) is of great importance for the astroparticle physics. It carries the information about the properties of primary cosmic ray (CR) particles, such as their mass, and electromagnetic and hadronic nature. It provides a sensitive test for the hadronic interaction models, which are inevitable for describing the cascade shower development of cosmic rays in EAS experiments. The YangBaJing Hybrid Array (YBJ-HA) experiment has been in operation since the end of 2016. Surface detectors are used for the measurements of primary energy, angular direction and core position of a shower event, while underground muon detectors are used for measuring the density of muons at various locations. Using the data obtained by the YBJ-HA experiment, this work reports the first measurement of the lateral muon distribution for the primary cosmic ray energy in the 100 TeV region. The punch-through effect is evaluated via MC simulation.
The muonic component of the extensive air showers (EAS) is of great importance for the astroparticle physics. It carries the information about the properties of primary cosmic ray (CR) particles, such as their mass, and electromagnetic and hadronic nature. It provides a sensitive test for the hadronic interaction models, which are inevitable for describing the cascade shower development of cosmic rays in EAS experiments. The YangBaJing Hybrid Array (YBJ-HA) experiment has been in operation since the end of 2016. Surface detectors are used for the measurements of primary energy, angular direction and core position of a shower event, while underground muon detectors are used for measuring the density of muons at various locations. Using the data obtained by the YBJ-HA experiment, this work reports the first measurement of the lateral muon distribution for the primary cosmic ray energy in the 100 TeV region. The punch-through effect is evaluated via MC simulation.
2019, 43(7): 075101. doi: 10.1088/1674-1137/43/7/075101
Abstract:
The equation of state (EoS) of dark energy plays an important role in the evolution of the universe and has attracted considerable interest in the recent years. With the progress in observational technique, a precise constraint on the EoS of dark energy can be obtained. In this study, we reconstruct the EoS of dark energy and cosmic expansion using Gaussian processes (GP) from the most up-to-date Pantheon compilation of type Ia supernovae (SNe Ia), which consists of 1048 finely calibrated SNe Ia. The reconstructed EoS of dark energy has a large uncertainty owing to its dependence on the second-order derivative of the construction. Adding the direct measurements of Hubble parameters\begin{document}$H(z)$\end{document} ![]()
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\begin{document}$H_0$\end{document} ![]()
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\begin{document}$H_0$\end{document} ![]()
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\begin{document}$H(z)$\end{document} ![]()
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\begin{document}$H_0=70.5\pm 0.5~{\rm km~s^{-1}~Mpc^{-1}}$\end{document} ![]()
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\begin{document}$\Omega_M$\end{document} ![]()
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\begin{document}$H_0$\end{document} ![]()
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\begin{document}$\Omega_M$\end{document} ![]()
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The equation of state (EoS) of dark energy plays an important role in the evolution of the universe and has attracted considerable interest in the recent years. With the progress in observational technique, a precise constraint on the EoS of dark energy can be obtained. In this study, we reconstruct the EoS of dark energy and cosmic expansion using Gaussian processes (GP) from the most up-to-date Pantheon compilation of type Ia supernovae (SNe Ia), which consists of 1048 finely calibrated SNe Ia. The reconstructed EoS of dark energy has a large uncertainty owing to its dependence on the second-order derivative of the construction. Adding the direct measurements of Hubble parameters
2019, 43(7): 075102. doi: 10.1088/1674-1137/43/7/075102
Abstract:
The observation of GW150914 gave a new independent measurement of the luminosity distance of a gravitational wave event. In this paper, we constrain the anisotropy of the Universe by using gravitational wave events. We simulate hundreds of events of binary neutron star merger that may be observed by the Einstein Telescope. Full simulation of the production process of gravitational wave data is employed. We find that 200 binary neutron star merging events with the redshift in (0,1) observed by the Einstein Telescope may constrain the anisotropy with an accuracy comparable to that from the Union2.1 supernovae. This result shows that gravitational waves can be a powerful tool for investigating cosmological anisotropy.
The observation of GW150914 gave a new independent measurement of the luminosity distance of a gravitational wave event. In this paper, we constrain the anisotropy of the Universe by using gravitational wave events. We simulate hundreds of events of binary neutron star merger that may be observed by the Einstein Telescope. Full simulation of the production process of gravitational wave data is employed. We find that 200 binary neutron star merging events with the redshift in (0,1) observed by the Einstein Telescope may constrain the anisotropy with an accuracy comparable to that from the Union2.1 supernovae. This result shows that gravitational waves can be a powerful tool for investigating cosmological anisotropy.
2019, 43(7): 075103. doi: 10.1088/1674-1137/43/7/075103
Abstract:
We investigate primordial perturbations and non-gaussianities in the Hořava-Lifshitz theory of gravitation. In the UV limit, the scalar perturbation in the Hořava theory is naturally scale-invariant, ignoring the details of the expansion of the Universe. One may thus relax the exponential inflation and the slow-roll conditions for the inflaton field. As a result, it is possible that the primordial non-gaussianities, which are " slow-roll suppressed” in the standard scenarios, become large. We calculate the non-gaussianities from the bispectrum of the perturbation and find that the equilateral-type non-gaussianity is of the order of unity, while the local-type non-gaussianity remains small, as in the usual single-field slow-roll inflation model in general relativity. Our result is a new constraint on Hořava-Lifshitz gravity.
We investigate primordial perturbations and non-gaussianities in the Hořava-Lifshitz theory of gravitation. In the UV limit, the scalar perturbation in the Hořava theory is naturally scale-invariant, ignoring the details of the expansion of the Universe. One may thus relax the exponential inflation and the slow-roll conditions for the inflaton field. As a result, it is possible that the primordial non-gaussianities, which are " slow-roll suppressed” in the standard scenarios, become large. We calculate the non-gaussianities from the bispectrum of the perturbation and find that the equilateral-type non-gaussianity is of the order of unity, while the local-type non-gaussianity remains small, as in the usual single-field slow-roll inflation model in general relativity. Our result is a new constraint on Hořava-Lifshitz gravity.
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