2024 Vol. 48, No. 2
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2024, 48(2): 023001. doi: 10.1088/1674-1137/acf701
Abstract:
The identification of jets originating from quarks and gluons, often referred to as quark/gluon tagging, plays an important role in various analyses performed at the Large Hadron Collider, as Standard Model measurements and searches for new particles decaying to quarks often rely on suppressing a large gluon-induced background. This paper describes the measurement of the efficiencies of quark/gluon taggers developed within the ATLAS Collaboration, using\begin{document}$\sqrt{s} = 13$\end{document} ![]()
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\begin{document}$^{-1}$\end{document} ![]()
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The identification of jets originating from quarks and gluons, often referred to as quark/gluon tagging, plays an important role in various analyses performed at the Large Hadron Collider, as Standard Model measurements and searches for new particles decaying to quarks often rely on suppressing a large gluon-induced background. This paper describes the measurement of the efficiencies of quark/gluon taggers developed within the ATLAS Collaboration, using
2024, 48(2): 023101. doi: 10.1088/1674-1137/ad0f89
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Combining the dark matter and muon\begin{document}$ g-2 $\end{document} ![]()
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\begin{document}$ U(1)_{L_\mu-L_\tau} $\end{document} ![]()
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\begin{document}$ U(1)_{L_\mu-L_\tau} $\end{document} ![]()
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\begin{document}$ E_1,\; E_2,\; N $\end{document} ![]()
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\begin{document}$ U(1)_{L_\mu-L_\tau} $\end{document} ![]()
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\begin{document}$ Z' $\end{document} ![]()
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\begin{document}$ X_I $\end{document} ![]()
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\begin{document}$ X_R $\end{document} ![]()
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\begin{document}$ g-2 $\end{document} ![]()
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\begin{document}$\min(m_{E_1},m_{E_2},m_N,m_{X_R})$\end{document} ![]()
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\begin{document}$\min(m_{Z'},m_S)$\end{document} ![]()
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\begin{document}$ m_{X_I} $\end{document} ![]()
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\begin{document}$ g-2 $\end{document} ![]()
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\begin{document}$ U(1)_{L_\mu-L_\tau} $\end{document} ![]()
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Combining the dark matter and muon
2024, 48(2): 023102. doi: 10.1088/1674-1137/ad123f
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The s-wave pion-pion scattering lengths\begin{document}$ a_0 $\end{document} ![]()
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\begin{document}$ a_2 $\end{document} ![]()
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\begin{document}$ a_0 $\end{document} ![]()
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\begin{document}$ a_2 $\end{document} ![]()
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\begin{document}$ a_0 $\end{document} ![]()
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The s-wave pion-pion scattering lengths
2024, 48(2): 023103. doi: 10.1088/1674-1137/ad102c
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Radiative decays\begin{document}$ D^*_{(s)}\to D_{(s)}\gamma $\end{document} ![]()
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\begin{document}$ g_{D^*D\gamma} $\end{document} ![]()
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\begin{document}$ \rm{GeV}^{-1} $\end{document} ![]()
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\begin{document}$ |g_{D^{*+}D^+\gamma}| = 0.45(9) $\end{document} ![]()
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\begin{document}$ |g_{D^{*0}D^0\gamma}| = 1.72(34) $\end{document} ![]()
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\begin{document}$ |g_{D^{*+}D^+\gamma}|=0.47(7) $\end{document} ![]()
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\begin{document}$ |g_{D^{*0}D^0\gamma}|=1.77(16) $\end{document} ![]()
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\begin{document}$ D^*_s\to D_s\gamma $\end{document} ![]()
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\begin{document}$ |g_{D^*_s D_s\gamma}|=0.60(19) $\end{document} ![]()
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\begin{document}$ |g_{D^*_s D_s\gamma}|=0.11(2) $\end{document} ![]()
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\begin{document}$ 3\sigma $\end{document} ![]()
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\begin{document}$ |g_{D^*_s D_s\gamma}|=0.29(6) $\end{document} ![]()
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Radiative decays
2024, 48(2): 023104. doi: 10.1088/1674-1137/ad13f8
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This study explores the possibility of discovering\begin{document}$ H^{\pm} $\end{document} ![]()
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\begin{document}$ H^{\pm}\rightarrow W^\pm\phi $\end{document} ![]()
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\begin{document}$ m_{H^\pm} $\end{document} ![]()
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\begin{document}$ H^\pm\rightarrow W^\pm\phi $\end{document} ![]()
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\begin{document}$ pp $\end{document} ![]()
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\begin{document}$ \sqrt{s} $\end{document} ![]()
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This study explores the possibility of discovering
2024, 48(2): 023105. doi: 10.1088/1674-1137/ad13f9
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In this study, we assign the tetraquark state for the\begin{document}$ Y(4230) $\end{document} ![]()
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\begin{document}$ Y(4230) $\end{document} ![]()
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\begin{document}$ g_{Y J/\psi f_0} $\end{document} ![]()
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\begin{document}$ g_{Y J/\psi f_0} $\end{document} ![]()
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\begin{document}$ Y(4230)\to $\end{document} ![]()
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\begin{document}$ J/\psi f_0(980) $\end{document} ![]()
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\begin{document}$ Y(4230)\to J/\psi f_0(980) $\end{document} ![]()
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In this study, we assign the tetraquark state for the
2024, 48(2): 024001. doi: 10.1088/1674-1137/ad0e5a
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The excitation function of the\begin{document}$ {}^{58}{\rm{Ni}} (n, p){}^{58}{\rm {Co}} $\end{document} ![]()
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\begin{document}$ \rm MeV $\end{document} ![]()
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\begin{document}$ ^{7}{\rm{Li}}(p, n) $\end{document} ![]()
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\begin{document}$ {}^{115}{\rm{In}} (n, n'){}^{115{\rm m}}{\rm{In}} $\end{document} ![]()
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\begin{document}$ {}^{58}{\rm{Ni}} (n, p){}^{58}{\rm{Co}} $\end{document} ![]()
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The excitation function of the
2024, 48(2): 024002. doi: 10.1088/1674-1137/ad11e4
Abstract:
In this study, experiments were performed at bremsstrahlung end-point energies of 10−23 MeV with the beam from the MT-25 microtron using the
In this study, experiments were performed at bremsstrahlung end-point energies of 10−23 MeV with the beam from the MT-25 microtron using the
2024, 48(2): 024101. doi: 10.1088/1674-1137/ad0e04
Abstract:
The equation of state (EOS) of dense nuclear matter is a key factor for determining the internal structure and properties of neutron stars. However, the EOS of high-density nuclear matter has great uncertainty, mainly because terrestrial nuclear experiments cannot reproduce matter as dense as that in the inner core of a neutron star. Fortunately, continuous improvements in astronomical observations of neutron stars provide the opportunity to inversely constrain the EOS of high-density nuclear matter. Several methods have been proposed to implement this inverse constraint, including the Bayesian analysis algorithm, the Lindblom's approach, and so on. Neural network algorithm is an effective method developed in recent years. By employing a set of isospin-dependent parametric EOSs as the training sample of a neural network algorithm, we set up an effective way to reconstruct the EOS with relative accuracy using a few mass-radius data. Based on the obtained neural network algorithms and according to the NICER observations on masses and radii of neutron stars with assumed precision, we obtain the inversely constrained EOS and further calculate the corresponding macroscopic properties of the neutron star. The results are basically consistent with the constraint on EOS in Huth et al. [Nature 606, 276 (2022)] based on Bayesian analysis. Moreover, the results show that even though the neural network algorithm was obtained using the finite parameterized EOS as the training set, it is valid for any rational parameter combination of the parameterized EOS model.
The equation of state (EOS) of dense nuclear matter is a key factor for determining the internal structure and properties of neutron stars. However, the EOS of high-density nuclear matter has great uncertainty, mainly because terrestrial nuclear experiments cannot reproduce matter as dense as that in the inner core of a neutron star. Fortunately, continuous improvements in astronomical observations of neutron stars provide the opportunity to inversely constrain the EOS of high-density nuclear matter. Several methods have been proposed to implement this inverse constraint, including the Bayesian analysis algorithm, the Lindblom's approach, and so on. Neural network algorithm is an effective method developed in recent years. By employing a set of isospin-dependent parametric EOSs as the training sample of a neural network algorithm, we set up an effective way to reconstruct the EOS with relative accuracy using a few mass-radius data. Based on the obtained neural network algorithms and according to the NICER observations on masses and radii of neutron stars with assumed precision, we obtain the inversely constrained EOS and further calculate the corresponding macroscopic properties of the neutron star. The results are basically consistent with the constraint on EOS in Huth et al. [Nature 606, 276 (2022)] based on Bayesian analysis. Moreover, the results show that even though the neural network algorithm was obtained using the finite parameterized EOS as the training set, it is valid for any rational parameter combination of the parameterized EOS model.
2024, 48(2): 024102. doi: 10.1088/1674-1137/ad021c
Abstract:
A neural network with two hidden layers is developed for nuclear mass prediction, based on the finite-range droplet model (FRDM12). Different hyperparameters, including the number of hidden units, choice of activation functions, initializers, and learning rates, are adjusted explicitly and systematically. The resulting mass predictions are achieved by averaging the predictions given by several different sets of hyperparameters with different regularizers and seed numbers. This can provide not only the average values of mass predictions but also reliable estimations in the mass prediction uncertainties. The overall root-mean-square deviations of nuclear mass are reduced from 0.603 MeV for the FRDM12 model to 0.200 MeV and 0.232 MeV for the training and validation sets, respectively.
A neural network with two hidden layers is developed for nuclear mass prediction, based on the finite-range droplet model (FRDM12). Different hyperparameters, including the number of hidden units, choice of activation functions, initializers, and learning rates, are adjusted explicitly and systematically. The resulting mass predictions are achieved by averaging the predictions given by several different sets of hyperparameters with different regularizers and seed numbers. This can provide not only the average values of mass predictions but also reliable estimations in the mass prediction uncertainties. The overall root-mean-square deviations of nuclear mass are reduced from 0.603 MeV for the FRDM12 model to 0.200 MeV and 0.232 MeV for the training and validation sets, respectively.
2024, 48(2): 024103. doi: 10.1088/1674-1137/ad1029
Abstract:
The angular distributions of 7Li + 144Sm elastic scattering over the energy range of 21.6–52 MeV are reanalyzed utilizing various interaction potentials. The analysis aims to study the consistency of the implemented potentials in representing the considered data and investigate the cluster nature of the weakly bound 7Li projectile. This will aid in the better understanding the impacts of 7Li breakup on the elastic scattering channel. Strong coupling to the breakup channel has a substantial impact on the elastic data and reproduces a repulsive dynamical polarization potential, which drastically diminishes the real potential strength. This reported impact was simulated by introducing a semi-microscopic repulsive DPP and by implementing the method of continuum discretized coupled channels. The analysis was also extended to understand the impact of triton transfer on the elastic scattering data.
The angular distributions of 7Li + 144Sm elastic scattering over the energy range of 21.6–52 MeV are reanalyzed utilizing various interaction potentials. The analysis aims to study the consistency of the implemented potentials in representing the considered data and investigate the cluster nature of the weakly bound 7Li projectile. This will aid in the better understanding the impacts of 7Li breakup on the elastic scattering channel. Strong coupling to the breakup channel has a substantial impact on the elastic data and reproduces a repulsive dynamical polarization potential, which drastically diminishes the real potential strength. This reported impact was simulated by introducing a semi-microscopic repulsive DPP and by implementing the method of continuum discretized coupled channels. The analysis was also extended to understand the impact of triton transfer on the elastic scattering data.
2024, 48(2): 024104. doi: 10.1088/1674-1137/ad1028
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The yields of photonuclear reactions in the 107Ag, 113In, and 115In nuclei were measured. Monte Carlo simulations were performed using the Geant4 code, and the results were compared with the experimental values. The isomeric ratios of the yields in the reactions 107Ag(γ, n)106m,gAg and 113In(γ, n)112m,gIn were determined, and the cross sections for the reactions 107Ag(γ, n)106gAg and 107Ag(γ, 2n)105Ag at an energy of 20 MeV were calculated based on the experimental data.
The yields of photonuclear reactions in the 107Ag, 113In, and 115In nuclei were measured. Monte Carlo simulations were performed using the Geant4 code, and the results were compared with the experimental values. The isomeric ratios of the yields in the reactions 107Ag(γ, n)106m,gAg and 113In(γ, n)112m,gIn were determined, and the cross sections for the reactions 107Ag(γ, n)106gAg and 107Ag(γ, 2n)105Ag at an energy of 20 MeV were calculated based on the experimental data.
2024, 48(2): 024105. doi: 10.1088/1674-1137/ad0f13
Abstract:
The photoproduction of the\begin{document}$ f_1(1285) $\end{document} ![]()
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\begin{document}$ \gamma p \to f_1(1285) p $\end{document} ![]()
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\begin{document}$ N(1990){7/2}^+ $\end{document} ![]()
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\begin{document}$ N(2000){5/2}^+ $\end{document} ![]()
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\begin{document}$ N(2040){3/2}^+ $\end{document} ![]()
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\begin{document}$ N(2060){5/2}^- $\end{document} ![]()
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\begin{document}$ N(2100){1/2}^+ $\end{document} ![]()
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\begin{document}$ N(2120){3/2}^- $\end{document} ![]()
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\begin{document}$ N(2190){7/2}^- $\end{document} ![]()
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\begin{document}$ N(2300){1/2}^+ $\end{document} ![]()
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\begin{document}$ N(2570){5/2}^- $\end{document} ![]()
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\begin{document}$ \gamma p \to f_1(1285) p $\end{document} ![]()
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\begin{document}$ \gamma p \to f_1(1285) p $\end{document} ![]()
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The photoproduction of the
2024, 48(2): 024106. doi: 10.1088/1674-1137/ad1924
Abstract:
The experimental data of elastic scattering angular distributions for 9Be, 10B, 11B, 12C, 13C, 15N, and 16O targets from 4.5 to 131.8 MeV and 7Li target from 8.0 to 42.0 MeV are fitted to realize the global phenomenological optical potentials (GPOPs) for the 7Li-induced reactions on 1p-shell nuclei. Thus, the 7Li elastic scattering from the 1p-shell nuclei can be systematically described using the established GPOPs. The elastic scattering angular distributions are also reanalyzed using a microscopic method within the framework of the new version of double folding São Paulo potential (SPP2). To better describe the elastic scattering at backward angles, the contribution of elastic transfer is further estimated by the distorted wave Born approximation (DWBA) method. Based on the obtained GPOPs, the inelastic scattering angular distributions are also obtained through the coupled channels (CC) method for the different excited states.
The experimental data of elastic scattering angular distributions for 9Be, 10B, 11B, 12C, 13C, 15N, and 16O targets from 4.5 to 131.8 MeV and 7Li target from 8.0 to 42.0 MeV are fitted to realize the global phenomenological optical potentials (GPOPs) for the 7Li-induced reactions on 1p-shell nuclei. Thus, the 7Li elastic scattering from the 1p-shell nuclei can be systematically described using the established GPOPs. The elastic scattering angular distributions are also reanalyzed using a microscopic method within the framework of the new version of double folding São Paulo potential (SPP2). To better describe the elastic scattering at backward angles, the contribution of elastic transfer is further estimated by the distorted wave Born approximation (DWBA) method. Based on the obtained GPOPs, the inelastic scattering angular distributions are also obtained through the coupled channels (CC) method for the different excited states.
2024, 48(2): 025101. doi: 10.1088/1674-1137/ad137f
Abstract:
In this study, we explore the properties of a non-rotating black hole in the Einstein-Maxwell-scalar (EMS) theory and investigate the luminosity of the accretion disk surrounding it. We determine all the orbital parameters of particles in the accretion disk, including the radius of the innermost stable circular orbit (ISCO) with angular velocity, angular momentum, and energy. Further, we study the radiative efficiency for different values of black hole parameters. Finally, we analyze the flux, differential luminosity, and temperature of the accretion disk.
In this study, we explore the properties of a non-rotating black hole in the Einstein-Maxwell-scalar (EMS) theory and investigate the luminosity of the accretion disk surrounding it. We determine all the orbital parameters of particles in the accretion disk, including the radius of the innermost stable circular orbit (ISCO) with angular velocity, angular momentum, and energy. Further, we study the radiative efficiency for different values of black hole parameters. Finally, we analyze the flux, differential luminosity, and temperature of the accretion disk.
2024, 48(2): 025102. doi: 10.1088/1674-1137/ad102a
Abstract:
We conducted a comprehensive study of the neutron capture cross section of\begin{document}$ ^{12}\mathrm C $\end{document} ![]()
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\begin{document}$ \pm $\end{document} ![]()
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\begin{document}$ \dfrac{1}{v} $\end{document} ![]()
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We conducted a comprehensive study of the neutron capture cross section of
Impact of a nearby subhalo on the constraint of dark matter annihilation from cosmic ray antiprotons
2024, 48(2): 025103. doi: 10.1088/1674-1137/ad13f7
Abstract:
Numerous simulations indicate that a large number of subhalos should be hosted by the Milky Way. The potential existence of a nearby subhalo could have important implications for our understanding of dark matter (DM) annihilation. In this study, we investigate the hypothetical presence of a nearby subhalo and set the upper limits on the DM annihilation cross section by analyzing the cosmic-ray antiproton spectrum. By presenting the ratios of annihilation cross section limits for scenarios with and without a nearby subhalo, we can quantitatively evaluate the potential impact of the nearby subhalo on the limits of the DM annihilation cross section. The impacts of the concentration model and the subhalo probability distribution have been considered. We explore the antiproton contribution of the potential nearby DM subhalo accounting for the DAMPE\begin{document}$ e^\pm $\end{document} ![]()
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\begin{document}$ \sim 1.4 $\end{document} ![]()
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Numerous simulations indicate that a large number of subhalos should be hosted by the Milky Way. The potential existence of a nearby subhalo could have important implications for our understanding of dark matter (DM) annihilation. In this study, we investigate the hypothetical presence of a nearby subhalo and set the upper limits on the DM annihilation cross section by analyzing the cosmic-ray antiproton spectrum. By presenting the ratios of annihilation cross section limits for scenarios with and without a nearby subhalo, we can quantitatively evaluate the potential impact of the nearby subhalo on the limits of the DM annihilation cross section. The impacts of the concentration model and the subhalo probability distribution have been considered. We explore the antiproton contribution of the potential nearby DM subhalo accounting for the DAMPE
2024, 48(2): 025104. doi: 10.1088/1674-1137/ad1677
Abstract:
In this study, we investigated the gravitational weak lensing and shadow of the Ellis-Bronnikov wormhole. First, we studied the photon motion in a plasma medium and a wormhole shadow. It was shown that the radius of the photon sphere of the Ellis-Bronnikov wormhole and the size of the wormhole shadow become larger under the influence of the parameter a. The upper limit of the parameter a in the Ellis-Bronnikov wormhole spacetime was obtained. Second, we investigated the weak gravitational lensing for the Ellis-Bronnikov wormhole and calculated the deflection angle for uniform and non uniform plasma cases. The value of the deflection angle for uniform plasma increased with the increase in plasma parameter value, and vice versa for non uniform plasma. We found that, under the influence of the parameter a, the values of the deflection angles for two cases decreased. Finally, we investigated the magnification of image brightness using the deflection angle of the light rays around the wormhole in the Ellis-Bronnikov theory.
In this study, we investigated the gravitational weak lensing and shadow of the Ellis-Bronnikov wormhole. First, we studied the photon motion in a plasma medium and a wormhole shadow. It was shown that the radius of the photon sphere of the Ellis-Bronnikov wormhole and the size of the wormhole shadow become larger under the influence of the parameter a. The upper limit of the parameter a in the Ellis-Bronnikov wormhole spacetime was obtained. Second, we investigated the weak gravitational lensing for the Ellis-Bronnikov wormhole and calculated the deflection angle for uniform and non uniform plasma cases. The value of the deflection angle for uniform plasma increased with the increase in plasma parameter value, and vice versa for non uniform plasma. We found that, under the influence of the parameter a, the values of the deflection angles for two cases decreased. Finally, we investigated the magnification of image brightness using the deflection angle of the light rays around the wormhole in the Ellis-Bronnikov theory.
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Original research articles, Ietters and reviews Covering theory and experiments in the fieids of
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- Cosmology
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