2024 Vol. 48, No. 12
Display Method: |
2024, 48(12): 123001. doi: 10.1088/1674-1137/ad70a0
Abstract:
We present a measurement of the integrated luminosity of\begin{document}$ e^+e^- $\end{document} ![]()
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\begin{document}$ E_{\rm cm} = 3.773 $\end{document} ![]()
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\begin{document}$ 4.995 \pm 0.019 $\end{document} ![]()
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\begin{document}$ ^{-1} $\end{document} ![]()
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\begin{document}$ 8.157 \pm 0.031 $\end{document} ![]()
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\begin{document}$ ^{-1} $\end{document} ![]()
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\begin{document}$ 4.191 \pm 0.016 $\end{document} ![]()
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\begin{document}$ ^{-1} $\end{document} ![]()
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We present a measurement of the integrated luminosity of
2024, 48(12): 123101. doi: 10.1088/1674-1137/ad75f5
Abstract:
We systematically examined the mass spectra and their two-body hadronic decays of the beauty-charm meson family considering coupled channel effects. Our results can effectively explain the observed\begin{document}$B_c$\end{document} ![]()
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\begin{document}$1S$\end{document} ![]()
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\begin{document}$2S$\end{document} ![]()
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\begin{document}$1P$\end{document} ![]()
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\begin{document}$1D$\end{document} ![]()
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\begin{document}$2^3P_2$\end{document} ![]()
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\begin{document}$3^1S_0$\end{document} ![]()
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\begin{document}$3^3S_1$\end{document} ![]()
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\begin{document}$2^3D_1$\end{document} ![]()
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\begin{document}$2D$\end{document} ![]()
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\begin{document}$2D^\prime$\end{document} ![]()
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\begin{document}$2^3D_3$\end{document} ![]()
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\begin{document}$B_c(n{}^3L_L)$\end{document} ![]()
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\begin{document}$B_c(n{}^1L_L)$\end{document} ![]()
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We systematically examined the mass spectra and their two-body hadronic decays of the beauty-charm meson family considering coupled channel effects. Our results can effectively explain the observed
2024, 48(12): 123102. doi: 10.1088/1674-1137/ad7247
Abstract:
The semileptonic and nonleptonic decays of the b-flavor vector mesons\begin{document}$B^{*}_{u,d,s}$\end{document} ![]()
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\begin{document}$B_{c}^{*}$\end{document} ![]()
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\begin{document}$B_{u, d, s, c}^{*}\to P$\end{document} ![]()
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\begin{document}$\pi, K, \eta_c(1S,2S), D_{(s)}, B_{(s)}$\end{document} ![]()
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\begin{document}$f_{L}, f_{\|}$\end{document} ![]()
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\begin{document}$A_{FB}$\end{document} ![]()
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\begin{document}$B_{s}^{*0}\to D_{s}^{-}\ell^{\prime+}{\nu}_{\ell^\prime}$\end{document} ![]()
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\begin{document}$B_{c}^{*+}\to B_{s}^{0}\ell^{\prime+}{\nu}_{\ell^\prime}, \eta_{c}\ell^{\prime+}{\nu}_{\ell^\prime}$\end{document} ![]()
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\begin{document}$\ell^\prime$\end{document} ![]()
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\begin{document}$\tau$\end{document} ![]()
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\begin{document}$B_{c}^{*+}\to $\end{document} ![]()
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\begin{document}$ B^0_{s} \pi^{+}, B^0_{s} \rho^{+}$\end{document} ![]()
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The semileptonic and nonleptonic decays of the b-flavor vector mesons
2024, 48(12): 123103. doi: 10.1088/1674-1137/ad77b3
Abstract:
Effective field theory (EFT) provides a model-independent framework for interpreting the results of dark matter (DM) direct detection experiments. In this study, we demonstrate that the two fermionic DM-quark tensor operators\begin{document}$(\bar{\chi} {\rm{i}}\sigma^{\mu\nu} \gamma^5 \chi) (\bar{q} \sigma_{\mu\nu}q)$\end{document} ![]()
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\begin{document}$ (\bar{\chi} \sigma^{\mu\nu} \chi) (\bar{q} \sigma_{\mu\nu} q) $\end{document} ![]()
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\begin{document}$m_\chi \lesssim 1\;{\rm{GeV}}$\end{document} ![]()
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\begin{document}$5\;{\rm{MeV}}$\end{document} ![]()
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\begin{document}$(\bar{\chi} \sigma^{\mu\nu}{\rm{i}}\gamma_5 \chi) (\bar{q} \sigma_{\mu\nu}q)$\end{document} ![]()
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\begin{document}$m_\chi \gtrsim 10\;{\rm{GeV}}$\end{document} ![]()
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Effective field theory (EFT) provides a model-independent framework for interpreting the results of dark matter (DM) direct detection experiments. In this study, we demonstrate that the two fermionic DM-quark tensor operators
2024, 48(12): 123104. doi: 10.1088/1674-1137/ad736f
Abstract:
Decay constants of pseudoscalar mesons D,\begin{document}$ D_s $\end{document} ![]()
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\begin{document}$ \eta_c $\end{document} ![]()
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\begin{document}$ D^* $\end{document} ![]()
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\begin{document}$ D_s^* $\end{document} ![]()
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\begin{document}$ J/\psi $\end{document} ![]()
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\begin{document}$ N_f=2+1 $\end{document} ![]()
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\begin{document}$ a\sim0.08 $\end{document} ![]()
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\begin{document}$ {{\overline{{\rm{MS}}}}} $\end{document} ![]()
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\begin{document}$ 2 $\end{document} ![]()
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\begin{document}$ a\sim0.11 $\end{document} ![]()
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\begin{document}$ f_{D_s^*}^T({{\overline{{\rm{MS}}}}},\text{ 2 GeV})/f_{D_s^*}=0.909(18) $\end{document} ![]()
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\begin{document}$ f_{D_s^*}=277(11) $\end{document} ![]()
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\begin{document}$ D_s^* $\end{document} ![]()
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\begin{document}$ 4.26(52)\times10^{-5} $\end{document} ![]()
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\begin{document}$ D_s^* $\end{document} ![]()
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Decay constants of pseudoscalar mesons D,
2024, 48(12): 123105. doi: 10.1088/1674-1137/ad77b2
Abstract:
The b-factories, such as BelleII, BarBar, and LHCb, emphasize the increasing importance of exotic hadron research. In this paper, we discuss the possible production of singly anti-charmed pentaquark states\begin{document}$\bar{c}q qqq$\end{document} ![]()
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\begin{document}$S U$\end{document} ![]()
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\begin{document}$P_{\bar c}$\end{document} ![]()
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\begin{document}$B^0 \to {P}_{\bar{c}sudu}^{(\prime) 0}\Sigma^0$\end{document} ![]()
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\begin{document}$P_{\bar c}$\end{document} ![]()
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The b-factories, such as BelleII, BarBar, and LHCb, emphasize the increasing importance of exotic hadron research. In this paper, we discuss the possible production of singly anti-charmed pentaquark states
2024, 48(12): 123106. doi: 10.1088/1674-1137/ad745c
Abstract:
The Pryce (e) spin and position operators of the quantum theory of Dirac's free field were re-defined and studied recently with the help of a new spin symmetry and suitable spectral representations [Eur. Phys. J. C 82, 1073 (2022)]. This approach is generalized here, associating a pair of integral operators acting directly on particle and antiparticle wave spinors in momentum representation to any integral operator in configuration representation, acting on mode spinors. This framework allows an effective quantization procedure, giving a large set of one-particle operators with physical meaning as the spin and orbital parts of the isometry generators, the Pauli-Lubanski and position operators, or other spin-type operators proposed to date. Special attention is paid to the operators that mix the particle and antiparticle sectors whose off-diagonal associated operators have oscillating terms producing Zitterbevegung. The principal operators of this type, including the usual coordinate operator, are derived here for the first time. As an application, it is shown that an apparatus measuring these new observables may prepare and detect one-particle wave packets moving uniformly without Zitterbewegung or spin dynamics, spreading in time normally as any other relativistic or even non-relativistic wave packet.
The Pryce (e) spin and position operators of the quantum theory of Dirac's free field were re-defined and studied recently with the help of a new spin symmetry and suitable spectral representations [Eur. Phys. J. C 82, 1073 (2022)]. This approach is generalized here, associating a pair of integral operators acting directly on particle and antiparticle wave spinors in momentum representation to any integral operator in configuration representation, acting on mode spinors. This framework allows an effective quantization procedure, giving a large set of one-particle operators with physical meaning as the spin and orbital parts of the isometry generators, the Pauli-Lubanski and position operators, or other spin-type operators proposed to date. Special attention is paid to the operators that mix the particle and antiparticle sectors whose off-diagonal associated operators have oscillating terms producing Zitterbevegung. The principal operators of this type, including the usual coordinate operator, are derived here for the first time. As an application, it is shown that an apparatus measuring these new observables may prepare and detect one-particle wave packets moving uniformly without Zitterbewegung or spin dynamics, spreading in time normally as any other relativistic or even non-relativistic wave packet.
2024, 48(12): 124001. doi: 10.1088/1674-1137/ad7370
Abstract:
In this study, measurements of the 128Te(n, 2n)127m,gTe reaction cross sections and the computation of the isomeric cross section ratio were performed around the neutron energy of 13−15 MeV. We used a γ-ray spectrometric technique to conduct the measurements. The neutron energy was produced by the 3H(d,n)4He reaction. For the 128Te(n, 2n)127m,gTe reaction, the excited state, ground state, total cross section, and isomeric cross section ratio were determined using the TALYS-1.96 code, a theoretical nuclear model that allows for variations in density options. The initial experimental data, assessed nuclear data, and theoretical calculations based on the TALYS-1.96 algorithm were compared with the measurement results. The new data produced by this study are essential for validating nuclear models and establishing parameters for nuclear reactions.
In this study, measurements of the 128Te(n, 2n)127m,gTe reaction cross sections and the computation of the isomeric cross section ratio were performed around the neutron energy of 13−15 MeV. We used a γ-ray spectrometric technique to conduct the measurements. The neutron energy was produced by the 3H(d,n)4He reaction. For the 128Te(n, 2n)127m,gTe reaction, the excited state, ground state, total cross section, and isomeric cross section ratio were determined using the TALYS-1.96 code, a theoretical nuclear model that allows for variations in density options. The initial experimental data, assessed nuclear data, and theoretical calculations based on the TALYS-1.96 algorithm were compared with the measurement results. The new data produced by this study are essential for validating nuclear models and establishing parameters for nuclear reactions.
2024, 48(12): 124101. doi: 10.1088/1674-1137/ad6e61
Abstract:
The intrinsic vibrational motion and the rotational behavior of the scissors mode in well deformed nuclei are investigated with an angular-momentum-projected approach, which is interpreted as a generator-coordinate-method with the generator coordinates corresponding to the degrees of freedom of interest. The picture of the intrinsic and rotational motion of the scissors mode is illustrated from the collective wave function within the framework of the generator-coordinate-method. The harmonicity of the scissors vibration is found to arise naturally from the present model but can be disturbed by the Coriolis effect as spin increases. The odd and even spin members of the rotational band based on the scissors mode rotate about different axes perpendicular to each other, leading to the flipping moment of inertia and the consequent splitting behavior that has been suggested previously.
The intrinsic vibrational motion and the rotational behavior of the scissors mode in well deformed nuclei are investigated with an angular-momentum-projected approach, which is interpreted as a generator-coordinate-method with the generator coordinates corresponding to the degrees of freedom of interest. The picture of the intrinsic and rotational motion of the scissors mode is illustrated from the collective wave function within the framework of the generator-coordinate-method. The harmonicity of the scissors vibration is found to arise naturally from the present model but can be disturbed by the Coriolis effect as spin increases. The odd and even spin members of the rotational band based on the scissors mode rotate about different axes perpendicular to each other, leading to the flipping moment of inertia and the consequent splitting behavior that has been suggested previously.
2024, 48(12): 124102. doi: 10.1088/1674-1137/ad6c0a
Abstract:
This study utilizes the Bayesian neural network (BNN) method in machine learning to learn and predict the cross-sectional data of 28Si projectile fragmentation for different targets at different energies and to quantify the uncertainty. The detailed modeling process of the BNN is presented, and its prediction results are compared with those of the Cummings, Nilsen, EPAX2, EPAX3, and FRACS models and experimental measurement values. The results reveal that, compared with other models, the BNN method achieves the smallest root-mean-square error (RMSE) and the highest agreement with the experimental values. Only the BNN method and FRACS model show a significant odd-even staggering effect; however, the results of the BNN method are closer to the experimental values. Furthermore, the BNN method is the only model capable of reproducing data features with low cross-section values at Z = 9, and the average ratio of the predicted to experimental values of the BNN is close to 1.0. These results indicate that the BNN method can accurately reproduce and predict the fragment production cross sections of 28Si projectile fragmentation and demonstrate its ability to capture key data characteristics.
This study utilizes the Bayesian neural network (BNN) method in machine learning to learn and predict the cross-sectional data of 28Si projectile fragmentation for different targets at different energies and to quantify the uncertainty. The detailed modeling process of the BNN is presented, and its prediction results are compared with those of the Cummings, Nilsen, EPAX2, EPAX3, and FRACS models and experimental measurement values. The results reveal that, compared with other models, the BNN method achieves the smallest root-mean-square error (RMSE) and the highest agreement with the experimental values. Only the BNN method and FRACS model show a significant odd-even staggering effect; however, the results of the BNN method are closer to the experimental values. Furthermore, the BNN method is the only model capable of reproducing data features with low cross-section values at Z = 9, and the average ratio of the predicted to experimental values of the BNN is close to 1.0. These results indicate that the BNN method can accurately reproduce and predict the fragment production cross sections of 28Si projectile fragmentation and demonstrate its ability to capture key data characteristics.
2024, 48(12): 124103. doi: 10.1088/1674-1137/ad766e
Abstract:
The existence of magic numbers of protons and neutrons in nuclei is essential for understanding the nuclear structure and fundamental nuclear forces. Over decades, researchers have conducted theoretical and experimental studies on a new magic number, Z(N)=6, focusing on observables such as radii, binding energy, electromagnetic transition, and nucleon separation energies. We performed ab initio no-core shell model calculations for the occupation numbers of the lowest single particle states in the ground states of Z(N)=6 and Z(N)=8 isotopes (isotones). The results of our calculations do not support Z(N)=6 as a magic number over a range of atomic numbers. However, 14C and 14O exhibit the characteristics of double-magic nuclei.
The existence of magic numbers of protons and neutrons in nuclei is essential for understanding the nuclear structure and fundamental nuclear forces. Over decades, researchers have conducted theoretical and experimental studies on a new magic number, Z(N)=6, focusing on observables such as radii, binding energy, electromagnetic transition, and nucleon separation energies. We performed ab initio no-core shell model calculations for the occupation numbers of the lowest single particle states in the ground states of Z(N)=6 and Z(N)=8 isotopes (isotones). The results of our calculations do not support Z(N)=6 as a magic number over a range of atomic numbers. However, 14C and 14O exhibit the characteristics of double-magic nuclei.
2024, 48(12): 124104. doi: 10.1088/1674-1137/ad7011
Abstract:
Research on the pairing phase transition in the odd-A nucleus\begin{document}$ ^{161}\text{Dy} $\end{document} ![]()
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\begin{document}$ ^{161}\text{Dy} $\end{document} ![]()
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Research on the pairing phase transition in the odd-A nucleus
2024, 48(12): 124105. doi: 10.1088/1674-1137/ad86b0
Abstract:
We employ the dinuclear system (DNS) model combined with a statistical model to calculate the evaporation residue cross sections of the reaction systems\begin{document}$ ^{48} $\end{document} ![]()
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\begin{document}$ ^{243} $\end{document} ![]()
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\begin{document}$ ^{48} $\end{document} ![]()
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\begin{document}$ ^{248} $\end{document} ![]()
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\begin{document}$ ^{48} $\end{document} ![]()
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\begin{document}$ ^{249} $\end{document} ![]()
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\begin{document}$ Z = 119 $\end{document} ![]()
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\begin{document}$ ^{54} $\end{document} ![]()
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\begin{document}$ ^{243} $\end{document} ![]()
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\begin{document}$ ^{51} $\end{document} ![]()
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\begin{document}$ ^{248} $\end{document} ![]()
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\begin{document}$ ^{50} $\end{document} ![]()
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\begin{document}$ ^{249} $\end{document} ![]()
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\begin{document}$ Z = 119 $\end{document} ![]()
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We employ the dinuclear system (DNS) model combined with a statistical model to calculate the evaporation residue cross sections of the reaction systems
2024, 48(12): 125101. doi: 10.1088/1674-1137/ad6e62
Abstract:
We investigated some Friedmann-Lemaître-Robertson-Walker (FLRW) cosmological models in the context of metric-affine\begin{document}$F(R,Q)$\end{document} ![]()
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\begin{document}$H_{0}$\end{document} ![]()
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\begin{document}$\Omega_{m0}$\end{document} ![]()
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\begin{document}$\omega_{de}$\end{document} ![]()
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We investigated some Friedmann-Lemaître-Robertson-Walker (FLRW) cosmological models in the context of metric-affine
2024, 48(12): 125102. doi: 10.1088/1674-1137/ad654e
Abstract:
This manuscript aims to study cosmic warm inflation (WI) in the framework of\begin{document}$f(Q)$\end{document} ![]()
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\begin{document}$2\sigma$\end{document} ![]()
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This manuscript aims to study cosmic warm inflation (WI) in the framework of
2024, 48(12): 125103. doi: 10.1088/1674-1137/ad745b
Abstract:
Our manuscript aims to analyze the viability and stability of anisotropic stellar objects in the modified symmetric teleparallel gravity. A particular model of this extended theory is considered to formulate explicit field equations that govern the interaction between matter and geometry. The configuration of static spherical symmetric structures is examined through the Finch-Skea solution. However, the values of unknown constants in the metric potentials are evaluated by the Darmois junction conditions. For the viability of the proposed stellar objects, physical parameters including density, pressure, anisotropy, mass, energy constraints, compactness function, and redshift are analyzed. Furthermore, the stability of the proposed stellar objects is investigated by the causality condition, Herrera cracking approach, and adiabatic index. Our findings indicate that the proposed stellar objects are viable as well as stable in the presence of correction terms.
Our manuscript aims to analyze the viability and stability of anisotropic stellar objects in the modified symmetric teleparallel gravity. A particular model of this extended theory is considered to formulate explicit field equations that govern the interaction between matter and geometry. The configuration of static spherical symmetric structures is examined through the Finch-Skea solution. However, the values of unknown constants in the metric potentials are evaluated by the Darmois junction conditions. For the viability of the proposed stellar objects, physical parameters including density, pressure, anisotropy, mass, energy constraints, compactness function, and redshift are analyzed. Furthermore, the stability of the proposed stellar objects is investigated by the causality condition, Herrera cracking approach, and adiabatic index. Our findings indicate that the proposed stellar objects are viable as well as stable in the presence of correction terms.
2024, 48(12): 125104. doi: 10.1088/1674-1137/ad78d5
Abstract:
By considering an asymmetric thin-shell wormhole (ATSW) surrounded by an optically and geometrically thin disk, we investigate the luminosity distribution of this ATSW with the spacetime on two sides encoded with the renormalization group improved (RGI) parameters (Ω, γ). Although some light rays are absorbed into the throat in the vicinity of the wormhole, they return through the throat with certain conditions, unlike in the case of black holes. The spacetime on one side of the wormhole can capture the additional photons emitted from the thin disk, resulting in several interesting observable features of the wormhole. The results in this paper show that there are two additional orbit numbers n in the ATSW and six transfer functions, rather than three as in the black hole case. In this case, the ATSW indeed has a more complex observable structure, where some additional light rings arise naturally. For instance, there are two additional photon rings for the emitted Model 1. Moreover, we also find a new wide hump between the first and second additional photon rings in Model 2. The effects of Ω and γ on the observed images are clearly addressed throughout this study, and the influence of Ω is found to be larger. Finally, we conclude that the observations of the RGI-ATSW can help further distinguish it from other ATSWs and black holes when a thin accretion disk exists around it.
By considering an asymmetric thin-shell wormhole (ATSW) surrounded by an optically and geometrically thin disk, we investigate the luminosity distribution of this ATSW with the spacetime on two sides encoded with the renormalization group improved (RGI) parameters (Ω, γ). Although some light rays are absorbed into the throat in the vicinity of the wormhole, they return through the throat with certain conditions, unlike in the case of black holes. The spacetime on one side of the wormhole can capture the additional photons emitted from the thin disk, resulting in several interesting observable features of the wormhole. The results in this paper show that there are two additional orbit numbers n in the ATSW and six transfer functions, rather than three as in the black hole case. In this case, the ATSW indeed has a more complex observable structure, where some additional light rings arise naturally. For instance, there are two additional photon rings for the emitted Model 1. Moreover, we also find a new wide hump between the first and second additional photon rings in Model 2. The effects of Ω and γ on the observed images are clearly addressed throughout this study, and the influence of Ω is found to be larger. Finally, we conclude that the observations of the RGI-ATSW can help further distinguish it from other ATSWs and black holes when a thin accretion disk exists around it.
2024, 48(12): 125105. doi: 10.1088/1674-1137/ad79d5
Abstract:
Pulsar timing array (PTA) data releases show strong evidence for a stochastic gravitational-wave background in the nanohertz band. When the signal is interpreted by a scenario of scalar-induced gravitational waves (SIGWs), we encounter overproduction of primordial black holes (PBHs). We wonder if varying the equation of state (EoS) of the early Universe can resolve this issue and thereby lead to a consistent interpretation of the PTA data. Analyzing a data combination of PTA, big-bang nucleosynthesis, and cosmic microwave background, we find that an epoch with EoS\begin{document}$w\sim{\cal{O}}(10^{-2})$\end{document} ![]()
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\begin{document}$w=0.44_{-0.40}^{+0.52}$\end{document} ![]()
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Pulsar timing array (PTA) data releases show strong evidence for a stochastic gravitational-wave background in the nanohertz band. When the signal is interpreted by a scenario of scalar-induced gravitational waves (SIGWs), we encounter overproduction of primordial black holes (PBHs). We wonder if varying the equation of state (EoS) of the early Universe can resolve this issue and thereby lead to a consistent interpretation of the PTA data. Analyzing a data combination of PTA, big-bang nucleosynthesis, and cosmic microwave background, we find that an epoch with EoS
2024, 48(12): 125106. doi: 10.1088/1674-1137/ad79d4
Abstract:
In both the canonical ensemble and grand canonical ensemble, the thermodynamic stability and phase structure of Einstein-Euler-Heisenberg-AdS black holes are studied. We derive the Hawking temperature, Helmholtz free energy, Gibbs potential, entropy and heat capacity of the black holes. We compute the minimum temperature to find that a phase transition may happen at the lowest point. The entropy-temperature diagram consists of two parts. The upper part belonging to the large black holes under the influence from the electromagnetic self-interactions keeps the positive heat capacity, leading the huge compact objects to survive. The lower curves corresponding to small black holes show that the heat capacity of the tiny black holes is negative, which means that the nonlinear-effect-corrected smaller sources will evaporate. The further discussions show that the nonlinear effect modifies the thermodynamic quantities, but the corrections limited by the nonlinear factor μ with allowed values can not change the properties and the phase structure fundamentally and thoroughly. We argue that the influence from self-interaction can not make the Einstein-Euler-Heisenberg-AdS black holes to split under the second law of thermodynamics.
In both the canonical ensemble and grand canonical ensemble, the thermodynamic stability and phase structure of Einstein-Euler-Heisenberg-AdS black holes are studied. We derive the Hawking temperature, Helmholtz free energy, Gibbs potential, entropy and heat capacity of the black holes. We compute the minimum temperature to find that a phase transition may happen at the lowest point. The entropy-temperature diagram consists of two parts. The upper part belonging to the large black holes under the influence from the electromagnetic self-interactions keeps the positive heat capacity, leading the huge compact objects to survive. The lower curves corresponding to small black holes show that the heat capacity of the tiny black holes is negative, which means that the nonlinear-effect-corrected smaller sources will evaporate. The further discussions show that the nonlinear effect modifies the thermodynamic quantities, but the corrections limited by the nonlinear factor μ with allowed values can not change the properties and the phase structure fundamentally and thoroughly. We argue that the influence from self-interaction can not make the Einstein-Euler-Heisenberg-AdS black holes to split under the second law of thermodynamics.
2024, 48(12): 125107. doi: 10.1088/1674-1137/ad73ac
Abstract:
Recent developments in deep learning techniques have provided alternative and complementary approaches to the traditional matched-filtering methods for identifying gravitational wave (GW) signals. The rapid and accurate identification of GW signals is crucial to the advancement of GW physics and multi-messenger astronomy, particularly considering the upcoming fourth and fifth observing runs of LIGO-Virgo-KAGRA. In this study, we used the 2D U-Net algorithm to identify time-frequency domain GW signals from stellar-mass binary black hole (BBH) mergers. We simulated BBH mergers with component masses ranging from 7 to 50\begin{document}$ M_{\odot}$\end{document} ![]()
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Recent developments in deep learning techniques have provided alternative and complementary approaches to the traditional matched-filtering methods for identifying gravitational wave (GW) signals. The rapid and accurate identification of GW signals is crucial to the advancement of GW physics and multi-messenger astronomy, particularly considering the upcoming fourth and fifth observing runs of LIGO-Virgo-KAGRA. In this study, we used the 2D U-Net algorithm to identify time-frequency domain GW signals from stellar-mass binary black hole (BBH) mergers. We simulated BBH mergers with component masses ranging from 7 to 50
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Cover Story
- Cover Story (Issue 12, 2024) | Doubly heavy meson puzzle: precise prediction of the mass spectra and hadronic decay with coupled channel effects to hunt for beauty-charm family
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