This study aimed to investigate the effect of BaF₂ on the radiation-shielding ability of lead telluride glass. A physical radioactive source was used to estimate the mass attenuation coefficient (μ_m) of the 60TeO₂-20PbO-(20-x)ZnO-xBaF₂ glass system (where x = 1,2,3,5,6,7,9 mol%). We tested the μ_m values at seven energies (0.059, 0.081, 0.122, 0.356, 0.662, 1.173, 1.332 MeV). To determine the accuracy of the obtained results, we compared the experimental data with the data calculated using the XCOM software. The experimental values obtained for the selected lead telluride glasses at different concentrations of BaF₂ are in good agreement with the results of XCOM at all energies. The addition of BaF₂ increased the μ_m value of the sample. At the same time, the half-value layer (HVL), mean free path (MFP), effective atomic number (Z_eff), and fast neutron removal cross-section (RCS) of the glass were studied. With the increase in the BaF₂ content, the HVL value and MFP value of the glass decreased, and the Z_eff value and RCS increased, indicating that the addition of BaF₂ enhanced the radiation-shielding performance of the glass.

The tellurite 60TeO₂‐20PbO‐(20‐x)ZnO‐xBaF₂ (x = 1, 3, 5, 6, 7, 9, and 11) series glass samples were prepared. The samples’ SEM, XRD, DSC, density, refractive index, and absorption spectra were tested. A self‐made optical platform was used to measure and calibrate the refractive index. The relationship between glass composition and crystallinity was discussed. The effects of density, molar refractive index, and metal standard value on the refractive index of glass samples were studied. The results showed that TPZBF glass has a high refractive index, and the refractive index increases with the increase in BaF₂ content.

Recent studies have shown that the anisotropy is of great value to decipher cosmic rays’ origin and propagation. We have built a unified scenario to describe the observations of the energy spectra and the large-scale anisotropy and called attention to their synchronous evolution with energy. In this work, the impact of the local regular magnetic field (LRMF) and corresponding anisotropic diffusion on large-scale anisotropy have been investigated. When the perpendicular diffusion coefficient is much smaller than the parallel one, the dipole anisotropy points to the LRMF and the observational phase below 100 TeV could be reproduced. Moreover, we find that the dipole phase above 100 TeV strongly depends on the evolution of local diffusion. But the current measurements at that energy are still scarce. We suggest that more precise measurements at that energy could be carried out to unveil the local diffusion and further the local turbulence.

Cosmic ray (CR) spectra and anisotropy are closely related to the distribution of CR sources, making them valuable probes for studying nearby sources. There are 12 nearby sources located within 1 kpc of the solar system, and which ones are the optimal candidates? In this work, we have selected the Geminga, Monogem, Vela, Loop I, and Cygnus SNR sources as the focus of our research, aiming to identify the optimal candidate by investigating their contribution to the energy spectra and anisotropy using the Spatially Dependent Propagation (SDP) model. Additionally, the anisotropic diffusion effect of the local regular magnetic field (LRMF) on CR particles is also considered in the SDP model. Our previous work only provided 1D anisotropy along the right ascension; this current work will further present 2D anisotropy maps along the right ascension and declination. When the injection power of different nearby sources is roughly equal, the results show that the Geminga, Momogem, and Loop I SNR sources contribute significantly to the nuclear energy spectra. Under the isotropic diffusion without considering the LRMF, the 2D anisotropy maps indicate that the phase points to the nearby source below 100 TeV. We further adjust the injection power of the Monogem SNR source in accordance with the spin-down energy of the Geminga and Monogem pulsars, and find that the contribution of the corrected Monogem SNR can be disregarded. Because the Loop I SNR source is located in the direction of the Galactic Center (GC), it cannot contribute to the excess of CRs in the anti-GC direction. Under anisotorpic diffusion with the consideration of the LRMF, the 2D anisotropy maps show that only the Geminga SNR can match the anisotropy measurement, while the other sources cannot. Finally, we conclude that the Geminga SNR source is the optimal nearby source.

Recent measurements of the spectra and anisotropy of cosmic rays (CRs) show a fine structure that reflects the spectral hardenings of CRs nuclei at the rigidity $\mathcal{R}$ ∼ 200 GV followed by softenings at $\mathcal{R}$ ∼ 10 TV, and reveal complicated energy dependence of the amplitude and phase of anisotropy from 100 GeV to PeV. Numerous studies have shown that the existence of nearby CR sources and a local interstellar magnetic field (LIMF) near the solar system are crucial for such CR spectral and anisotropic patterns. In this work, we analyze the CR spectra of different CR components and the anisotropy considering the nearby Geminga supernova remnants (SNRs) source. In the calculation process, we also introduce the anisotropic diffusion of CRs induced by the LIMF based on the spatial-dependent propagation (SDP) model. As a result, our model can simultaneously account for the CR spectra and the anisotropy from 100 GeV to PeV. Future high-precision measurements of the CR anisotropy, for example, by the LHAASO experiment, would be of the essence in the assessment of our proposed model.

The TIANFU Cosmic Ray Research Center plans to develop the Large Array of Imaging Atmospheric Cherenkov Telescopes (LACT), a large-scale, ultra-high-energy gamma-ray source stereoscopic tracking observation facility. In the LACT project, the SiPM (Silicon Photomultiplier) camera divides 1,616 pixels into 101 sub-modules to facilitate the development, testing, assembly, and maintenance of detector modules. Each module consists of a 4×4 pixel array and a 16-channel Front-End Electronics (FEE) board. The FEE board integrates two primary functions: 1) It shapes and amplifies the analog pulses generated by the SiPM into narrow pulses, performing both high- and low-gain amplification, followed by digital sampling using an ASIC chip developed by IHEP; 2) It provides voltage-temperature compensation for the 16-channel SiPM under varying temperature conditions. The LACT project will require 3,232 FEE boards. This study aims to develop an automated testing platform to efficiently calibrate the analog pulse sampling and temperature compensation sections within the FEE boards.