对比分析现行国家标准GB/T 31248—2014《电缆或光缆在受火条件下火焰蔓延热释放和产烟特性的试验方法》与欧盟标准EN 50399:2022 Common test methods for cables under fire conditions—Heat release and smoke production measureme...对比分析现行国家标准GB/T 31248—2014《电缆或光缆在受火条件下火焰蔓延热释放和产烟特性的试验方法》与欧盟标准EN 50399:2022 Common test methods for cables under fire conditions—Heat release and smoke production measurement on cables during flame spread test—Test apparatus,procedures,results主要技术差异,相比于国标,欧标关于试验装置的规定更加详细,同时增加了标准电缆试样校准、火焰形状校准、非圆形电缆数量及安装规定等技术内容。针对外径小于或等于5 mm的电缆,分析国标和欧标试样安装方式异同,并给出GB/T 31248—2014修订建议。展开更多
Non-isothermal aging(NIA)is a composite heat treatment process that involves heating aging,cooling aging,and complex solute precipitation sequences.The precipitation behavior and the strengthening and toughening mecha...Non-isothermal aging(NIA)is a composite heat treatment process that involves heating aging,cooling aging,and complex solute precipitation sequences.The precipitation behavior and the strengthening and toughening mechanisms of the 2014 Al alloy during NIA were studied by employing tensile,fatigue crack growth,hardness,and electronic conductivity tests,as well as high-resolution transmission electron microscopy and scanning electron microscopy.The results show that during NIA,theθ′phase exhibits a complex process of nucleation,nucleation and growth,nucleation and growth and coarsening,growth and coarsening,nucleation and growth,and nucleation.NIA treatment imparts a mixed precipitation characteristic on the alloy,which is manifested as coherent precipitates,including GP zones,θ′′phases,small-sizedθ′phases,and semi-coherent or non-coherent precipitates such as large-sizedθ′phases and equilibriumθphases.The simultaneous strengthening and toughening of the NIA-treated 2014 Al alloy is caused by the synergistic effects of the particle-shearing mechanism and Orowan bypassing mechanism.展开更多
SN 2014av is a type Ibn supernova(SN)characterized by the interaction between the SN ejecta and a helium-rich circumstellar medium(CSM).We use the^(56)Ni model,the ejecta-CSM interaction(CSI)model,and the CSI plus^(56...SN 2014av is a type Ibn supernova(SN)characterized by the interaction between the SN ejecta and a helium-rich circumstellar medium(CSM).We use the^(56)Ni model,the ejecta-CSM interaction(CSI)model,and the CSI plus^(56)Ni model to fit the multiband light curves(LCs)of SN 2014av.For the CSI and CSI plus^(56)Ni models,we assume that the CSM is a constant density shell(“shell”)or a steady-state stellar wind(“wind”)with density∝r-2.We find that both the^(56)Ni and CSI models fail to fit the multiband LCs of SN 2014av,while the CSI plus^(56)Ni model can account for the LCs.In the last scenario,the LCs around the peaks were mainly powered by the CSI,while the flattening of the LCs was mainly powered by the radioactive decay of^(56)Ni.For the wind case,the derived mass-loss rate of the progenitor is≈20.5-205.5 M_(⊙)yr^(-1),whose lower limit is significantly larger than the upper limit of normal stellar winds,and comparable the upper limit of hyper-winds.Hence,we suggest that the wind case is disfavored.For the shell case,the best-fitting values of the ejecta,^(56)Ni,and the CSM are2.29 M_(⊙),0.09 M_(⊙),and 5.00 M_(⊙),respectively.Provided the velocity of the CSM shell is 100-1000 km s^(-1),we infer that the shell might be expelled≈0.49-5.20 yr before the SN exploded.展开更多
文摘对比分析现行国家标准GB/T 31248—2014《电缆或光缆在受火条件下火焰蔓延热释放和产烟特性的试验方法》与欧盟标准EN 50399:2022 Common test methods for cables under fire conditions—Heat release and smoke production measurement on cables during flame spread test—Test apparatus,procedures,results主要技术差异,相比于国标,欧标关于试验装置的规定更加详细,同时增加了标准电缆试样校准、火焰形状校准、非圆形电缆数量及安装规定等技术内容。针对外径小于或等于5 mm的电缆,分析国标和欧标试样安装方式异同,并给出GB/T 31248—2014修订建议。
基金supported by the Science Foundation of Hunan Province,China(No.2020JJ5215)Scientific Research Project of Hunan Provincial Department of Education,China(No.21B0594)the Open Fund of Hunan Key Laboratory of Electromagnetic Equipment Design and Manufacturing,China(No.DC202007)。
文摘Non-isothermal aging(NIA)is a composite heat treatment process that involves heating aging,cooling aging,and complex solute precipitation sequences.The precipitation behavior and the strengthening and toughening mechanisms of the 2014 Al alloy during NIA were studied by employing tensile,fatigue crack growth,hardness,and electronic conductivity tests,as well as high-resolution transmission electron microscopy and scanning electron microscopy.The results show that during NIA,theθ′phase exhibits a complex process of nucleation,nucleation and growth,nucleation and growth and coarsening,growth and coarsening,nucleation and growth,and nucleation.NIA treatment imparts a mixed precipitation characteristic on the alloy,which is manifested as coherent precipitates,including GP zones,θ′′phases,small-sizedθ′phases,and semi-coherent or non-coherent precipitates such as large-sizedθ′phases and equilibriumθphases.The simultaneous strengthening and toughening of the NIA-treated 2014 Al alloy is caused by the synergistic effects of the particle-shearing mechanism and Orowan bypassing mechanism.
基金supported by the National Key R&D Program(2024YFA1611700)the National Natural Science Foundation of China(grant Nos.12133003,12494571 and 11963001)supported by the Guangxi Talent Program(“Highland of Innovation Talents”)and Program of Bagui Scholars(LHJ)。
文摘SN 2014av is a type Ibn supernova(SN)characterized by the interaction between the SN ejecta and a helium-rich circumstellar medium(CSM).We use the^(56)Ni model,the ejecta-CSM interaction(CSI)model,and the CSI plus^(56)Ni model to fit the multiband light curves(LCs)of SN 2014av.For the CSI and CSI plus^(56)Ni models,we assume that the CSM is a constant density shell(“shell”)or a steady-state stellar wind(“wind”)with density∝r-2.We find that both the^(56)Ni and CSI models fail to fit the multiband LCs of SN 2014av,while the CSI plus^(56)Ni model can account for the LCs.In the last scenario,the LCs around the peaks were mainly powered by the CSI,while the flattening of the LCs was mainly powered by the radioactive decay of^(56)Ni.For the wind case,the derived mass-loss rate of the progenitor is≈20.5-205.5 M_(⊙)yr^(-1),whose lower limit is significantly larger than the upper limit of normal stellar winds,and comparable the upper limit of hyper-winds.Hence,we suggest that the wind case is disfavored.For the shell case,the best-fitting values of the ejecta,^(56)Ni,and the CSM are2.29 M_(⊙),0.09 M_(⊙),and 5.00 M_(⊙),respectively.Provided the velocity of the CSM shell is 100-1000 km s^(-1),we infer that the shell might be expelled≈0.49-5.20 yr before the SN exploded.
