Primary proton spectrum around the knee deduced from the emulsion-chamber data obtained at Mts. Fuji and Kanbala

We have done extensive Monte Carlo simulations using the new simulation codes of CORSIKA and COSMOS to compare with the gamma-family data obtained at Mts. Fuji (3750 m above sea level) and Kanbala (5500 m above sea level). Then, we estimated the primary proton and helium spectra around the knee energy region using a multiple-layered feed-forward neural network as a classifier of primary particle kind. The selection efficiency of proton-induced family events is estimated to be 82%. The flux value of protons at 2×10¹⁵ eV is (5.5±1.5)×10⁻¹⁴ (m⁻² s⁻¹ sr⁻¹ GeV⁻¹). The result suggests heavy-enriched primary composition around the knee region.     

On gamma radiation from the magellanic clouds and galactic supernova remnants — Possible antiproton sources in the galaxy

Radiation from the Magellanic Clouds is discussed from the point of view of near future possibilities in observational γ-ray astronomy. The γ-ray fluxes expected according to the metagalactic and galactic theories of the origin of cosmic rays are compared. It is shown that the strongest test of the metagalactic hypothesis will be provided by a determination of the ratio of γ-ray fluxes from SMC and LMC. The γ-ray luminosity of a typical young supernova remnant that can generate sufficient antiprotons is estimated. It is shown that such remnants must have a short phase during which they are very powerful γ-ray emitters.     

常梯度声线跟踪中平均声速的改进算法

在对多波束测深常用声线跟踪算法进行分析的基础上,提出了一种改进的声线跟踪算法,即沿声线传播的圆弧路径进行积分来求取层内的平均声速,进而推导了严密的多波束测深波束脚印位置的计算公式。理论推导表明,常用的声线跟踪算法的平均声速是将声线的圆弧传播路径当作对应弧段弦时的改进算法平均声速的近似解。实验表明,改进的声线跟踪算法比常用的声线跟踪算法更严密。     

中山站高频雷达观测结果初步分析

中山站高频相干散射雷达于2010年4月建成投入观测,并加盟SuperDARN雷达观测网,成为我国探测电离层对流的重要手段。首先简要介绍中山站高频雷达的工作原理及工作模式,然后利用该雷达第一年的观测数据,给出了每个波束观测的电离层回波总数随距离和回波强度、多普勒速度及谱宽的分布,以及电离层回波发生率随频率的变化特性。观测结果和射线追踪的模拟计算表明,由于波束指向不同,电波波矢方向与地磁场形成正交条件的区域有所不同,因此会造成不同频率下,不同波束观测的电离层回波发生率的差别。     

一次华北平原大雾天气CINRAD/SA雷达超折射回波的射线追踪分析

为准确分析和识别超折射雷达回波,发挥多普勒天气雷达效益,利用石家庄CINRAD/SA型多普勒天气雷达资料,结合探空实况对2005年11月19—21日华北平原大雾天气过程的超折射回波进行了射线追踪分析。结果表明:华北平原大雾天气有利于大气波导的形成,产生3层模式超折射回波。超折射回波使得雷达的目标视位置与实际位置产生偏差,特别是对雷达测高影响较大。超折射回波一般出现在大雾天气的发展和维持过程中,为进行雷达空间定位和华北平原大雾天气的监测、预报提供新的技术手段和科学依据。     

The sensitivity of the next generation of lunar Cherenkov observations to UHE neutrinos and cosmic rays

We present simulation results for the detection of ultra-high energy (UHE) cosmic ray (CR) and neutrino interactions in the Moon by radio-telescopes. We simulate the expected radio signal at Earth from such interactions, expanding on previous work to include interactions in the sub-regolith layer for single dish and multiple telescope systems. For previous experiments at Parkes, Goldstone (GLUE), and Kalyazin we recalculate the sensitivity to an isotropic flux of UHE neutrinos. We find the published sensitivity for the GLUE experiment to be too high (too optimistic) by an order of magnitude, and consequently the GLUE limit to be too low by an order of magnitude. Our predicted sensitivity for future experiments using the Australia Telescope Compact Array (ATCA) and the Australian SKA Pathfinder (ASKAP) indicate these instruments will be able to detect the more optimistic UHE neutrino flux predictions, while the square kilometre array (SKA) will also be sensitive to all bar one prediction of a diffuse ‘cosmogenic’, or ‘GZK’, neutrino flux.Outstanding theoretical uncertainties at both high-frequency and low-frequency limits currently prevent a reliable estimate of the sensitivity of the lunar Cherenkov technique for UHE cosmic ray (CR) astronomy. Here, we place limits on the effects of large-scale surface roughness on UHE CR detection, and find that when near-surface ‘formation-zone’ effects are ignored, the proposed SKA low-frequency aperture array could detect CR events above 56 EeV at a rate between 15 and 40 times that of the current Pierre Auger Observatory. Should further work indicate that formation-zone effects have little impact on UHE CR sensitivity, observations of the Moon with the SKA would allow directional analysis of UHE cosmic rays, and investigation of correlations with putative cosmic ray source populations, to be conducted with very high statistics.     

Comprehensive study of the drying behavior of Boom clay: Experimental investigation and numerical modeling

This paper presents a thermo‐hydro‐mechanical framework to model the drying behavior of Boom clay. First, the experimental campaign conducted Noémie Prime is briefly presented because it is used to validate the model. The data acquisition and processing is emphasized because of the use of X‐ray microtomography to be able to more accurately compare experimental and numerical strain fields. The different submodels are introduced. Numerical simulations are performed to illustrate the capability of the proposed model to reproduce the observed behavior. Finally, a comprehensive sensitivity study on several key model parameters associated with the water retention curve, and the permeability of the medium, is performed to get a better understanding of the physics behind the coupled model.     

Cosmic-ray positrons: are there primary sources?

Galactic cosmic rays consist of primary and secondary particles. Primary cosmic rays are thought to be energized by first order Fermi acceleration processes at supernova shock fronts within our Galaxy. The cosmic rays that eventually reach the Earth from this source are mainly protons and atomic nuclei, but also include electrons. Secondary cosmic rays are created in collisions of primary particles with the diffuse interstellar gas. They are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy Antimatter Telescope (HEAT) balloon-borne instrument, we have measured the abundances of positrons and electrons at energies between 1 and 50 GeV. The data suggest that indeed a small additional antimatter component may be present that cannot be explained by a purely secondary production mechanism. Here we describe the signature of the effect and discuss its possible origin.