Cosmic neutrinos of ultra-high energies and detection possibility

The fluxes and spectra of galactic and extragalactic neutrinos at energy 10¹¹–10¹⁹ eV are calculated. In particular, the neutrino flux from the normal galaxies is calculated taking into account the spectral index distribution. The only assumption that seriously affects the calculated neutrino flux atE _v 10¹⁷ eV is the power-like generation spectrum of protons in the entire considered energy region.The normal galaxies with the accepted parameters generate the metagalactic equivalent electron component (electrons+their radiation) with energy density _e8.5×10^–7 eV cm^–3, while the density of the observed diffuse X-ray radiation alone is 100 times higher. This requires the existence of other neutrino sources and we found the minimized neutrino flux under two limitations: (1) the power-law generation spectrum of protons and (2) production of the observed energy density of the diffuse X-an -radiation. These requirements are met in the evolutionary model of origin of the metagalactic cosmic rays with modern energy density _M83.6×10^–7 eV cm^–3.The possibility of experiments with cosmic neutrinos of energyE _v 3×10¹⁷ eV is discussed. The upper bound on neutrino-nucleon cross-section <2.2×10^–29 cm² is obtained in evolutionary model from the observed zenith angular distribution of extensive air showers.In Appendix 2 the diffuse X-and -ray flux arising together with neutrino flux is calculated. It agrees with observed flux in the entire energy range from 1 keV up to 100 MeV.     

On convection in the sun

Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure.     

Diffuse cosmic gamma-ray background in the 28 ke V-4.1 MeV range from Kosmos 461 observations

Diffuse cosmic background and atmospheric gamma-radiation in the range 28 keV-4.1 MeV were studied with a scintillation spectrometer on board of the Kosmos 461 satellite. Separation of the cosmic and atmospheric components was made possible through a reliable determination of the geomagnetic dependences of albedo gamma-radiation: The spectrum of diffuse background in the energy range covered cannot be fitted with a common law. At energies below 400 keV the spectrum follows a power-law $$I = (5.6 \pm 0.5) \times 10^{ - 3} E^{ - (2.80 \pm 0.05)} cm^{ - 2} s^{ - 1} sr^{ - 1} MeV^{ - 1} .$$ Starting from 400 keV, this power-law breaks down; the spectrum revealing a clearly pronounced shoulder. Extrapolation of the power-law spectrum to higher energies shows that the gamma-ray component responsible for the change in the shape of the spectrum is quite strong, becoming predominant in the diffuse background in the range 1–100 MeV. The intensity of excess radiation is maximum in the region of 700–800 keV reaching ～1.8×10^?2 cm^?2s^?1sr^?1 MeV^?1. The shape of the high energy component spectrum of the diffuse background constructed using the data of Kosmos 461 and SAS-2 is in agreement with the hypotheses of the cosmological origin of the radiation.     

Some problems of dynamics of lunar regolith glass particle formation

Various glass particles present in great amounts in lunar regolith and affecting some of its specific physical characteristics (e.g., optical and others) are indicators of surficial processes. The objective of this study has been to analyze possibilities of a particular process to occur on the lunar surface, and the relationship of this process with glass particle formation, on the basis of different estimates. A conclusion is reached that condensation mechanism does not appreciably contribute to the formation of small (10^?1?10 μm) spherical particles of the regolith. Their formation is mainly caused by vibrations and decay of liquid jets in the process of surficial material splashing as a result of lunar surface meteorite bombardment. Large spherical and elongated particle (100–500 μm) formation accompanies liquid spraying due to endogenous events (volcanism, etc.) characterized by significantly lower velocities. Certain notions concerning particle formation mechanisms mentioned in the literature by some authors are shown to be erroneous. This concerns, first of all, the formation of dumb-bells and elongated particles that cannot be the result of rotation but must be formed in the process of jet decay due to linear vibrational processes. Collisions of secondary particles created by meteorite impact are not followed by glass particle formation; only their forms can change from regular to irregular. Equations describing surficial material transformation are given.     

河外H_2O超脉泽辐射

介绍了近年来河外Ｈ２Ｏ超脉泽的主要观测结果。Ｈ２Ｏ超脉泽通常起源于活动星系核中央的拱核盘。它们主要寄生在 Ｓｅｒｆｅｒｔ ２星系或低电离核区。至今为止，已有２０个星系探测到Ｈ２Ｏ超脉泽。脉泽辐射的各向同性光度为１０～６０００Ｌ⊙。所有超脉泽星系显示出核的活动，显然，脉泽是由核活动所产生的射电和Ｘ射线光子或激波来抽运的。Ｈ２Ｏ超脉泽倾向存在于高倾斜度的星系，这使得沿视线上的分子柱密度增高，产生足够大的放大光深。最有可能产生Ｈ２Ｏ超脉泽辐射的星系应有一个包含着射电源的侧向的分子盘以及一个适当的抽运机制。     

基于性能的结构抗风设计理论框架

提出了基于性能的结构抗风设计理论框架,将风压强度划分为4个设计风压等级（弱风压、中风压、强风压及超强风压）,将人体振动舒适度划分为6个等级（无振感、轻微振感、中等振感、烦恼、非常烦恼和无法忍受）、三种振动水平（与人的舒适感相关的振动水平、与人正常工作和操作有关的振动水平、与人的生理健康直接相关的振动水平）。结合不同类别建筑物的性能需求及人体振动舒适度的要求,将结构风振性能水准划分为4种状态（性能健康、性能亚健康、性能病态及性能丧失）,将结构风振性能目标划分为5个等级（A、B、C、D、E）。提出了结构抗风概念设计与计算分析的一般原则,给出了结构性能抗风安全性评价及社会经济评价基本内容的建议。     

含钙铝铁水解聚合产物的矿物学研究Ⅱ:热分解特性

分别以NaOH和Ca(OH)2作为碱化剂,合成了聚合氯化铝铁(PAFCNa,PAFCCa),比较样聚合氯化铝(PACNa,PACCa)、聚合氯化铁(PFCNa,PFCCa),制成低温干燥样进行热分解检测.热重分析证明,PAFCCa中的含水量高,主要是配位水与结晶水.当n(Al)/n(Fe)>5:5后,PAFCCa的含水量平均为42.3%.按Ca6Al2(SO4)3(OH)12·26H2O分子式计算,钙矾石的结构水(含OH水)含量为43.06%,两者含水量相当接近.TG-DTG热分析结果支持XRD对PAFCCa中存在含Ca3Al2(OH)12柱体的类钙矾石结构体的认定.PAFC-Ca根据其DTG曲线上的125℃和180℃两个脱水速率(肩)峰可以判别其中有无钙矾石结构体,以及相对量的多少.     

基于自发地理信息的人行道路信息提取

人类的行为轨迹可快速提取到车辆难以通行的人行道路以及人行道路设施等信息,这些信息是行人LBS的关键性元素,它的完备性程度决定了行人LBS服务质量的高低。本文使用志愿者数据集与百度地图,研究了一整套基于VGI数据的人行道路信息提取方法。通过轨迹数据清洗、道路几何路网提取、人行道路设施的检测与识别3个主要板块实现了人行道路信息的提取。算法在完成道路几何路网信息提取的同时,实现了人行横道、过街天桥、地下通道等道路设施信息的获取。     

基于全球分布的地震观测数据估计0S0模态的特征频率及品质因子

选取2011-03-11日本MW9.3地震后全球地震台站记录的约220 h波形数据,基于一定的判断准则,筛选出质量较高的448个垂向观测数据,采用频域AR方法对0S0模态的特征频率和品质因子进行估值,并以信噪比为权重进行加权平均,得到特征频率f=0.814 658 4±5.3×10-7,品质因子Q=5 586±12。该结果与已有研究成果相比精度更高,有助于约束现有地球介质密度和衰减模型,使其更接近真实地球。     

基于傅里叶级数的中国沿海地区Tm模型精化研究

本文采用中国沿海地区13个探空站2010~2014年实测地表温度T_s与平均温度T_m数据,利用傅里叶级数分析法精化中国沿海地区T_m模型,并将2015年探空站实测T_m数据与精化模型进行对比检验。结果表明,精化模型在T_m探测方面具有更高的计算精度,其计算大气可降水量的误差概率分布趋近于正态分布,具有较强的稳定性。