Radio identification and continuum spectra of decameter-wavelength sources

The paper describes a method for the radio identification of decameter-wavelength sources based on their continuum spectra and analysis of their coordinates in relatively large error boxes surrounding a specified position on the sky. The distribution of continuum spectra and identifications in other wavelength ranges are analyzed for the resulting radio catalog. Using identifications with the FIRST and NVSS surveys, the statistics of the spectral index-size and spectral index-flux density distributions for steep-spectrum sources have been studied, and a catalog of ultrasteep-spectrum (α相似文献   

Moons' magnetism: from Io's and Ganymede's present magnetic signatures to the ancient lunar dynamo

Intrinsic magnetic fields, corresponding to virtual axial dipole moments of the order of 10²⁰ Am², have recently been evidenced for the Jovian satellites Io and Ganymede. By reviewing the rock magnetic and palaeomagnetic properties together with the history of Io, the hypothesis of a moment due to induced or remanent magnetization of crustal rocks acquired within the ambient Jovian field is clearly eliminated. This demonstration is all the more valid for Ganymede, which experiences a much lower Jovian field. The demonstration of a present dynamo action for these Jovian moons, possibly sustained by Jupiter through tidal heating and background magnetic field, may be an actualistic model for the early lunar history. The hypothesis of a lunar dynamo, active at 3–4 Ga, seems to be strongly supported by this analogy.     

Gravito-electrodynamics and the structure of planetary ring systems

Recent spacecraft observations of the Saturnian and Jovian ring systems have highlighted a plethora of interesting new phenomena associated with those regions containing fine (micron and sub-micron sized) dust. Recognizing that these dust grains, by virtue of being immersed within the planetary magnetospheres, are electrostatically charged to the point that they experience comparable gravitational and electric forces, a new “gravito-electrodynamic” theory has been developed to describe their dynamics. This theory has been successful in explaining all these phenomena in a systematic way. In this review, the basic model and its range of validity are outlined, and its application to the Saturnian and Jovian ring systems are discussed.     

爆破震动灾害主动控制方法研究

在微差爆破工程中,用干扰降震法实现爆破震动灾害主动控制的关键在于确定合理的微差延期时间。由于所使用的普通雷管存在延期误差,设计或选择的延期微差时间往往与实际的有较大出入,影响了微差爆破的效果和顺利实施。确定微差爆破中的实际微差延迟时间对优化微差爆破效果、降低爆破地震效应具有很大的现实意义。用基于小波分析的时能密度法以及信号时-频域转换技术,从实测微差爆破震动信号中分离出各分段震波,通过比较各分段震波在不同延期时间下的叠加效果,得到了微差爆破的较优微差延期时间,实现了爆破震动灾害主动控制。该方法对研究爆破震动效应及其灾害的控制,具有较高的理论和应用价值,为系统开展爆破震动危害控制和预测研究奠定了理论和技术基础。     

Detection of gravitational waves through observations of a group of pulsars

We suggest a new approach to the detection of gravitational waves using observations of a group of millisecond pulsars. In contrast to the usual method, based on increasing the accuracy of the arrival times of pulses by excluding possible distorting factors, our method supposes that the additive phase noise that is inevitably present even in the most accurate observational data has various spectral components, which have characteristic amplitudes and begin to appear on different time scales. We use the “Caterpillar” (Singular Spectral Analysis, SSA) method to decompose the signal into its components. Our initial data are the residuals of the pulse arrival times for six millisecond pulsars. We constructed the angular correlation function for components of the decomposition of a given number, whose theoretical form for the case of an isotropic and homogeneous gravitational-wave background is known. The individual decomposition components show a statistically significant agreement with the theoretical expectations (correlation coefficient ρ = 0.92 ± 0.10).     

A comparative analysis of the integrated radio luminosities of normal and millisecond pulsars

We present the results of a comparative statistical analysis of the integrated radio luminosities of millisecond and normal pulsars and their dependences on other parameters of the pulsars. The analysis is based on our own measurements of the flux densities, spectra, and integrated radio luminosities of the millisecond pulsars, as well as data from the literature used to determine the integrated radio luminosities for 545 pulsars, 50 of them millisecond pulsars. Despite large differences in their periods P, period derivatives $\dot P$ , magnetic fields B, and ages τ, the integrated radio luminosities of the millisecond and normal pulsars and their dependences on other parameters are approximately the same. The integrated radio luminosity depends on the parameter B/P ², which is proportional to the potential difference in the polar-cap gap; this may indicate that the radio energy of pulsars is determined by the energy of primary particles accelerated in the polar-cap gap. Secular decreases in the radio luminosities of both normal and millisecond pulsars were also detected.     

The radius spectrum of solid grains settling in gaseous giant protoplanets

Growth of grains having different initial sizes (10^?3 cm?≤?r ₀?≤?1 cm) has been investigated by coagulation processes inside gas giant protoplanets, formed by disk instability, in the mass range 0.3 to 10 Jovian masses. In doing so, we have determined distribution of thermodynamic variables inside the protoplanets and using the results we have determined growth of the grains having assumed initial sizes. Regarding the transference of heat inside the protoplanets, we have considered the possible two cases of interest, namely convection and conduction-radiation. The results of our calculation show that growth of the grains depends on protoplanetary masses and on initial states of the protoplanets and eventually all the grains having assumed different initial sizes acquire almost the same distribution in the central regions of respective protoplanets in the respective cases.     

Finite Prandtl number 2-D convection at high Rayleigh numbers

Finite Prandtl number thermal convection is important to the dynamics of planetary bodies in the solar system. For example, the complex geology on the surface of the Jovian moon Europa is caused by a convecting, brine-rich global ocean that deforms the overlying icy “lithosphere”. We have conducted a systematic study on the variations of the convection style, as Prandtl numbers are varied from 7 to 100 at Rayleigh numbers 106 and 108. Numerical simulations show that changes in the Prandtl number could exert significant effects on the shear flow, the number of convection cells, the degree of layering in the convection, and the number and size of the plumes in the convecting fluid. We found that for a given Rayleigh number, the convection style can change from single cell to layered convection, for increasing Prandtl number from 7 to 100. These results are important for determining the surface deformation on the Jovian moon Europa. They also have important implications for surface heat flow on Europa, and for the interior heat transfer of the early Earth during its magma ocean phase. Electronic Supplementary Material is available if you access this article at . On that page (frame on the left side), a link takes you directly to the supplementary material. Electronic Supplementary Material is available if you access this article at . On that page (frame on the left side), a link takes you directly to the supplementary material.     

超深孔一次成井微差爆破技术研究

起爆时差是超深孔一次成井爆破设计中的一个重要参数,合理设计起爆时差和起爆顺序,能够达到先起爆炮孔为后起爆炮孔创造良好自由面和补偿空间,实现筒状硐室分层、分段爆破的目的,并能降低围岩震动破坏。为合理选取起爆时差,基于超深孔微差爆破破岩机制,从理论上推导了一次成井预裂爆破延期时间,掏槽孔与相邻辅助孔、同分段辅助孔、相邻分段辅助孔的起爆时差等计算公式;同时提出了自下而上预裂爆破、先上下后中间光面爆破等6种一次成井起爆顺序。在华恒矿-650矸石仓,结合施工条件合理确定起爆时差等爆破参数,形成爆破设计方案。爆破过程中实现了分层、分段爆破,获得了良好的硐室成型,验证了形成的超深孔微差爆破技术是成功的,其结果对类似工程的实施具有一定的参考价值。     

雷管延期误差引起爆破震动叠加问题的遗传算法研究

微差爆破实践中,由于延期雷管通常存在延期误差,不能准确按设计延期时间起爆,导致各分段爆破产生的震动可能发生叠加,引起质点振速超标。尤其是在大规模的微差爆破中,这种因雷管延期误差而产生的震动叠加现象更不容忽视。应用遗传算法对该问题进行了研究,可得到由于雷管延期误差导致震动叠加后的最大可能放大倍数,以此来评价雷管延期误差带来的危害性,可为工程实践中的爆破网路设计和震动控制提供参考。     

石笕岭隧道掘进爆破方案设计

分析了石笕岭隧道短台阶掘进爆破施工中存在的问题，在使用自制简易凿岩平台可实现全断面掘进钻眼条件下，提出了全断面掘进爆破方案。采用工程类比法设计，并通过场试验确定了合理适用的光面爆破参数。探讨了在隧道掘进中，利用非电毫秒差雷管孔外微差接力传爆，扩大起爆雷管使用段数的方法。     

Acceleration of close binaries in supernova explosions

We investigate the orientation of the orbital planes of X-ray binary systems relative to the direction of the additional velocity acquired by the binary in a supernova explosion or as a result of radiative acceleration. In the second case, the acceleration occurs due to X-ray radiation during a stage of intense accretion onto the neutron star, which has an asymmetric magnetic field. Observational consequences that could enable estimation of the role of each acceleration mechanism are discussed. The results are also applicable to binary millisecond radio pulsars, assuming that they have gone through an accretion stage.     

The formation of millisecond radio pulsars in close binary systems

An analysis of the basic parameters of a sample of radio and X-ray pulsars that are members of close binary systems is used to separate them into several families according to the nature of the pulsar companions and the previous evolution of the systems. To quantitatively describe the main parameters of close binaries containing neutron stars, we have performed numerical modeling of their evolution. The main driving forces of the evolution of these systems are the nuclear evolution of the donor, the magnetically coupled and radiation-induced stellar winds of the donor, and gravitational-wave radiation. We have considered donors that are low-mass stars in various stages of their evolution, nondegenerate helium stars, and degenerate stars. The systems studied are either the products of the normal evolution of close binaries with large initial component-mass ratios or result from inelastic collisions of old neutron stars with single and binary low-mass, main-sequence stars in the dense cores of globular clusters. The formation of single millisecond pulsars requires either the dynamical disruption of a low-mass (?0.1M_⊙) donor or its complete evaporation under the action of the X-ray radiation of the millisecond pulsar. The observed properties of binary radio pulsars with eccentric orbits combined with the bimodal spatial-velocity distribution of single radio pulsars suggest that it may be possible to explain the observed rotational and spatial motions of all radio pulsars as a result of their formation in close binaries. In this case, neutron stars formed from massive single stars or the components of massive wide binaries probably cannot acquire the high spatial velocities or rapid rotation rates that are required for the birth of a radio pulsar.     

A 27-Day Period in the Flux of Jovian Electrons at the Earth’s Orbit

Variations in the flux of Jovian electrons near the Earth in two synodic cycles of the Earth–Jupiter system, in 1974–1975 and 2007–2008, are considered. In the 1974–1975 cycle, Jovian electrons were observed by IMP-8 during 13 successive solar rotations; electrons were observed by SOHO during 14 solar rotations during the 2007–2008 cycle. The fluxes of these electrons in each solar revolution experienced variations with a characteristic time scale of ~27 ^d , with the maximum flux near the middle of the rotation. The mean period of the variations does not coincide with the synodic period for the Sun–Earth system, equal to 27.3 ^d . The mean variation periods for the electron fluxes were 26.8 ^d in 1974–1975 and 26.1 ^d in 2007–2008. The detected variations are interpreted as reflecting variations in the structure of the solar wind speed and associated magnetic traps, the confinement time of the electrons in thesemagnetic traps, and the influence of the relative positions of the Earth and Jupiter in space.     

水泥厂球磨机基础切割拆除控制爆破

介绍了基础切割拆除爆破的实践和经验。同时成功地应用了非电毫秒导爆管雷管孔外多级接力扩大雷管起爆段数的方法。     

隧洞开挖重复爆炸荷载作用下围岩累积损伤特性

隧洞毫秒爆破开挖推进过程中,预留岩体在重复爆炸荷载作用下产生不可逆的损伤叠加。而现有的岩体爆破损伤数值模拟基本都是针对单孔装药和单段爆破,很少涉及实际工程中的重复爆炸。基于LS-DYNA程序的用户自定义材料接口,将统计损伤演化模型嵌入到弹塑性本构材料中,模拟圆形隧洞全断面毫秒爆破过程中重复爆炸荷载作用下的岩体累积损伤效应,并考虑地应力对岩体爆破损伤的影响。计算结果表明,围岩损伤范围和损伤程度随重复爆炸荷载次数而增加,在一个爆破进尺内,围岩损伤的临界峰值质点振动速度较单段爆破降低了12%;爆炸荷载作用下,围岩主要表现为拉损伤,围岩地应力对爆破张拉效应起到非常敏感的"抑制"作用,在2¹0 MPa应力水平时,围岩爆破累积损伤范围随着应力增加而明显减小,围岩损伤的临界峰值质点振动速度增加24%10 MPa应力水平时,围岩爆破累积损伤范围随着应力增加而明显减小,围岩损伤的临界峰值质点振动速度增加24%⁵7%。     

Solar millisecond spikes manifest large-and small-scale inhomogeneities of the coronal plasma

A model for the generation of solar millisecond radio spikes via a maser cyclotron resonance is proposed. The model takes into account the large-scale inhomogeneity of the magnetic field and small-scale inhomogeneities of the coronal plasma. The efficiency of the energy transformation from a electron beam into maser radiation is estimated. Appropriate parameters of the magnetic field inhomogeneity and the plasma turbulence are found.     

爆炸荷载下岩石损伤机理及其力学特性研究

基于所建立的反映岩石冲击压缩、拉伸损伤理论模型以及深孔微差爆破数值模拟结果,研究了爆炸载荷作用下岩石损伤演化和破碎规律,分析了岩石的动态力学特性;通过对水平边界条件下爆破破岩物理、力学过程的研究,探讨了深孔微差爆破的作用机制和爆破设计原则。     

塔中地区中晚奥陶世内波、内潮汐沉积

现代海底普遍发育由内波、内潮汐引起的深水牵引流,内波、内潮汐不仅可形成各种厘米级的深水牵引流沉积构造,还可建造千米级的大型沉积物波。这种大型沉积物波既可沿斜坡向下迁移,也可沿斜坡向上迁移。在古代地层记录中已发现各种厘米级的内波、内潮汐沉积单元,但尚未发现内波成因的大型沉积物波。塔中地区中上奥陶统碎屑岩段内发育内波及内潮汐形成的各种牵引流沉积构造单元。通过详细的岩心观察,识别出 4种内波、内潮汐沉积微相类型及 5种基本垂向沉积层序。此外,通过地震剖面分析,在研究区中上奥陶统陆坡相中识别出顺坡向上迁移的大型沉积物波,该沉积物波的特征与现代海底发育的沉积物波的特征类似,运用内波理论可对其成因进行合理的解释。     

Unusual features of the millisecond pulsar 1937 + 21 at 406.9 MHz

Observations of the millisecond pulsar PSR B1937 + 21 acquired in Summer 1997 with the Medicina cross telescope revealed two interesting features: the existence of long-lived microstructures persisting over several minutes, and a close relationship between the pulsar flux and pulse arrival times, due to refraction on a discrete inhomogeneity. The latter effect, though observed earlier at higher frequencies by the Nancay group, is rather peculiar at our low frequency.