关联指数误差和样本容量     

吴云  周硕愚  孙建中 《大地测量与地球动力学》1994,(1)

根据关联指数的定义，推导了ＧＰ法计算关联指数时的观测数据误差与关联指数误差的关系，导出了任意两个嵌入空间维上关联指数之差的表达式，并提出了一种确定样本容量限的方法。  相似文献   

活动星系的非相对论性外流     

王挺贵 《天文学进展》2001,19(2):232-236

活动星系核有两类常见外流，相对论性的射电喷流和非相对论性的物质外流，前者主要在射电强的适动星系核中，以非热辐射为特征，非相对论性外流主要通过紫外吸收线观测到，总结了类星体非对论性外流的一些性质及其X射线观测给出了的问题，指出现有的观测表明非相对论性外流引起的质量损失很重要。  相似文献   

G359.95-0.04: an energetic pulsar candidate near Sgr A*     

Q. D. Wang  F. J. Lu  E. V. Gotthelf 《Monthly notices of the Royal Astronomical Society》2006,367(3):937-944

We report the discovery of a prominent non-thermal X-ray feature located near the Galactic centre that we identify as an energetic pulsar wind nebula. This feature, G359.95-0.04, lies 1-lyr north of Sgr A* (in projection), is comet like in shape, and has a power-law spectrum that steepens with increasing distance from the putative pulsar. The distinct spectral and spatial X-ray characteristics of the feature are similar to those belonging to the rare class of ram-pressure confined pulsar wind nebulae. The luminosity of the nebula at the distance of Sgr A*, consistent with the inferred X-ray absorptions, is   L_x ∼ 1 × 10³⁴ erg s⁻¹  in the 2–10 keV energy band. The cometary tail extends back to a region centred at the massive stellar complex IRS 13 and surrounded by an enhanced diffuse X-ray emission, which may represent an associated supernova remnant. Furthermore, the inverse Compton scattering of the strong ambient radiation by the nebula consistently explains the observed TeV emission from the Galactic centre. We also briefly discuss plausible connections of G359.95-0.04 to other high-energy sources in the region, such as the young stellar complexes IRS 13 and SNR Sgr A East.  相似文献   

胶东半岛乳山地区低角度韧性剪切带几何学、运动学特征:对中国东部岩石圈减薄作用的启示     

郝志宣  金超  田忠华  李同宇  文飞 《地质科学》2022,57(1):43-60

大规模伸展构造是华北克拉通东部岩石圈减薄的重要表现形式。部分低角度韧性剪切带是地壳伸展变形后所展现的构造形式。本文研究了王格庄韧性剪切带的岩石学、几何学、运动学等特征显示:韧性剪切带走向近南北向,剪切带断层面倾向多变(倾向西、西南、西北方向)。大部分区域面理低角度倾向西,矿物拉伸线理近东西向,不对称旋转碎斑及S-C组构指示顶端指向西的剪切特征。结合研究区西侧与伸展构造相匹配的半地堑伸展盆地证据:本研究认为伸展构造的形成可能与西太平洋板块的后撤相关,即大规模伸展构造作用引发了华北克拉通东部的地壳减薄作用。  相似文献   

Fe(Ⅱ)/针铁矿复合系统对水中橙黄G的吸附-还原脱色研究     

赵丹  肖丹玲  何广平  吴宏海 《岩石矿物学杂志》2015,34(1):97-102

系统研究了Fe(Ⅱ)/针铁矿复合系统对偶氮染料橙黄G(简称OG)的吸附-还原脱色机理,重点考察了反应条件p H值、Fe(Ⅱ)与OG摩尔比对OG还原脱色效果的影响。研究结果表明,矿物表面结合态Fe(Ⅱ)能够有效提高还原脱色反应速率;OG脱色反应非常符合准一级反应动力学方程,速率常数(k)随p H值的升高、亚铁离子吸附量的增加而显著增大;当OG初始浓度为50 mg/L、Fe(Ⅱ)与OG的摩尔比为27.0时,Fe(Ⅱ)/针铁矿复合系统对OG的去除脱色率在弱碱性条件下1 h内可达到100%。该系统对OG去除脱色的高效性是界面吸附与还原协同作用的结果。该研究可为有效应用Fe(Ⅱ)/针铁矿复合系统在缺氧环境中的污染修复提供理论指导。  相似文献   

Shocked molecular hydrogen towards the Tornado nebula     

J. S. Lazendic  M. Wardle  M. G. Burton  F. Yusef-Zadeh  A. J. Green  J. B. Whiteoak 《Monthly notices of the Royal Astronomical Society》2004,354(2):393-400

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INTEGRAL observations of TeV plerions     

A. I. D. Hoffmann  D. Horns  A. Santangelo 《Astrophysics and Space Science》2007,309(1-4):215-219

Amongst the sources seen in very high gamma-rays several are associated with Pulsar Wind Nebulae (“TeV plerions”). The study of hard X-ray/soft gamma-ray emission is providing an important insight into the energetic particle population present in these objects. The unpulsed emission from pulsar/pulsar wind nebula systems in the energy range accessible to the INTEGRAL satellite is mainly synchrotron emission from energetic and fast cooling electrons close to their acceleration site. Our analyses of public INTEGRAL data of known TeV plerions detected by ground based Cherenkov telescopes indicate a deeper link between these TeV plerions and INTEGRAL detected pulsar wind nebulae. The newly discovered TeV plerion in the northern wing of the Kookaburra region (G313.3+0.6 powered by the middle aged PSR J1420-6048) is found to have a previously unknown INTEGRAL counterpart which is besides the Vela pulsar the only middle aged pulsar detected with INTEGRAL. We do not find an INTEGRAL counterpart of the TeV plerion associated with the X-ray PWN “Rabbit” G313.3+0.1 which is possibly powered by a young pulsar.  相似文献   

3G通信技术在移动气象视频会商咿的研究与应用     

苏轶  刘树峰  孟令旺  马骏 《气象与环境科学》2012,35(1)

目前山东省气象部门已有多部移动气象台投入业务使用,在防御气象灾害和突发气象事件应急服务中发挥了重要作用。由于移动气象台通信（通过通信卫星连接互联网和气象局内音旷网）费用高,且需提前向运营商申请增加宽带以满足视频会商需求,因此提出了利用3G通信技术,建立VPDN网络访问气象局内部网络,来实现移动气象台和济南市气象台视频会商的方案。该方案的应用,大大降低了移动一气象台的通信费用,提高了传输效率。  相似文献   

Wind-swept clouds and possible triggered star formation associated with the supernova remnant G357.7+0.3     

J. P. Phillips  G. Ramos-Larios  J. A. Perez-Grana 《Monthly notices of the Royal Astronomical Society》2009,397(3):1215-1227

We present evidence for interaction between the supernova remnant (SNR) G357.7+0.3 and nearby molecular clouds, leading to the formation of wind-swept structures and bright emission rims. These features are not observed at visual wavelengths, but are clearly visible in mid-infrared mapping undertaken using the Spitzer Space Telescope . Analysis of one of these clouds, the bright cometary structure G357.46+0.60, suggests that it contains strong polycyclic aromatic hydrocarbon emission features in the 5.8 and 8.0 μm photometric bands, and that these are highly variable over relatively small spatial scales. The source is also associated with strong variations in electron density; a far-infrared continuum peak associated with dust temperatures of ∼30 K; and has previously been observed in the 1720 MHz maser transition of OH, known to be associated with SNR shock excitation of interstellar clouds. This source also appears to contain a young stellar object (YSO) within the bright rim structure, with a steeply rising spectrum between 1.25 and 24 μm. If the formation of this star has been triggered recently by the SNR, then YSO modelling suggests a stellar mass  ∼5–10 M_⊙  , and luminosity   L _YSO∼10²–2 × 10³ L_⊙  .
Finally, it is noted that a further, conical emission region appears to be associated with the Mira V1139 Sco, and it is suggested that this may represent the case of a Mira outflow interacting with a SNR. If this is the case, however, then the distance to the SNR must be ∼half of that determined from CS   J = 2–1  and 3–2 line radial velocities.  相似文献   

Excursion to Woldingham: Saturday,May 6th, 1905     

N.F. Robarts 《Proceedings of the Geologists' Association. Geologists' Association》1905,19(3):133-135

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