Colors and collision rates within the Kuiper belt: problems with the collisional resurfacing scenario

We present a numerical check of the collisional resurfacing (CR) hypothesis proposed to explain the observed color diversity within the Kuiper Belt (where surface reddening due to space weathering is counteracted by regular resurfacing of neutral material after mutual collisions). Deterministic simulations are performed in order to estimate the relative spatial distribution of kinetic energy received by collisions, , for a population of target Kuiper Belt objects (KBOs) embedded in a swarm of impactors distributed within the belt. Four different impactor disks have been considered, depending on the excitation and the external limit of the belt and the density of the scattered KBOs (SKBOs) population. The obtained results are compared to the relative color index distribution within the observed Kuiper Belt, in order to derive possible similarities between the high vs low objects spatial distribution in our simulations and the bluer vs redder KBOs distribution in the “real” Kuiper Belt. Such similarities are found for several important features, in particular the general correlations between highly impacted objects and high rms excitation and low perihelion q values that are in good agreement with equivalent correlations found for the bluest objects of the observed belt. Nevertheless, simulations disagree with observations on two crucial points. (1) The plutinos are significantly more collisionally affected than the rest of our test KBO population, whereas there is no observed tendency toward bluer plutinos. (2) There is always a much stronger correlation between and eccentricities than inclinations, whereas observations show just the opposite feature. The presence of numerous SKBO impactors could significantly damp these problematic features, but cannot erase them. Whether these contradictions invalidate the whole CR scenario or not remains yet uncertain, since the physical processes at play are still far from being fully understood and the sample of available observational data is still relatively limited. But it seems nevertheless that the scenario might not hold in its simple present form.     

用神舟三号中分辨率成像光谱仪数据反演大气水汽

2002年3月中国神舟三号飞船发射成功，所携带的中分辨率成像光谱仪获取了一批940nm波段的遥感数据。本文用其中的部分资料做了反演水汽的试验，给出一些结果和分析。     

基于约束条件的地图目标移位

地图目标移位是地图综合和空间信息可视化研究中的一个重要问题,其难点是如何在移位过程中满足一定的约束条件以保持目标之间的空间关系。本文以城市道路扩张为例,借助带约束性Delaunay三角网,结合有限元和空间推理方法,重点探讨顾及空间关系的基于约束条件的地图目标移位问题,并给出满足一定约束条件下的节点移位算法和计算实例。     

2005年10月8日巴基斯坦7.8级地震热红外异常

收集了2005年巴基斯坦7.8级地震区Noaa17/AVHRR的2004-2005年的热红外遥感资料,并进行地表温度反演,得到了以震中为中心7°×7°范围的地表温度值。经热红外图像解译与构造关系对比分析,表明热红外解译图像与构造分布具有一致性。震源区地表温度时间序列显示:震前大约3个月内震源区存在明显的热红外异常。     

可液化地基土三维地震响应分析

编制完全耦合的三维排水有效应力动力反应分析程序，对可液化地基进行三维地震响应分析，探讨了不同土性参数、不同土层构成和不同附加压重等因素对可液化地基抗液化性能的影响。结果表明：在地震荷载作用下，天然饱和砂土地基中的超孔隙水压力随深度的增大而增大；在不同深度处，超孔压峰值到达的时刻比地震加速度峰值到达的时刻要晚；随输入地震加速度的减弱，深层处的超孔压开始消散或基本保持不变，浅层处的超孔压保持不变或略有上升，这一现象与土性参数、输入地震荷载的情况等因素有关；土性参数对土体本身的抗液化性能有重要影响，初始孔隙比越小，相对密度越大，土体的抗液化能力越强；附加压重有利于地基抗液化能力的提高；随着附加压重的增大，超孔压比减小；附加压重对地基中超孔隙水压力的增长有明显的抑制作用。     

地震活动热红外异常的影响因素分析

对地表热红外辐射的基础理论和各类地物的热红外辐射特性进行了简略介绍;对地形地貌、地物类型和气象等非震因素对地表热红外辐射的影响及地表热红外亮温的时空变化特征进行了详细的分析;对各类非震因素的去除方法进行了探讨。初步认为,充分研究活动构造区带在各类非震因素影响下的热红外影像特征,掌握无震条件下的红外亮温时空演化过程,建立红外亮温变化的基准模型及各类非震因素的扣除模型,将有可能较好地排除非震因素的影响,检测出与地震活动有关的热异常。     

网络中移动对象的二维时空索引

基于2DSTMON(2-Dimensional spatio-temporal indexfor moving objects in network)二维时空数据模型,提出了一种新的二维网络中移动对象的时空索引2DSTI及其时空查询算法。这种二维时空索引机制简单且易于实现,支持当前轨迹数据和历史轨迹数据的大量时空查询操作。在此基础上,通过实验实现并验证了二维时空索引机制及其时空查询算法。     

The clustering of K∼20 galaxies in 17 radio galaxy fields

We investigate the angular correlation function, ο(θ), of the galaxies detected in the 2.1-μm K ' band in 17 fields (101.5 arcmin² in total), each containing a z ∼1.1 radio galaxy. There is a significant detection of galaxy clustering at a limit of K ∼20, with a ο(θ) amplitude similar to that estimated by Carlberg et al. at K =21.5. The ο(θ) amplitudes of these K -limited samples are higher than expected from the faint galaxy clustering in the blue and red passbands, but consistent with a pure luminosity evolution model if clustering is stable (ε=0) and the correlation function of early-type galaxies is steeper than that of spirals.
We do not detect a significant cross-correlation between the radio galaxies and the other galaxies in these fields. The upper limits on the cross-correlation are consistent with a mean clustering environment of Abell class 0 for z ∼1.1 radio galaxies, similar to that observed for radio galaxies at z ∼0.5, but would argue against an Abell class 1 or richer environment. As Abell 0 clustering around the radio galaxies would not significantly increase the ο(θ) amplitude of galaxies in these fields, stable clustering with a steep ξ( r ) for E/S0 galaxies appears to remain the most likely interpretation of the ο(θ) amplitude.
At K ≤20, the number of galaxy–galaxy pairs of 2–3 arcsec separation exceeds the random expectation by a factor of 2.15±0.26. The excess of close pairs is comparable to that previously reported for R -band data, and consistent with a ∼(1+ z )² evolution of the galaxy merger rate.     

Infrared Observations of Comet Hale–Bopp (C/1995 O1) from Gurushikhar Observatory

During the recent apparition of comet Hale—Bopp (1995 O1) near infrared photometric observations were carried out in the J, H, K filter bands and also in the 3.0—3.4 μm region at the 1.2 m telescope at Gurushikkar, India. The effective temperature of the comet was substantially higher than the equilibrium blackbody temperature. A mean superheat value of 1.83 was derived in the post-perihelion phase which implies that a large fraction of the grain population are made up of small and hot grains with radii <0.5 μm. High albedo values of ∼0.4 were also derived in the scattering angle range 135° to 160° which could explain the unusual brightness of comet Hale—Bopp. This revised version was published online in July 2006 with corrections to the Cover Date.     

AGN Detection Ranges of MACE and TACTIC Imaging Gamma-Ray Telescopes

Two high-sensitivity imaging gamma-ray telescopes, MACE and TACTIC, are being set up at Mt. Abu, India, for making detailed spectral and temporal investigations of galactic and extragalactic gamma-ray sources in the photon energy bands. E 20–200 GeV and 0.5–5TeV respectively. Here, we estimate the effective red-shift ranges of these telescopes for detecting gamma-ray signals from the EGRET-detected AGN's and identify the most likely candidate-sources for detection by the MACE and the TACTIC, under the assumption that the EGRET-inferred power-law spectra for these AGN's extend into the GeV-TeV range without any change in shape. Extremum bounds of the relevant intergalactic background radiation fields, suggested by various observational and theoretical considerations, have been used to estimate the attenuation of VHE gamma-ray fluxes due to photon-photon pair-production process, leading to the desired z-ranges for these instruments.