恒星形成区GGD12-15的近红外观测

给出恒星形成区GGD12-15的宽波段JHK和窄波段H2v=1-0S(1)近红外成像观测．观测图像揭示了致密的年轻红外星团和与红外源成协的红外星云，并发现了以H2发射结表征的星团外流活动．大多数红外点源在光学波段不可见；对76颗红外点源的JHK′测光结果显示，有32颗具有红外超，其中5颗表现原恒星特征，表明分子云中的恒星形成活动很活跃．以B8光谱型作为大质量星分界，由色星等图估计出大质量星所占星团比例为-10％～26％．GGD12—15星团的K′星等分布的峰值位于15.0mag，并在13．0mag-16．0mag平坦分布；[H—K′]色分布的峰值出现在-0．7mag，在此以上更红的星团成分占70％．在GGD12-15区新发现的氢分子发射结集中在星团中心领域，其空间分布明显与剧烈的恒星形成活动相关；有5个发射结位于分子外流的中心区域，暗示其激发可能与分子外流同源．     

Gaseous Jets in Comet Hale-Bopp (1995 O1)

We report the identification of gas jets in comet Hale-Bopp in OH, NH, CN, C₂ and C₃. This is the first time OH and NH jets without an obvious optical dust jet counterpart have been identified in narrowband comet images. We also confirm the existence of CN jets as reported by Larson et al. (1997) and Mueller et al. (1998). Jet features can be seen in the March and April 1997 datasets, approximately a month before and after perihelion. Our results contribute to the understanding of both the chemical properties of the comet as well as the physical mechanisms necessary to produce these features. This revised version was published online in July 2006 with corrections to the Cover Date.     

Shock temperatures in anorthite glass

Summary. Temperatures of CaAl₂Si₂O₈ (anorthite glass) shocked to pressures between 48 and 117 GPa have been measured in the range from 2500 to 5600 K, using optical pyrometry techniques. The pressure dependence of the shock temperatures deviates significantly from predictions based on a single high-pressure phase. Either a variable specific heat, or the existence of three phase transitions, at pressures of about 55, 85 and 100 GPa and with transition energies of about 0.5 MJ kg⁻¹ each (∼ 1.5 MJ kg⁻¹ total) can explain the shock-temperature data. The proposed phase transition at 100 GPa can possibly be identified with the stishovite melting transition. Theoretical models of the time dependence of the thermal radiation from the shocked anorthite based on the geometry of the experiment and the absorptive properties of the shocked material yield good agreement with observations, indicating that it is not necessary to invoke intrinsic time dependences to explain the data in many cases. Observed time dependences were used to calculate absorption coefficients of the shocked material of from about 2 mm⁻¹ to greater than 24 mm⁻¹– an increasing function of shock pressure. The assumption that the shocked material radiates as a black body is supported by the theoretical model, and by the close agreement between measured and calculated black body spectral radiance as a function of wavelength.     

红外相机CASCAM光学设计

介绍紫金山天文台研制的光学-近红外相机CASCAM（Chinese Academy of Science，CAMera)的光学系统设计．CASCAM相机以红外列阵HAWAII-1和光学CCD为探测器，配备国家天文台兴隆观测站2．16米和1．26米望远镜进行0．4—2．5μm波长范围的成像和偏振成像观测．相机的光学系统由F／9→F／6缩焦系统和Offner反射成像系统构成．优化设计结果表明，光学设计方案已满足天文观测的要求．CASCAM相机在设计上实现了光学-近红外很宽波段的消色差变焦，并在楔形分柬片、常温滤光片轮和折射式焦面摆动技术等方面进行了新的尝试．     

PRIMA for the VLTI – Science

The four main scientific objectives of PRIMA – the Phase-Referenced Imaging and Micro-arc second Astrometry facility for the VLTI – will be described:– extra-solar system characterization with astrometry, to detect planets and evaluate their mass, and imaging of the dust accretion disk,– galactic center study with astrometry(dynamics of the bulge stars) and imaging at 10μm (piercing the gas and dust clouds surrounding the galactic center),– observations of AGNs and other extra-galactic objects, too faint to be observed without PRIMA, for which partial imaging is needed to constrain their structuremodels,– micro-gravitational lensing event resolution (imaging and astrometry of their photo-center) in the Galactic Bulge and Magellanic Clouds, helping to determine directly the lens mass and distance. This revised version was published online in July 2006 with corrections to the Cover Date.     

用CE-318太阳光度计资料研究银川地区气溶胶光学厚度特性

根据CE-318数据,利用Bouguer定律计算了银川地区的大气气溶胶光学厚度,并分析其变化特征。结果表明,该地区大气气溶胶光学厚度具有明显的日变化和季节变化。日变化有4种类型：1)变化相对稳定;2)整体上呈上升的趋势;3)早晚小,中午大;4)早晨09-11时出现峰值,其他时间变化较小。季节变化则是冬、春季节大,秋季次之,夏季最小;春季大气中的主要成分是沙尘,冬季大气的主要成分是人类活动排放的颗粒物,夏季由于降水多,气溶胶数浓度较低,气溶胶光学厚度较小。     

用卫星高光谱数据提取德兴铜矿区植被污染信息

在深入分析研究德兴铜矿矿区植被光谱特征的基础上,利用美国EO-1卫星Hyperion高光谱数据,通过反演表征植物生理状态的光谱特征参数(红边位置和最大吸收深度)变异,提取与污染相关的信息,获取了矿山植被污染生态效应概况,为矿山污染的诊断和监测提供新技术和知识支撑。     

镇江圌山绍隆禅寺“活地”成因

"活地"是宗教的传奇,而由于以往知识与技术的限制以及宗教圣地的"不可侵犯性","活地"也成了大自然的千年未解之谜。通过现场考察和资料调研,明晰了"活地"所在地区的地质构造特征。采用高频率表面波监测、分析技术,通过现场试验,研究了"活地"附近地表浅层岩土体分布情况。采用图像分析技术,经室内试验研究得出了"活地"及周围地区出露岩石的矿物组成。最终,对于"活地"的成因提出以下看法:1.否定了地下深层生长性岩脉诱发"活地"现象的观点;2.膨胀岩及膨胀土吸水膨胀对"活地"的隆升有一定作用,但这不是"活地"的主要诱因;3.提出"活地"是岩石风化作用及特殊地理环境综合作用结果的观点:风化作用使岩体疏松、体积增大,地面隆起;两侧山体运动对其交界处岩石产生挤压作用,为"活地"的持续隆升提供动力源。     

小洋山岛大气气溶胶光学厚度的特征分析

小洋山岛位于上海东南面距海岸线约30km处,四面环海,研究其上空的大气气溶胶光学特性对了解我国东部沿海地区及其近海海域的环境和气候影响等都具有重要的意义。对于近岸海岛的气溶胶光学厚度(AOD)观测,至今国内尚未见这方面的实测资料与分析。本次实验利用2006～2007年连续观测得到的AOD值,分析了AOD的季节变化及其与地面风向、湿度和能见度等气象要素的关系,并给出了气溶胶消光谱。分析发现:小洋山地区AOD具有春季最大,冬季次之,秋季较小的特点,而且在低能见度情况下,气溶胶以大粒子为主;盛行西风时,AOD值增大且大粒子比重增加;AOD与湿度有较好的正相关关系。