怀柔太阳观测基地三通道太阳望远镜局域网内远程观测终端系统设计

利用怀柔三通道太阳磁场望远镜对太阳进行多层次同步观测可以同时获得日面不同层次的活动图像,这对于更好的理解太阳物理有着重要意义.本文基于怀柔三通道太阳磁场望远镜开发了在局域网内能够对三通道CCD进行同步观测的远程终端观测系统,并通过此系统实现了怀柔基地三通道望远镜和小磁场望远镜的协同观测.系统设计采用vc.net集成开发环境,使用TCP/IP协议,通过套接字网络编程,对三通道太阳望远镜的三个CCD进行同步远程控制,目前系统已经在局域网内实现了图像数据和相机控制命令的传输等远程观测功能,大大降低了观测成本,并取得了初步的观测结果.     

Spanish Monitoring of Comets: Making Sense of Amateur Photometric Data

Amateur astronomers have always represented an important observing group in cometary astronomy. Much of our knowledge of cometary light curves has come from amateur data, initially in the form of total visual magnitude estimates and now increasingly in the form of CCD observations. The increasingly widespread use by amateur astronomers of CCD cameras of excellent sensitivity and good cosmetic quality has revolutionised astrometry, allowing far more intensive astrometric monitoring of comets to be carried out down to magnitude 18 and fainter, with a corresponding enormous increase in the quality of calculated orbits. Although amateur CCD photometry is extensively available in the Internet, its use has been less widespread. The reason is the lack of standardisation in the way that this data is taken that leads to amateur CCD light curves having enormous dispersion. All amateur CCD photometry is aperture photometry, but it is seen that neither does it represent well the equivalent of m1 (total visual magnitude), even with a large aperture, nor is it close to the definition of m₂ (the nucleus magnitude). The problem is examined using data from the Spanish Comet Observers Group archives to show that by careful standardisation of data acquisition amateur CCD data can produce high quality, well-sampled and physically meaningful light curves. Examples are presented of the results for recent comets including 19P/Borrelly, 51P/Harrington, C/2001 TU80 (LINEAR-NEAT), C/2000 WM1 (LINEAR) & C/2001 A2 (LINEAR).     

A discussion on the mass loss formulae for OH/IR stars

It is found that the mass loss rate derived from S₂₅/S₁₂ is generally greater than that from the OH flux. This suggests an increasing loss rate with time. It is found that the gas-to-dust ratio decreases during the evolution Of OH/IR stars. An empirical relation between the gas-to-dust ratio and the dust mass loss rate is derived, leading to a formula for calculating the total mass loss rate directly from the IRAS 60 μm flux. OH/IR stars with silicate emission have a larger range of mass loss ratio, from 10⁻⁷ to 10⁻⁵ M/yr; those with silicate absorption, a smaller range between 10⁻⁵ and 10⁻⁴ M/yr. So a large increase in the mass loss rate takes place during the emission phase.     

10m口径射电望远镜天线计算机远程控制系统

本文从当前天文观测所受自然环境的影响入手 ,提出远程控制观测是解决目前观测所遇到的困扰的好方法 ,并介绍了中科院云南天文台太阳射电组的 1 0m口径抛物面天线的计算机远程控制系统。本文着重讨论了远程控制的实施方案 ,包括天线当前的性能测试、如何安全地做到远程通信、前端控制 (即现场控制 )等问题 ,把TCP/IP协议族原理和Client/Server原理与模糊逻辑控制思想相结合 ,对 1 0m口径天线实施自动控制 ,并开发了用于现场控制、远程控制的网络控制软件。     

COSMIC计划

为了获得足够多的地面掩星点资料，用于全球和局部天气预报和大气研究，1997年中国台湾地区和美国联合制定了耗资1亿美元的COSMIC（Constellation Observing System for Meteorology，Ionosphere and Climate)计划。COSMIC是气象、电离层和气候星座观测系统，它包括卫星、地面数据接受和卫星控制站、数据分析中心和数字通讯网络，计划于2005年开始实施。介绍了COSMIC计划产出的历史背景、科学任务及其整个系统的组成，并针对COSMIC和其它LEO（低地球轨道）星座计划，提出了我们应做和正在做的研究工作。     

新一代天文用CCD控制器及将来的设想

介绍了目前世界上两种先进的ＣＣＤ控制器，并提出了新一代天文用ＣＣＤ控制器的设想     

X-ray emission as a tracer of circumstellar matter around herbig ae/be stars

We have detected X-ray emission (1 keV) from young intermediate-mass stars (Herbig Ae/Be stars). Since these stars are not supposed to produce intrinsic X-ray emission (no convection, no coronae), we believe that our results suggest that the X-ray emission actually traces the shock interaction of the Ae/Be star stellar winds with remnant circumstellar matter left over from the star formation process, the presence of which is also indicated by far-infrared (IRAS) and submm/mm continuum data.     

Organizing a professional-amateur collaboration with a Lhires III spectrograph

Amateur spectroscopists are getting organized to contribute to professional astronomy work. We present here the work done within the AUDE association to design, manufacture and distribute the Lhires III high-resolution Littrow spectrograph, which fits usual amateur telescopes and CCD cameras. We also review how the communication is organized through the ARAS distribution list (Spectro-L), forums, and workshops to develop and promote spectroscopic work among amateurs. Last but not least, we introduce the Be stars spectra (BeSS) Virtual Observatory-compatible database and its use for the monitoring of Be stars in association with the COROT satellite.     

海洋潮汐模型在浅海区域的应用

海洋潮汐和大气、海洋、海冰之间存在复杂的相互作用,它对地球气候有复杂而深远的影响。海潮对流经大陆沿岸或大陆架的洋流有很强烈的作用。潮汐流产生混合湍动;潮汐耗散和内潮波效应对海洋环流的传输和循环也有一定的影响。1995年前后,使用TOPEX／POSEIDON测高卫星资料。建立了十多个海潮模型。研究表明,1994-1996年期间发展起来的正压波海潮模型在深海的精度为2—3cm,空间分辨率为50km量级,在浅海区域的精度显著下降。近年来运用更加成熟精细的流体动力学理论模型,在数据同化技术中使用时间跨度更长的测高资料,已经建立了一些改进的海潮模型。该文使用验潮站潮汐常数、测高资料以及交叉点资料,评估了6个海潮模型在浅海区域(包括中国海海域)的表现,以应用于今后对海平面的研究。初步分析表明,浅海区域的海平面高度的误差仍然相当显著。要发展海洋潮汐模型需要进一步减小潮汐混淆效应,提高长周期潮汐的精度,尤其在浅海区域。模型的改进必将增进对潮汐现象的认识,促进学科间进行相互融合和相互渗透的研究(例如潮汐摩擦引起的月球自转的长期缓慢减速、地球内部结构的物理学研究等)。     

长三角地区电离层变化的GPS监测

利用GPS双频观测量可获取电离层总电子含量(Total Electron Content,TEC),以监测区域上空电离层的分布和变化特征,从而可以发现不同尺度的电离层异常。该文采用2004年上海地区GPS综合应用网(SCGAN)以及中国地壳运动监测网络(CMONC)的部分台站的观测,计算得到1年时间序列的TEC数据,来研究长三角地区上空的电离层TEC的变化与活动。应用这些数据,综合利用高斯权函数和滑动平均等几种数据处理方法,重点分析和讨论了长三角地区上空电离层的周日变化、周年变化和季节性变化特性,揭示了电离层冬季异常等现象。同时,通过对1年时间序列TEC进行谱分析,得到了其相应的变化周期。     

Coma Morphology of Three Non-periodic Comets

The coma morphology and short-term evolution was investigated of three non-periodic comets in retrograde orbits, C/2001 Q4 (NEAT), C/2002 T7 (LINEAR), and C/2003 K4 (LINEAR). All three comets display distinct coma features, which were very different from one comet to the next and remained rather constant in shape during the observational period. A single, broad feature perpendicular to the sun-tail direction dominated the coma of C/2003 K4 in all used filters (B,V,R,I), whereas the coma of Comet C/2002 T7 exhibited different features in blue and red filters. C/2001 Q4 showed rather complex coma morphology with clear short-term variability in coma brightness. Therefore, these non-periodic comets neither show a featureless coma nor any similarities of the features detected. The overall distribution of coma material was investigated from the shape of radial coma profiles averaged around the comet nucleus. For C/2001 Q4 and C/2002 T7, the slopes fitted to the linear part of these profiles are flatter in the blue than in the red, which can be explained by the presence of coma gas. For C/2003 K4 no such difference is indicated in the May observations (r = 2.3 AU), while in July (r = 1.7 AU) the profiles in the B-filter are flatter than in V, R, and I, hence gas contamination was relevant at least in the B filter. The R and I filter images were used to determine approximate Afρ values of each comet as a function of time.     

Herbig Ae/Be星的尘埃壳层形态研究

我们使用Kurucz恒星大气模型以及黑体模型对22颗Herbig Ae/Be星的紫外数据、IRAS观测数据、地面光学及近红外测光数据资料等进行了拟合计算,用能量平衡方法进行了统计分析,得出Herbig Ae/Be星的尘埃壳层为盘状的结论.     

Long-Term Stability Of Geoidal Geopotential FromTopex/Poseidon Satellite Altimetry 1993–1999

The TOPEX/POSEIDON (T/P) satellite altimeter data from January 1, 1993to October 24, 1999 (cycles 11–261) was used for investigating thelong-term variations in the geoidal geopotential W₀ and/orin the geopotential scale factor R₀ = GM/W₀ (GM is theadopted geocentric gravitational constant). The mean valuesdetermined for the whole period covered are: W₀ =(62 636 856.161 ± 0.002) m² s^-2, R₀ =(6 363 672.5448 ± 0.0002) m. The actual accuracy is limited bythe altimeter calibration error (2–3 cm) and it isestimated to be about ± 0.5 m² s^-2 (± 5 cm).The yearly variations of the above mean values are at the formalerror level. No long-term trend in W₀, representing the oceanvolume change, was found for the seven years period 1993–9 on thebasis of T/P altimeter (AVISO) data. No sea surface topography modelwas used in the solution. This revised version was published online in July 2006 with corrections to the Cover Date.     

Spin Axis Direction of Comet 19p/Borrelly Based on Observations from 2000 and 2001

We calculate the direction of the rotational angular momentum vector,M, of comet 19P/Borrelly based on rotational lightcurve data from 2000, groundbased imaging of the coma during the Deep Space 1encounter, and the basic near-nucleus coma morphology as revealed by the Deep Space 1 spacecraft. For the most likely direction, we derivea family of solutions (with center at RA = 221°, Dec = -7°) if the direction of M is towards the sunward hemisphere during the Deep Space 1 encounter, whereas if the rotation is of opposite sense, the diametrically opposite family of solutions (with center at RA = 41°, Dec = 7°) would result. We argue that the coma morphology in September 2001 is consistent with the nucleus being a principal axis rotator or one observationally indistinguishable from it. Therefore, for all practical purposes, the direction of the rotational angular momentum vector coincides with the spin axis. We also discuss why the determination of the spin axis direction based on observations from the last apparition is in disagreement with the current result.     

HD 104237,εCha和HD 100546的演化状态

根据Ｈｉｐｐａｒｃｏｓ的资料和ＴＤ－１对εＣｈａ和ＨＤ１００５４６的紫外观测资料讨论了εＣｈａ、ＨＤ１０４２３７和ＨＤ１００５４６在赫罗图上的位置以及它们的演化状态．     

苏梅克－利维9号彗星撞击木星事件的光学观测

本文给出了１９９４年７月１７日至２２日，彗星碰撞期间，福州和乌鲁木齐两个观测点所取得的部分光学观测资料。     

TOPO-EUROPE: The geoscience of coupled deep Earth-surface processes

TOPO-EUROPE addresses the 4-D topographic evolution of the orogens and intra-plate regions of Europe through a multidisciplinary approach linking geology, geophysics, geodesy and geotechnology. TOPO-EUROPE integrates monitoring, imaging, reconstruction and modelling of the interplay between processes controlling continental topography and related natural hazards. Until now, research on neotectonics and related topography development of orogens and intra-plate regions has received little attention. TOPO-EUROPE initiates a number of novel studies on the quantification of rates of vertical motions, related tectonically controlled river evolution and land subsidence in carefully selected natural laboratories in Europe. From orogen through platform to continental margin, these natural laboratories include the Alps/Carpathians–Pannonian Basin System, the West and Central European Platform, the Apennines–Aegean–Anatolian region, the Iberian Peninsula, the Scandinavian Continental Margin, the East-European Platform, and the Caucasus–Levant area. TOPO-EUROPE integrates European research facilities and know-how essential to advance the understanding of the role of topography in Environmental Earth System Dynamics. The principal objective of the network is twofold. Namely, to integrate national research programs into a common European network and, furthermore, to integrate activities among TOPO-EUROPE institutes and participants. Key objectives are to provide an interdisciplinary forum to share knowledge and information in the field of the neotectonic and topographic evolution of Europe, to promote and encourage multidisciplinary research on a truly European scale, to increase mobility of scientists and to train young scientists. This paper provides an overview of the state-of-the-art of continental topography research, and of the challenges to TOPO-EUROPE researchers in the targeted natural laboratories.     

CCD imaging polarimetry of Comet 2P/Encke

We present results and analysis of imaging polarimetric observations of Comet 2P/Encke. The observations were carried out at the 2-m RCC telescope of the Bulgarian National Astronomical Observatory on December 13, 1993 and on January 14, 1994, at phase angles 51.1° and 80.5°, respectively. A wide-band red filter 6940/790 Å was used. This filter is transparent for the continuum and the weak emission bands of NH₂ and H₂O⁺. There is a sunward dust fan with well-defined polarization, which peaks at≈13% in the image obtained on January 14, 1994. Along the sunward fan the degree of polarization decreases progressively. Outside of the fan the coma displays a low polarization of ≈3%. We suggest that this low polarization is caused by the NH₂ emission in the pass-band of the red wide-band filter. Assuming a spherically symmetric NH₂ coma we are able to correct the observed polarization for this effect. The correction leads to an increase of the observed polarization by 1 to 4% at distances 10,000 and 1500 km from the nucleus. A rough estimate shows that the polarization in the near nucleus region of Comet Encke is similar to that for the dusty comets. Even after correction the polarization of Comet Encke's dust fan is significantly less that the polarization observed in dusty comets. The reasons influencing the distribution of dust polarization in the coma are discussed. More polarimetric and colorimetric observations of the dust in Comet Encke on its return in 2003 are needed.     

Photometry and Imaging of Comet C/2000 Wm1 (Linear)

Earth, Moon, and Planets -