一套小型化杜瓦的机械结构

随着天文实测的发展，对小型化杜瓦出现了一定需求。本文介绍了我们新设计的一套小型化半导体制冷杜瓦，给出了机械设计的要点，可供有兴趣的同行参考。     

液氮杜瓦瓶热力与漏热分析

杜瓦瓶是天文观测中重要的终端设备部件.本文主要采用有限元方法对液氮杜瓦瓶进行热力分析,以确定液氮杜瓦瓶优化设计中注意的问题,并通过对液氮杜瓦瓶各种传热途径的分析,计算出液氮杜瓦瓶的漏热.     

天文用热电制冷杜瓦的一种实现

杜瓦是天文观测终端设备重要的部件。本文总结了我们研制二级热电制冷杜瓦中的一些重要经验 ,其恒温点依不同的系统可以改变 ,方法可供有兴趣的同行参考。试验表明 ,这套系统温控精度能达到± 0 .1℃     

制冷接收机低温杜瓦温度监测系统的研制

从设计、制作和测试方法方面介绍了一种制冷接收机低温杜瓦温度监测系统.主要阐述了低温杜瓦对温度监测系统的要求,根据要求合理设计,涉及到各种器件参数的选择以及布局制板等问题,为高精度温度采集系统的硬件设计提供了理论依据.设计采用多路模拟输入通道即集中采集方式,根据系统的需要划分不同的功能区块进行电路设计.制作完成的温度监测系统先后经调试校准、实验室模拟测试以及安装在乌鲁木齐25m射电望远镜18cm制冷双极化接收机上测试,各项设计功能都能很好地实现,并且运行可靠.     

基于以太网的射电天文制冷接收机的监视系统

制冷接收机是射电望远镜的核心设备,它是否正常工作直接决定望远镜观测的效果。制冷接收机的制冷温度和杜瓦真空度是反映接收机是否正常工作的最重要、最直接的指标之一。因此实现制冷接收机制冷温度和杜瓦真空度的远程实时监控,及时了解接收机是否正常工作对保证射电望远镜正常运行、提高观测效率有重要意义。为乌鲁木齐天文站25m射电望远镜1.3cm制冷接收机研制的一套基于单片机和以太网的数据采集和数据传输的远程监视系统,实现了制冷接收机制冷温度和杜瓦真空度的远程实时监控。该系统采用了美国ATMEL公司生产的8位单片机AVR ATmega16、Microchip Technology公司生产的ENC28J60以及MAXIM公司生产的MAX7219,实现对射电天文制冷接收机制冷温度和杜瓦真空度的数据采集,并利用以太网传输数据实现了远程实时监控接收机的制冷状态。阐述了以太网数据采集及远程监控电路的设计原理及其实现方法。该系统首次在国内大型射电望远镜上实现了对制冷接收机工作状态的远程实时监控,对于保证乌鲁木齐天文站25m射电望远镜1.3cm波段的观测效果有重要作用。     

一种锁相环调频方法在铷原子频标中的应用

为了进一步实现铷原子频标小型化,分析了几种典型的锁相环调频电路及其特点,设计了一种锁相环二进制移频键控2FSK(binary frequency shift keying)调频方案,给出了调频信号的频谱测试结果。该调频方案已成功地应用在小型化数字式铷原子频标中,能够满足小型化铷原子频标的要求。     

铷原子频标小型化发展现状

铷原子频标使用最广泛,小型化是其最重要的发展趋势。微波腔小型化、电子线路数字化以及附加特殊功能是铷原子频标小型化的主要技术手段。相干布居囚禁(CPT)频标是一种可以做到芯片级的新型原子频标。目前相干布居囚禁频标的技术方案有:传统方案,物理系统采用MEMS(micro-electro-mechanical system)[0]技术的方案和整机采用MEMS[0]技术的方案。实现小型化后的原子频标将会迎来蓬勃发展的前景。     

嵌入式TCP/IP协议在接收机杜瓦性能参数监测系统中的应用

介绍了射电天文望远镜接收机杜瓦温度与真空度监测系统的设计,具体讨论了监测系统的硬件结构与嵌入式TCP/IP协议在该系统中的实现.针对目前大量使用8位微控制器的嵌入式系统,硬件主控系统芯片采用ATMEL公司生产的8位单片机ATmega16,网络控制芯片采用美国MICROCHIP公司生产的带SPI接口的独立以太网微控制器ENC28J60,设计实现了低成本、高效率、高稳定性的性能参数监测系统.对该系统进行测试分析、数据比对,测试结果表明该系统能够高效与PC机进行通信,PC机所接收到的温度值与标准数据的误差在±0.3 K范围内,接收到的真空值绝对误差在±10 ubar范围内,能够达到系统设计要求.     

用于锶原子光钟永磁体塞曼减速器设计

研究用于锶原子光钟的永磁体塞曼减速器,根据实验条件计算88Sr原子束塞曼减速器的磁场分布,将起始速度为410 m/s的锶原子减速至50 m/s,经过横向磁场的原子通量为7.9×105.基于永磁体制作的塞曼减速器,可靠性高、体积小、重量轻,磁场分布可调,而且无需高电流和水冷装置,实现了永磁体塞曼减速器的小型化.     

氢原子频标的小型化

小型化是目前氢钟的发展方向之一，氢钟的小型化主要是谐振腔的改进，它的结构尺寸决定了氢钟的最小尺寸和重量，目前要用的小型腔主要有电极负载腔，磁控管腔，介质负载腔和TE111腔，新型的谐振腔虽然减小了体积减轻的重量，但量由于它本身已经很难满中立起振条件，所以在伺服电路上也不同于主动型氢钟，根据电路原理的不同，将小型化的氢钟分为反馈振荡型和被动型，反馈振荡型氢钟使激射器工作在反馈振荡状态，通过正反馈维持激射器振荡，被动型氢钟的激射器工作在振荡阈值之下，其作用与揩振放大器相似。     

G-MODE CLASSIFICATION OF SPECTROSCOPIC DATA

We present the results of the application of the G-mode method to the spectral classification of the icy satellites of the giant planets. G-mode is a multivariate statistical technique for the classification of samples depending on many variables. Here this method is tested on the infrared spectra acquired by the Cassini/VIMS instrument onboard the Cassini spacecraft. This work demonstrates the suitability of automatic spectral classification methods for the study of fair resolution spectra, such as those from VIMS. Our data set is composed by two different kinds of data: observations of point targets (Galilean satellites data) and observations with medium spatial resolution (Phoebe data). In both situations, the G-mode classification performed well. In the first case, of a large number of subpixel observations of the Galilean satellites, through the G-mode it was possible to find statistically meaningful spectral groups of observations. In the case of Phoebe, of some spatially resolved observations, the G-mode classification of␣the infrared spectra of the surface led to several types, dominated by the different illumination geometry of the pixels, because, due to the irregular shape of the satellite, a proper illumination correction was not trivial to apply. Nevertheless, the decrease of the confidence level of the test as well as the re-application of the G-mode on the main type found, led to further types, whose statistical distance can be related to different chemical abundances. We plan to use the G-mode also on the data coming from ongoing and future observations of the icy Saturnian satellites.In the helioseismology literature, G-modes are gravity wave modes of the frequencies of oscillations of the Sun. Here we are dealing with a clustering method, which is essentially different.*E-mail: federico.tosi@rm.iasf.cnr.it     

The Dynamics of Ejecting Stellar Systems

We consider the ejection of one stellar system from the centre of another stellar system, representing both by Plummer models. Using the impulsive appoximation, we derive analytically the overall and differential energy changes and also the mass escape from the systems. We compare the results with those obtained for colliding systems.We find that the disruptive effects are considerably less in the case of ejection. If the ejected system is compact, it escapes with negligible disruptive effects.In the case of ejections, stars are also accelerated in the direction of motion of the system. Using a dimensionless parameter λ defined as the ratio of the squares of the stellar velocity perturbations in the direction of motion of the system and perpendicular to it, we find a significant difference between ejecting systems and colliding systems. In fast head-on collisions of spherical stellar systems, the systems become elongated in the direction perpendicular to the direction of motion whereas in the case of ejecting systems, they also become elongated in the direction of motion. These effects are more pronounced in the outer regions of the smaller system and the innner regions of the bigger system. These effects are enhanced if the ejected system is compact.     

The influence of mergings on galaxy evolution

The evolution of the galaxy mass function MF (and luminosity function LF) depending on merging of galaxies is discussed. The richness and masses of most massive (and most luminous) galaxies of a cluster are chosen as a characteristic of the bright edge of LF. Mergers are simulated by a Monte-Carlo method. The probability of merging depends on the masses of galaxies. The ratio of the current number of galaxies to the initial one plays the role of the time scale. Transformation to real time and redshift is realized with help of the Smoluchowsky kinetic equation (SE) solution, describing the merging process and making possible to find the dependence of the galaxy number on time. The dependencies of richness, masses and magnitude differences of most massive and brightest galaxies of a cluster on redshift have been obtained. Creation of cD-galaxy has been retraced on small redshifts. The masses of the second and less massive cluster galaxies grow, but after the creation of the cD-galaxy they begin to decrease. Comparison of obtained results with data of the catalogues is provided. Correspondence in mentioned dependencies is observed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Optimisation of seismic network design: Application to a geophysical international lunar network

Fundamental scientific questions concerning the internal structure and dynamics of the Moon, and their implications on the Earth-Moon System, are driving the deployment of a new broadband seismological network on the surface of the Moon. Informations about lunar seismicity and seismic subsurface models from the Apollo missions are used as a priori information in this study to optimise the geometry of future lunar seismic networks in order to best resolve the seismic interior structure of the Moon. Deep moonquake events and simulated meteoroid impacts are the assumed seismic sources. Synthetic P and S wave arrivals computed in a radial seismic model of the Moon are the assumed seismic data. The linearised estimates of resolution and covariance of radial seismic velocity perturbations can be computed for a particular seismic network geometry. The non-linear inverse problem relating the seismic station positions to the linearised estimates of covariance and resolution of radial seismic velocity perturbations is written and solved by the Neighbourhood Algorithm. This optimisation study favours near side seismic station positions at southern latitudes in order to constrain the deep mantle structure from deep moonquake data at large epicentral distances. The addition of a far side station allows to divide by two the size of the error bar on the seismic velocity model. The monitoring of lunar impact flashes from the Earth allows to improve the radial seismic model in the top of the mantle by adding much more meteor impact data at short epicentral distances due to the high accuracy of the space/time location of these seismic sources. Such meteor impact detections may be necessary to investigate the 3D structure of the lunar crust.     

Algorithm Analysis of Autonomous Navigation of Spacecraft Based on X-ray Pulsars

A pulsar has the very stable rotation and can be used as the time standard. The astrometric parameters and astrophysical parameters of many pulsars, such as the spatial position, proper motion, distance, rotation period and its derivative, etc., can be all accurately determined. Since the pulsar can provide the time signal and the coordinates of its spatial position simultaneously, the pulsar navigation system installed on a spacecraft enables the autonomous navigation of the spacecraft to be realized. Firstly, the position of the spacecraft is predicted based on the equation of orbit dynamics of the spacecraft and then the Kalman filtering is applied to calculating the estimation error of the spacecraft position through the difference between the pulse arrival time observed on the spacecraft and the predicted pulse arrival time, thereby modifying the position of the spacecraft. Finally, the effects of the initial error, measuring accuracy of the pulse arrival time and number of pulsars on the navigation accuracy are analyzed.     

Averaging on the motion of a fast revolving body. Application to the stability study of a planetary system

Exploring the global dynamics of a planetary system involves computing integrations for an entire subset of its parameter space. This becomes time-consuming in presence of a planet close to the central star, and in practice this planet will be very often omitted. We derive for this problem an averaged Hamiltonian and the associated equations of motion that allow us to include the average interaction of the fast planet. We demonstrate the application of these equations in the case of the μ Arae system where the ratio of the two fastest periods exceeds 30. In this case, the effect of the inner planet is limited because the planet’s mass is one order of magnitude below the other planetary masses. When the inner planet is massive, considering its averaged interaction with the rest of the system becomes even more crucial.     

Relation of Seismic Wave Energy and Magnetic Field Intensity on the Solar Surface

As shown by a series of previous researches, on the solar photospheric surface, together with the intensi?cation of longitudinal magnetic ?eld, the ob- served energy of seismic waves decreases. In order to further investigate the relation between seismic waves and magnetic ?elds, using the data of Helioseis- mic and Magnetic Imager (HMI) and via the extrapolation of the potential ?eld from the line-of-sight magnetic ?eld, we can get the total intensity of magnetic ?eld and correlate it with the energy of seismic waves. By ?tting the energies of p-mode seismic waves within a certain region of total magnetic ?eld, the relation between the energy of seismic waves and the total intensity of magnetic ?eld can be obtained. Our study has con?rmed that between the energy of seismic waves and the total intensity of magnetic ?eld there is a stronger correlation. As shown by the results of various active regions, the tendencies of decrease of the energy of p-mode seismic waves with the total intensity of magnetic ?eld below 500 GS are very close to each other, but in the range from 500 GS to 1000 GS there are small differences. Besides, between the logarithm of the energy of p-mode seis- mic waves and the total intensity of magnetic ?eld there is a rather strong linear correlation. As revealed by comparing the results of Michelson Doppler Imager (MDI) and HMI, although in totality the observational results of magnetic ?elds of MDI are larger than those of HMI, but the results of comparison and analysis on the relation between the normalized energy of p-mode seismic waves and the intensity of magnetic ?eld do not differ much in these two cases.     

Mars

Mars is the fourth planet out from the sun. It is a terrestrial planet with a density suggesting a composition roughly similar to that of the Earth. Its orbital period is 687 days, its orbital eccentricity is 0.093 and its rotational period is about 24 hours. Mars has two small moons of asteroidal shapes and sizes (about 11 and 6 km mean radius), the bigger of which, Phobos, orbits with decreasing semimajor orbit axis. The decrease of the orbit is caused by the dissipation of tidal energy in the Martian mantle. The other satellite, Deimos, orbits close to the synchronous position where the rotation period of a planet equals the orbital period of its satellite and has hardly evolved with time. Mars has a tenous atmosphere composed mostly of CO with strong winds and with large scale aeolian transport of surface material during dust storms and in sublimation-condensation cycles between the polar caps. The planet has a small magnetic field, probably not generated by dynamo action in the core but possibly due to remnant magnetization of crustal rock acquired earlier from a stronger magnetic field generated by a now dead core dynamo. A dynamo powered by thermal power alone would have ceased a few billions of years ago as the core cooled to an extent that it became stably stratified. Mars' topography and its gravity field are dominated by the Tharsis bulge, a huge dome of volcanic origin. Tharsis was the major center of volcanic activity, a second center is Elysium about 100° in longitude away. The Tharsis bulge is a major contributor to the non-hydrostaticity of the planet's figure. The moment of inertia factor together with the mass and the radius presently is the most useful constraint for geophysical models of the Martian interior. It has recently been determined by Doppler range measurements to the Mars Pathfinder Lander to be (Folkner et al. 1997). In addition, models of the interior structure use the chemistry of the SNC meteorites which are widely believed to have originated on Mars. According to the models, Mars is a differentiated planet with a 100 to 200 km thick basaltic crust, a metallic core with a radius of approximately half the planetary radius, and a silicate mantle. Mantle dynamics is essential in forming the elements of the surface tectonics. Models of mantle convection find that the pressure-induced phase transformations of -olivine to -spinel, -spinel to -spinel, and -spinel to perovskite play major roles in the evolution of mantle flow fields and mantle temperature. It is not very likely that the -spinel to perovskite transition is present in Mars today, but a few 100 km thick layer of perovskite may have been present in the lower mantle immediately above the core-mantle boundary early in the Martian history when mantle temperatures were hotter than today. The phase transitions act to reduce the number of upwellings to a few major plumes which is consistent with the bipolar distribution of volcanic centers of Mars. The phase transitions also cause a partial layering of the lower mantle which keeps the lower mantle and the core from extensive cooling over the past aeons. A relatively hot, fluid core is the most widely accepted explanation for the present lack of a self-generated magnetic field. Growth of an inner core which requires sub-liquidus temperatures in the core would have provided an efficient mechanism to power a dynamo up to the present day. Received 10 May 1997