宽范围数字化精密频率测量系统的研制

由于奈奎斯特采样定律的限制,传统的数字化精密频率测量设备难以对频率较高的信号进行高精度的精密频率测量.作者研制了一种宽范围数字化精密频率测量系统,能够通过基于频谱分析的粗测过程和基于欠采样的精测过程,克服奈奎斯特定律的限制.实验表明,该宽范围数字化精密频率测量系统对于10 MHz信号的测量(相对)频率偏差为1.13×10-11,测量稳定度达到1×10-12量级.     

光抽运铯原子束频标的二级多普勒频移研究

结合光抽运铯束频标的具体结构,论证了用余弦傅里叶逆变换的方法推导原子速度分布的可行性;用该理论对实验系统测量的Ramsey花样进行了分析,得到铯束管中有效原子真实的速度分布,该速度分布与铯束管的具体结构对速度的要求相一致;通过速度分布精确计算了影响光抽运铯束频标准确度的重要因素——二级多普勒频移,其大小为-3．5×10-13。     

速度分布和银盘厚度效应对正常脉冲星Z向分布的影响

基于彭秋和等1978年得到的无扰动有限厚盘引力势,根据两个引力势参数(h_(z1)= 0．001kpc,h_(z2)=0．325 kpc)和两个速度分布参数(σ_(v1)=115km/s,σ_(v2)=200 km/s)组合的4种情况,对4×10~5颗脉冲星做了三维蒙特卡洛模拟．4×10~5颗脉冲星按着10~8年间隔被分成20组,计算了每组“逃逸”脉冲星所占比例．对每组中“未逃逸”脉冲星,分别在0＜r＜25kpc和5＜r＜11kpc两个区域中对|z|分布做了统计,研究了“未逃逸”脉冲星在这两个区域中的分段标高和累积标高的演化特征．“未逃逸”脉冲星的分段标高在一定空间范围内的变化不规则,但累积标高的变化却比较平滑．在相对长的时间里(＞10~8年),银盘厚度对脉冲星累积标高演化有显著的复杂影响；在相对短的时间中(＜2×10~7年),这种效应很小,而且累积标高对时间的依赖关系是线性的．在长时间里,初始速度分布对累积标高也有显著影响．在引力势h_(z2)=0．325 kpc的条件下,在径向范围5＜r＜11kpc和时间t=9．22×10~6年以及σ_(v2)=200km/s的情况下,模拟的累积标高是0．596±0．005 kpc．     

基于DSP的小型化高精度频标比对系统研制

针对传统双混频时差法测频的局限性,提出了一种差拍数字化精密频率测量方法,基于正弦差拍技术、同步采样技术和数字信号处理技术设计实现了一种新型频标比对系统,可实现对5MHz、10MHz等频标信号的比对测量。实验结果证明,测量10MHz频标信号时系统本底噪声约为1×10^-12／s。系统拥有测量精度高,体积小以及成本低的特点,在时频测量领域具有良好的推广和应用价值。     

天秤座EH光变周期变化新探

我们于1980年5月18、19日及6月15日和1981年1月15日四夜,用高速光电光度计观测了天秤座EHLib,获得6个光度极大时刻。与前人的观测资料综合分析,得出该星的观测极大时刻与计算极大时刻间的差值(O—C)随周期数E的变化,可以定性地表示为其中T_o=H.J.D.2433438.6088,P_o=0.0884132445天,β6.0×10~(-13)天/周-2.4×10~(-9)天/年-2.8×10~(-8)/年,A0.0015天,E_o70700P_o6250天17.1年。假如用双星系统的光时效应来解释其中的正弦项,则双星系统轨道的半长径α近似为0.28天文单位,轨道视向速度峰值投影K=(2παsini)/(E_o)0.45km/s,质量函数f(m)6×10~(-5)M_☉。     

中微子静止质量与Lemaitre模型

本文根据最近关于中微子静质量可能不为零的实验,用Lemaitre模型讨论了中微子静止质量及宇宙年龄对宇宙常数项∧和哈勃常数H_0的限制,并得出了∧的上限∧≤15×10~(-57)/cm~2和H_0的可能范围.     

超新星坍缩与中微子泄漏

本文用简化的中微子泄漏模式代替输运方程，计算超新星坍缩过程中的中微子变化，通过调节模式中的参数可改变中微子的俘陷密度，使之达到较为合适的值，还讨论了在中微子俘陷密度到达之前，特定密度区段（10~(-10)－5×10~(11)g／cm~3）内使电子俘获率有显著变化的一种参数方法及研究结果。     

氢脉泽的壁移实验

本文介绍了用更换五个储存泡的方法进行的氢脉泽壁移实验,这些泡均涂以国产聚四氟乙烯。其实验结果为:K(40℃)=-293±17mHz·cm,α(40℃)=(-17±2)×10~(-3)/℃;并通过罗兰—C长期比对,求得未干扰氢原子基态超精细跃迁频率为f_(0_0)=1420405751.767±0.002Hz。     

GPS BLOCK IIF星载原子钟长期性能分析

星载原子钟长期性能的分析对于系统完好性监测、卫星钟差确定与预报等具有重要的作用.GPS最新型的BLOCK IIF系列卫星于2016年2月6日部署完成.通过星载原子钟的频率准确度、频率漂移率、频率稳定度、观测噪声水平和钟差周期特性这5个指标的长期变化,分析评估了GPS BLOCK IIF星载原子钟的长期性能.计算分析表明:铷钟的频率准确度为7.1×10~(-12)±2.1×10~(-13),频率漂移率为(5.5×10~(-14)±1.1×10~(-14))/d,平均噪声水平约为0.2 ns;铯钟的频率准确度为1.0×10~(-12)±2.9×10~(-15),频率漂移率为(3.4×10~(-15)±5.4×10~(-16))/d,平均噪声水平约为1.0 ns,并且指标变化相对平稳;铷钟的2 h、6 h、12 h和天稳定度分别为3.4×10~(-14)、2.3×10~(-14)、7.3×10~(-15)与6.0×10~(-15);铯钟对应的稳定度指标分别为1.9×10~(-13)、1.1×10~(-13)、7.9×10~(-14)和5.5×10~(-14);卫星钟差存在显著周期项,主周期分别近似为卫星轨道周期的1/2、1倍或2倍.     

小行星Icarus激光测距空间任务科学价值的研究

小行星Icarus激光测距空问任务是在第1566号小行星上放置激光反射器、定时器并与地面站之间进行激光干涉测距,对PPN参数γ和β、太阳四极矩J2、万有引力常数的时间变化率G/G和太阳系天体的质心引力常数进行精确测量.随着激光技术的发展,10ps(用测距量表示是3mm)的计时精度是可以实现的.2015年Icarus与地球接近,为Icarus着陆器提供了良好的发射窗口.本文采用PMOE 2003行星历表框架,从2015年9月25日起,对地面站和小行星之间的激光测距进行了为期800天的模拟,应用Kalmam滤波方法,得到18个参数的不确定度,其中γ,β、J2和G/G的不确定度分别为7.8×10-8、9.0×10-7,9.8×10-11和7.0×10-15yr-1,均高于现有实验的精度1-3个数量级.模拟结果表明,这个空间任务对相对论的检验、太阳系基本参数的测定、以及时空基本定律的检验等都有重要的科学意义.     

A thermodynamic model of high temperature lava vaporization on Io

We modified the MAGMA chemical equilibrium code developed by Fegley and Cameron (1987, Earth Planet. Sci. Lett. 82, 207-222) and used it to model vaporization of high temperature silicate lavas on Io. The MAGMA code computes chemical equilibria in a melt, between melt and its equilibrium vapor, and in the gas phase. The good agreement of MAGMA code results with experimental data and with other computer codes is demonstrated. The temperature-dependent pressure and composition of vapor in equilibrium with lava is calculated from 1700 to 2400 K for 109 different silicate lavas in the ONaKFeSiMgCaAlTi system. Results for five lavas (tholeiitic basalt, alkali basalt, Barberton komatiite, dunite, and a molten type B1 Ca, Al-rich inclusion) are discussed in detail. The effects of continuous fractional vaporization on chemistry of these lavas and their equilibrium vapor are presented. The predicted abundances (relative to Na) of K, Fe, Si, Al, Ca, and Ti in the vapor equilibrated with lavas at 1900 K are lower than published upper limits for Io's atmosphere (which do not include Mg). We predict evaporative loss of alkalis, Fe, and Si during volcanic eruptions. Sodium is more volatile than K, and the Na/K ratio in the gas is decreased by fractional vaporization. This process can match Io's atmospheric Na/K ratio of 10±3 reported by Brown (2001, Icarus 151, 190-195). Silicon monoxide is an abundant species in the vapor above lavas. Spectroscopic searches are recommended for SiO at IR and mm wavelengths. Reactions of metallic vapors with S- and Cl-bearing volcanic gases may form other unusual gases including MgCl₂, MgS, MgCl, FeCl₂, FeS, FeCl, and SiS.     

Instructions for authors

正Research in Astronomy and Astrophysics publishes original research papers and reviews on all branches of astronomy and astrophysics.Reviews are by invitation only.Important new results that require rapid publication can be submitted as a Letter(Letters must be restricted in length to 6 printed pages).Authors who submit a paper are expected to be able to certify that the paper is original work,     

Research in Astronomy and Astrophysics CONTENTS

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Alkali and halogen chemistry in volcanic gases on Io

We use chemical equilibrium calculations to model the speciation of alkalis and halogens in volcanic gases emitted on Io. The calculations cover wide temperature (500-2000 K) and pressure (10⁻⁶ to 10⁺¹ bars) ranges, which overlap the nominal conditions at Pele (T=1760 K, P=0.01 bars). About 230 compounds of 11 elements (O, S, Li, Na, K, Rb, Cs, F, Cl, Br, I) are considered. The elemental abundances for O, S, Na, K, and Cl are based upon observations. CI chondritic elemental abundances relative to sulfur are used for the other alkalis and halogens (as yet unobserved on Io). We predict the major alkali species in Pele-like volcanic gases and the percentage distribution of each alkali are LiCl (73%), LiF (27%); NaCl (81%), Na (16%), NaF (3%); KCl (91%), K (5%), KF (4%); RbCl (93%), Rb (4%), RbF (3%); CsCl (92%), CsF (6%), Cs (2%). Likewise the major halogen species and the percentage distribution of each halogen are NaF (88%), KF (10%), LiF (2%); NaCl (89%), KCl (11%); NaBr (89%), KBr (10%), Br (1%); NaI (61%), I (30%), KI (9%). We predict the major halogen condensates and their condensation temperatures at P=0.01 bar are NaF (1115 K), LiF (970 K); NaCl (1050 K), KCl (950 K); KBr (750 K), RbBr (730 K), CsBr (645 K); and solid I₂ (200 K). We also model disequilibrium chemistry of the alkalis and halogens in the volcanic plume. Based on this work and our prior modeling for Na, K, and Cl in a volcanic plume, we predict the major loss processes for the alkali halide gases are photolysis and/or condensation onto grains. Their estimated photochemical lifetimes range from a few minutes for alkali iodides to a few hours for alkali fluorides. Condensation is apparently the only loss process for elemental iodine. On the basis of elemental abundances and photochemical lifetimes, we recommend searching for gaseous KCl, NaF, LiF, LiCl, RbF, RbCl, CsF, and CsCl around volcanic vents during eruptions. Based on abundance considerations and observations of brown dwarfs we also recommend a search of Io's extended atmosphere and the Io plasma torus for neutral and ionized Li, Cs, Rb, and F.     

Study on the Stressed Mirror Polishing with a Continuous Polishing Machine for Large Aperture Off-axis Aspheric Mirrors

A special stressed annular polishing technique is proposed to mill the off-axis aspheric sub-mirrors of a large segmented mirror with an annular polishing machine. Based on the basic principle of stressed annular polishing technique, a set of special stressing mechanisms are designed to convert milling the aspheric surfaces of sub-mirrors with different off-axis distances into milling the spherical surfaces with identical radii of curvature, so that they can be pol- ished simultaneously on a continuous polishing machine. It took about contin- uous 40 hours to polish a scaled-down mirror of the planning Chinese Future Giant Telescope (CFGT) using this technique. This mirror has the 330 mm di- ameter, 3.6 m off-axis distance, and the 21.6 m radius of curvature, and its max- imum asphericity is 16 micron. The experiment shows that this method has a high effciency, suits batch manufacturing, especially the batch manufacturing of aspheric sub-mirrors of the segmented primary mirror of an extremely large aperture telescope.     

The climatic and physiographic controls of the eastern Mediterranean over the late Pleistocene climates in the southern Levant and its neighboring deserts

Modern-day synoptic-scale eastern Mediterranean climatology provides a useful context to synthesize the diverse late Pleistocene (60–12 ka) paleohydrologic and paleoenvironmental indicators of past climatic conditions in the Levant and the deserts to its south and east. We first critically evaluate, extract, and summarize paleoenvironmental and paleohydrologic records. Then, we propose a framework of eastern Mediterranean atmospheric circulation features interacting with the morphology and location of the southeast Mediterranean coast. Together they strongly control the spatial distribution of rainfall and wind pattern. This cyclone–physiography interaction enforces the observed rainfall patterns by hampering rainfall generation south and southeast of the latitude of the north Sinai coast, currently at 31°15′.The proposed framework explains the much-increased rains in Lebanon and northern Israel and Jordan as deduced from pollen, rise and maintenance of Lake Lisan, and speleothem formation in areas currently arid and semiarid. The proposed framework also accounts for the southward and eastward transition into semiarid, arid, and hyperarid deserts as expressed in thick loess accumulation at the deserts' margins, dune migration from west to east in the Sinai and the western Negev, and the formation of hyperarid (< 80 mm yr^− 1) gypsic–salic soils in the southern Negev and Sinai. Our climatic synthesis explains the hyperarid condition in the southern Negev, located only 200–250 km south of the much-increased rains in the north, probably reflecting a steeper rainfall gradient than the present-day gradient from the wetter Levant into its bordering southern and eastern deserts.At present, the rainiest winter seasons in Lebanon and northern and central Israel are associated with more frequent (+ 20%), deeper Cyprus Lows traversing the eastern Mediterranean at approximately the latitude of southern Turkey. Even these wettest years in northern Israel do not yield above average annual rainfall amounts in the hyperarid southern Negev. This region is mainly influenced by the Active Red Sea Troughs that produce only localized rains. The eastern Mediterranean Cyprus Lows also produce more dust storms and transport higher amounts of suspended dust to the loess area than any other atmospheric pattern. Concurrent rainfall and dust are essential to the late Pleistocene formation of the elongated thick loess zone along the desert northern margin. Even with existing dust storms, the lack of rain and very sparse vegetation account for the absence of late Pleistocene loess sequences from the southern Negev and the formation of hyperarid soils.When the north Sinai coast shifted 30–70 km northwest due to last glacial global sea level lowering, the newly exposed coastal areas supplied the sand and dust to these active eastern Mediterranean cyclones. This enforced the latitude of the northern boundary of the loess zone to be directly due east of the LGM shoreline. This shift of coast to the northwest inhibited rainfall in the southern Levant deserts and maintained their hyperaridity. Concurrently, frequent deep eastern Mediterranean Cyprus Lows were funneled along the northern Mediterranean increasing (probably doubling) the rains in central and northern Israel, Lebanon, southwestern Syria and northern Jordan. These storms and rains formed lakes, forests, and speleothems only a short distance north of the deserts in the southern Levant.     

Active hot star shells

Interferometry in the visible provides milliarcsecond spatial resolution and thus has been used for studying the circumstellar environment of active hot stars. In this paper I will illustrate how the visibility modulus and phase can be used to better constrain the physics of Be disks through results from the VLA, the MkII and the GI2T interferometers. I will insist on the importance and the potential of coupling high angular resolution with high spectral resolution to the study of Be shells. Finally I will present a possible study of the circumstellar disk of Be stars using the VLTI. This revised version was published online in July 2006 with corrections to the Cover Date.     

Fitting X-ray Afterglow Light curves of Gamma-ray Bursts by Using the Magnetar Energy Injection Model

The central compact object for some gamma-ray bursts (GRBs) may be a strongly magnetized millisecond pulsar. It can inject energy to the outer shock of the GRB by through the magnetic dipole radiation, and therefore causes the shallow decay of the early afterglow. Recently, from a large number of GRB X-ray afterglows observed by Swift/XRT(X-ray telescope), it is revealed that many of them exhibit the shallow decay about 10²∼10⁴ s after the burst prompt emission. We have fitted the X-ray afterglow light curves of 11 GRBs by using the energy injection model of a magnetar with the rotation period in the millisecond order of magnitude. The obtained result shows the validity and universality of the magnetar energy injection model in explaining the shallow decay of afterglows, and simultaneously provides some constraints on the magnetic field strength and rotation period of the central magnetar.