对地方电视台转播CCTV时延的测定

讲述了同步广播卫星电视时间信号的测量方法和测量结果，获得了ＣＣＴＶ、ＣＣＴＶ２通过同一颗卫星（亚太－１Ａ）转播的时延差值为１６３．３３μｓ，测量精度在１０ｎｓ以内；ＣＣＴＶ２、ＣＣＴＶ４分别经两颗卫星（亚太－１Ａ，亚洲－Ⅱ）转播，在陕西天文台卫星地面接收站时延差值为１６４４．２０μｓ，严谨为５０μｓ，并分析了影响时延差值和精度的原因，同时测量了地方电视台转播亚太－１Ａ的ＣＣＴＶ信号与直接接收亚太－     

同步广播卫星电视中秒信号的测量结果及其分析

简单介绍了国家授时中心的卫星电视比对系统,给出了利用时间比对系统测量CCTV信号中插入的时间信号(它们或仅由卫星转发或由卫星转发后再经地方电视台转播)时延的方法和测量结果,并对其进行了分析,对定时用户具有参考价值。     

三站时差法荧光屏卫星(714MHz)定位及时刻同步

利用同步的三个地面站,同时接收荧光屏卫星(714MHz)的信号,由卫星信号至各地面站的传播时延差,计算出卫星的位置,定位精度在0.1以内。国内任何接收点,接收卫星信号并作卫星位置的时延修正,则与陕西天文台时刻同步误差小于5μs(1σ)。     

基于伪随机码的低压电力线信道时延测量技术研究

提出了一种基于伪随机码的低压电力线信道时延测量方法,是低压电力线授时的关键技术,利用现有的低压电力线网络,无需搭建额外的通信线路,不受外界物体遮蔽或天气影响。根据双向时间同步原理:服务器首先与标准时间同步,使用BPSK调制方式将1号C/A码经低压电力线传输至客户端,客户端对1号C/A码信号解调捕获后回传服务器2号C/A码,服务器根据信号发射时刻和接收时刻时间差计算出信道传输时延。实验表明:该方法可以用于低压电力线信道的时延测量,在80 m电力线距离内,时间同步误差优于100μs。     

低频时间信号周期修正项的扣除和时延、场强的色散修正

本文从理论上说明用定时接收机接收低频时间信号进行台站时间同步时周期修正项是30.18(≈30.2)μs而不是30μs;说明在—定的条件下脉冲色散对信号时延和场强测量的影响。导出定时信号色散影响不能忽略时场强和时延的修正公式。     

直播卫星(714MHz)信号至两地面站传播时延差的测定

位于东经99°赤道上空的直播电视卫星(714MHz)是静止轨道的同步卫星,陕西天文台和北京天文台合作,同时接收卫星的电视信号,提取规定的某行同步脉冲,记录本地原子钟的秒信号与该脉冲的时刻差,并且利用Loran-C长波定时信号使两天文台的原子钟同步,对卫星比对结果作钟差修正,从而获得卫星信号至两地面站的传播时延差。初步结果表明:卫星信号至陕台、北台的时延差变化范围是60μs,用二次曲线分段拟合,标准偏差(10)在1μs左右。这结果对于卫星定位、研究静止卫星轨道的运动及初步的时刻同步是有意义的。     

双向不对等几何路径对卫星双向时间频率传递的影响

分析了在卫星双向时间频率传递中,由地面站间钟差和卫星运动引起的双向几何路径不对等导致的双向几何路径时延差对双向时间比对计算结果的影响。选取了3颗卫星（中卫1号、北斗3G、IGSO70）和3组地面站（北京-成都、北京-喀什、北京-三亚）组成的9条卫星双向时间频率传递链路作仿真计算。对于这9条链路,仿真结果显示：1）当两地面站间钟差在1μs～10 ms范围内时,通过GEO卫星比通过IGSO卫星的双向不对等几何路径时延之差对双向时间比对计算结果的影响（τ值）较小;2）假设地面站间钟差在1 ms内时,通过 GEO卫星的卫星双向时间比对链路所对应的τ值均在皮秒量级,一般可忽略;通过 IGSO 卫星的卫星双向时间比对链路所对应的τ值均在纳秒量级,一般不可忽略。     

荧光屏电视广播卫星的初步定位及卫星时刻同步

利用三个地面站同时接收卫星电视信号,分离出Line—319同步脉冲,并记录本地钟与分离脉冲的时刻差。在三个地面站时钟同步的情况下,可得卫星信号至各地面站的传播时延差;在假定地心距为常数的情况下,解算出卫星的位置。确定卫星经纬度,国内任何可接收卫星信号的地方,通过卫星与陕西天文台标准时刻同步的均方误差小于±3.5μs     

非坐标方法确定卫星时间信号的传递时延

在卫星电视授时系统方案中，为确定标准秒信号从发射站经卫星到用户接收站的传播时延值，需要知道收、发地面站及卫星的坐标，所以，在高精度的卫星电视授时系统中，需要建立高精度的同步卫星定位同。本文提出在没有卫星定位同的条件下，用非坐标方法来确定卫星时间信号到用户的传递时延，其授时精度为几μｓ。     

非坐标方法确定卫星时间信号的传递时延

在卫星电视授时系统方案中，为确定标准秒信号从发射站经卫星到用户接收站的传播时延值，需要知道收，发地面站及卫星的坐标，所以，在高精度的卫星电视授时系统中，需要建立高精度的同步卫星定位网。本文提出在没有卫星定位网的条件下，用非坐标方法来确定卫星时间信号到用户的传递时延，其授时精度为几μｓ。     

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,     

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.     

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.     

Born–Infeld type phantom model in the ω–ω′ plane

In this paper, we investigate the dynamics of Born–Infeld (B–I) phantom model in the ω–ω′ plane, which is defined by the equation of state parameter for the dark energy and its derivative with respect to N (the logarithm of the scale factor a). We find the scalar field equation of motion in ω–ω′ plane, and show mathematically the property of attractor solutions which correspond to ω _φ ∼−1, Ω _φ =1, which avoid the “Big rip” problem and meets the current observations well.      

Shear and vorticity in a combined Einstein-Cartan-Brans-Dicke inflationary lambda-Universe

A combined BCDE (Brans-Dicke and Einstein-Cartan) theory with lambda-term is developed through Raychaudhuri’s equation, for inflationary scenario. It involves a variable cosmological constant, which decreases with time, jointly with energy density, cosmic pressure, shear, vorticity, and Hubble’s parameter, while the scale factor, total spin and scalar field increase exponentially. The post-inflationary fluid resembles a perfect one, though total spin grows, but the angular speed does not (Astrophys. Space Sci. 312: 275, 2007d).