The Orbital Evolution of Two Sounding Satellites and Analysis of the Accuracy of Orbit Determination

The satellites TC-1 and TC-2 are the two Chinese satellites with great elliptical orbits which are still in orbit around the earth at present. Since the launch the orbits of the two satellites have continuously evolved, which has a certain effect on the orbit determination and prediction precision. The regularities of the orbital evolution of the two sounding satellites are qualitatively and quantitatively analyzed. Under the current tracking mode the corresponding prediction precision of orbit determination is analyzed based on the different stages of the orbital evolution, thereby providing the basis for the adjustment of planning mode by the satellite application departments and the guarantee of normal satellite payload. Finally, the orbital lifetimes of the two satellites are predicted through the trend of the orbital evolution.     

New magnetic field measurements of β Cephei stars and slowly pulsating B stars

We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B‐type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B (hereafter SPB) stars, along with a small number of normal B‐type stars. A weak mean longitudinal magnetic field of the order of a few hundred Gauss was detected in three β Cephei stars and two stars suspected to be β Cephei stars, in five SPB stars and eight stars suspected to be SPB stars. Additionally, a longitudinal magnetic field at a level larger than 3σ has been diagnosed in two normal B‐type stars, the nitrogen‐rich early B‐type star HD 52089 and in the B5 IV star HD 153716. Roughly one third of β Cephei stars have detected magnetic fields: Out of 13 β Cephei stars studied to date with FORS 1, four stars possess weak magnetic fields, and out of the sample of six suspected β Cephei stars two show a weak magnetic field. The fraction of magnetic SPBs and candidate SPBs is found to be higher: Roughly half of the 34 SPB stars have been found to be magnetic and among the 16 candidate SPBs eight stars possess magnetic fields. In an attempt to understand why only a fraction of pulsating stars exhibit magnetic fields, we studied the position of magnetic and non‐magnetic pulsating stars in the H‐R diagram. We find that their domains in the H‐R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence. It is possible that stronger fields tend to be found in stars with lower pulsating frequencies and smaller pulsating amplitudes. A somewhat similar trend is found if we consider a correlation between the field strength and the v sin i ‐values, i.e. stronger magnetic fields tend to be found in more slowly rotating stars (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A Study on the Long-term Spectral Variability of the Black-hole Candidate X-ray Binary Cyg X-1

Using the All-Sky Monitor (ASM, 1.5–12–kev) data of Rossi X-ray Timing Explorer (RXTE) from January 1996 to May 2005, we have made a detailed analysis of the correlation between photon-count rate and spectral hardness ratio HR2 (5–12 keV/3–5 keV) of the black-hole candidate X-ray binary Cyg X-1 in 3 energy bands, namely the A-band (1.5–3 keV), B-band (3–5 keV) and Cband (5–12 keV). By the study on the ASM data of 1-day time scale, we find: (1) When Cyg X-1 is in the soft state, the A-band photon-count rate and hardness ratio HR2 exhibit an anticorrelation, but in B-band and C-band there appears the positive correlation. When Cyg X-1 is in hard state, the photon-count rates in the A,B,C bands are all inversely correlated with the hardness ratio HR2; (2) No matter whether Cyg X-1 is in the soft state or the hard state, the hardness ratios HR2 and HR1 are always positively correlated. In addition, we have analyzed the “dwell by dwell” data of the ASM, and obtained the following interesting results: (1) In the period of MJD = 52600–52760 (while Cyg X-1 is in the hard state), the photon-count rates in the A-band and B-band are inversely correlated with HR2, but in the C-band there appears a relatively strong positive correlation; (2) During the hard state, a clear anticorrelation exists between the hardness ratios HR2 and HR1.     

New doubly-symmetric families of comet-like periodic orbits in the spatial restricted (N + 1)-body problem

For any positive integer N ≥ 2 we prove the existence of a new family of periodic solutions for the spatial restricted (N +1)-body problem. In these solutions the infinitesimal particle is very far from the primaries. They have large inclinations and some symmetries. In fact we extend results of Howison and Meyer (J. Diff. Equ. 163:174–197, 2000) from N = 2 to any positive integer N ≥ 2.      

Observations of the OH Radical in Comet C/1995 O1 (Hale-Bopp) with the Nançay Radio Telescope

We present OH 18-cm observations of comet Hale-Bopp (C/1995 O1) at the Nançay radio telescope. On nucleus and offset position observations allowed us to obtain both OH production rates and quenching radii. The maximum OH production rate was reached around perihelion, at about10³¹ s^-1.     

Novel Analysis of Tadpole and Horseshoe Orbits

A simple analysis of tadpole and horseshoe orbits is performed using a new perturbation technique. The first-order results are presented explicitely, extension to any perturbation order is delineated. This revised version was published online in July 2006 with corrections to the Cover Date.     

单环刺螠soxb基因的克隆及其在幼虫发育中的表达特征

SOXB作为重要的转录因子,参与了动物内胚层分化、消化道形成、神经细胞和感官细胞分化的调控。本研究利用RACE技术克隆了单环刺螠(Urechis unicinctus)2个soxb亚族基因soxb1(Uu-soxb1)和soxb2(Uu-soxb2)的cDNA全长序列,大小分别是1871 bp和2906 bp。在两个推导的氨基酸序列中均包含SOX家族的HMG-box结构和SOXB亚族蛋白特有的Group B homology序列,进化树分析它们分别与SOXB1和SOXB2聚类。原位杂交结果显示,Uu-soxb1和Uu-soxb2为母源表达基因;二者在担轮幼虫中的表达图式存在差异,其中早期担轮幼虫中Uu-soxb1 mRNA广泛分布于虫体中,Uu-soxb2 mRNA则集中于顶纤毛束基部和虫体后部(口后纤毛环之后),中期担轮幼虫中,Uu-soxb2阳性信号主要位于纤毛环及虫体的下半球;而Uu-soxb1 mRNA主要位于虫体下半球;之后的发育中二者的表达位点基本一致,即:晚期担轮幼虫中主要位于虫体后部,体节幼虫和蠕虫状幼虫中主要分布于消化道和体壁处。本研究结果表明,单环刺螠soxb在消化道发育过程中的表达模式与其他已报道动物类似,提示其在消化道发育中具有保守的功能。     

卫星散射计与海面平台所测的风场数据比较

基于南海北部海面PY30-1石油平台气象站测风仪2011年7月19日—2012年9月17日实测的风场数据,分别开展了对卫星搭载的ASCAT和HY-2散射计所测风场数据的比较研究,分析散射计的测风能力(选取的时空窗口为30 min和25 km)。结果表明:在南海北部海域,ASCAT 散射计所测风速和PY30-1石油平台气象站观测风速的均方根误差为2.53 m/s,风向偏差较大,均方根误差为47.87°;HY-2散射计所测风速和PY30-1石油平台气象站观测风速的均方根误差为3.41 m/s,风向的均方根误差为58.66°。分别按低、中和高风速的不同条件将ASCAT和HY-2散射计所测的风场数据与PY30-1石油平台气象站观测的风场数据加以比较可知,ASCAT和HY-2散射计都具有较好的测风能力, 前者所测风速与PY30-1石油平台气象站测风仪观测风速的均方根误差稍小于后者。在150 min和15 km的时空窗口下,ASCAT与HY-2散射计所测风速的均方根误差为0.72 m/s,风向的均方根误差为8.50°。