河南省强对流天气诊断分析预报系统

强对流预报是天气预报的难点,为了提高预报强对流、特别是预报区域性强对流天气的预报能力,应用河南省1995—2004年的气象观测资料作分析样本,并计算多个大气动力和热力学参数。经过统计分析、诊断分析,选择预报能力强、指示性好的大气动力或热力学参数作为强对流天气的预报因子,采用加权集成建立预报方程。应用计算机技术自动实现从数据采集、物理参数计算、预报因子临界值判别、诊断预报方程运算,到以MICAPS图形方式输出预报结果,建立了河南省区域强对流天气预报系统。该系统为预报员提供了一种科学客观的参考依据,在近两年的业务运行中取得了比较理想的预报效果,提升了河南省强对流天气的预报能力。     

Multiwavelength study of X-ray selected star-forming galaxies within the Chandra Deep Field-South

We have combined multiwavelength observations of a selected sample of star-forming galaxies with galaxy evolution models in order to compare the results obtained for different star formation rate (SFR) tracers and to study the effect that the evolution of the star-forming regions has on them. We also aimed at obtaining a better understanding of the corrections due to extinction and nuclear activity on the derivation of the SFR. We selected the sample from Chandra data for the well studied region Chandra Deep Field -South (CDFS) and chose the objects that also have ultraviolet (UV) and infrared (IR) data from Galaxy Evolution Explorer ( GALEX ) and Great Observatories Origins Deep Survey (GOODS) Spitzer , respectively.
Our main finding is that there is good agreement between the extinction corrected SFR(UV) and the SFR(X), and we confirm the use of X-ray luminosities as a trustful tracer of recent star formation activity. Nevertheless, at SFR(UV) larger than about  5 M_⊙ yr⁻¹  there are several galaxies with an excess of SFR(X) suggesting the presence of an obscured active galactic nucleus (AGN) not detected in the optical spectra. We conclude that the IR luminosity is driven by recent star formation even in those galaxies where the SFR(X) is an order of magnitude higher than the SFR(UV) and therefore may harbour an AGN. One object shows SFR(X) much lower than expected based on the SFR(UV); this SFR(X) 'deficit' may be due to an early transient phase before most of the massive X-ray binaries were formed. An X-ray deficit could be used to select extremely young bursts in an early phase just after the explosion of the first supernovae associated with massive stars and before the onset of massive X-ray binaries.     

Cepheid parallaxes and the Hubble constant

Revised Hipparcos parallaxes for classical Cepheids are analysed together with 10 Hubble Space Telescope ( HST )-based parallaxes. In a reddening-free V , I relation we find that the coefficient of log  P is the same within the uncertainties in our Galaxy as in the Large Magellanic Cloud (LMC), contrary to some previous suggestions. Cepheids in the inner region of NGC 4258 with near solar metallicities confirm this result. We obtain a zero-point for the reddening-free relation and apply it to the Cepheids in galaxies used by Sandage et al. to calibrate the absolute magnitudes of Type Ia supernova (SNIa) and to derive the Hubble constant. We revise their result for H ₀ from 62 to 70 ± 5 km s⁻¹ Mpc⁻¹. The Freedman et al. value is revised from 72 to 76 ± 8 km s⁻¹ Mpc⁻¹. These results are insensitive to Cepheid metallicity corrections. The Cepheids in the inner region of NGC 4258 yield a modulus of 29.22 ± 0.03 (int.) compared with a maser-based modulus of 29.29 ± 0.15. Distance moduli for the LMC, uncorrected for any metallicity effects, are 18.52 ± 0.03 from a reddening-free relation in V , I ; 18.47 ± 0.03 from a period–luminosity relation at K ; 18.45 ± 0.04 from a period–luminosity–colour relation in J , K . Adopting a metallicity correction in V , I from Macri et al. leads to a true LMC modulus of 18.39 ± 0.05.     

Correlations among color,morphology, and luminosity for the luminous red galaxy (LRG) sample of the SDSS data release 5

We have investigated the correlations among color, morphology and luminosity for all LRGs, cut I LRGs, cut II LRGs, and Main galaxies that are also classified as LRGs. It is found that the morphology of LRGs is tightly correlated with luminosity. The rest-frame u-g color of cut I LRGs and cut II LRGs is nearly independent of luminosity, but the color of Main galaxies is correlated with luminosity. For cut I LRGs and Main galaxies, the early type proportion apparently changes with color: at the rest-frame u-g < 1.3 it increases strongly with increasing color, while at the rest-frame u-g > 1.3 it decreases with increasing color. We also notice that the morphology of cut II LRGs is only a weak function of color. Published in Astrofizika, Vol. 50, No. 3, pp. 335–345 (August 2007).     

Monte‐Carlo simulation of a possible correlation between the estimated luminosity distances and internal extinctions of type Ia supernovae

This paper describes a Monte Carlo simulation of type Ia supernova data. It was shown earlier that the data of SNe Ia might contain a possible correlation between the estimated luminosity distances and internal extinctions. This correlation was shown by different statistical investigations of the data. In order to remove observational biases (for example the effect of the detection limit of the observing instrument) and to test the reality of the effect found earlier we developed a simple routine which simulates extinction values, redshifts and absolute magnitudes for Ia supernovae. We pointed out that the correlation found earlier in the real data between the internal extinction and luminosity distance does not occur in the simulated sample. Furthermore, it became obvious that the detection limit of the observing devices used in supernova projects does not affect the far end of the redshift‐luminosity distance relationship of Ia supernovae. This result strengthens the earlier conclusions of the authors that SN Ia supernovae alone do not support the existence of dark energy. (© 2007 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

A New Feature Vector Using Selected Line Spectra for Pulsar Signal Bispectrum Characteristic Analysis and Recognition

Average pulse profiles of pulsar signals are analyzed using the bispectrum tech-nique. The result shows that there are nonlinear phase couplings between the two frequency axes of the bispectrum charts, which indicate nonlinear factors in the generation and prop-agation of pulsar signals. Bispectra can be used as feature vectors of pulsar signals because of their being translation invariant. A one-dimension selected line spectrum algorithm for ex-tracting pulsar signal characteristic is proposed. Compared with selected bispectra, the pro-posed selected line spectra have the maximum interclass separability measurements from the point of view of the whole one-dimension feature vector. Recognition experiments on several pulsar signals received at several frequency bands are carried out. The result shows that the selected line spectrum algorithm is suitable for extracting pulsar signal characteristics and has a good classification performance.     

松科二井早白垩世早期玄武安山岩的发现及地质意义

松科二井超深钻探获取了松辽盆地连续沉积-火山岩心,为系统研究中生代松辽盆地形成机制、揭示中国东北地区构造演化历史提供了极好的研究材料。本文对取自松科二井井深-6035~-6084m的玄武安山岩开展了系统的锆石U-Pb定年、全岩主微量元素和Sr-Nd同位素分析测试。研究结果表明,松科二井玄武安山岩隶属于火石岭组底部,其形成时代为早白垩世早期（141.6±1.4Ma）。玄武安山岩样品富集大离子亲石元素,亏损高场强元素,具有弧岩浆的地球化学特征。这些样品显示了一定程度的轻重稀土元素分异（（La/Yb）_N=8.40~11.88）,具有轻微亏损的Sr-Nd同位素特征（（⁸⁷Sr/⁸⁶Sr）_i=0.70496~0.70478,ε_Nd（t）=1.05~1.61）,表明它们很可能源自于岩石圈地幔。早白垩世时期中国东北地区主要受控于蒙古-鄂霍茨克洋的南向俯冲和东侧古太平洋俯冲过程,目前研究揭示了前者影响了同期的大兴安岭地区的火山活动,但其影响范围是否延伸至松辽盆地内部尚不清楚。古太平洋岩石圈开始俯冲后很可能诱发了松辽盆地西侧晚中生代火山岩的形成。早白垩世松辽盆地演化主要受蒙古-鄂霍茨克洋还是古太平洋板块的活动影响仍存在较多争议。松科二井玄武安山岩具有与板内玄武岩相近的Th/Hf比值（1.10~2.87）及Zr/Y比值（10.1~18.7）,表明它们具有板内岩浆的地球化学特征,且松科二井样品比同时代盆地西部的大兴安岭地区玄武岩具有更高的Nb/Ta比值,更高的Zr、Hf与Ti含量,以及更亏损的Nd同位素特征,可能指示与大兴安岭地区玄武岩形成于不同的构造背景。松辽盆地内早白垩世火山岩很可能为古太平洋板片回转诱发形成,指示早白垩世古太平洋板片回转诱发的岩石圈伸展促进了松辽盆地的形成。