Spectroscopic binaries near the North Galactic Pole paper 15: HD 106947

Photoelectric radial-velocity measurements show that HD 106947 is a double-lined spectroscopic binary. The components have spectral types of about F6 V and G5 V and are in a 59-day orbit of moderate eccentricity. The system is a member of the Coma Cluster.     

Spectroscopic binaries near the North Galactic Pole paper 6: BD 33° 2206

Photoelectric radial-velocity measurements have confirmed O. C. Wilson’s finding that BD 33° 2206, the secondary star in the wide visual binary ADS 8470, is a spectroscopic binary. It has an eccentric orbit with a period of 100 days. Its γ-velocity is close to the constant radial velocity of the visual primary, confirming the physical association of the stars.     

The Boumerdes (Algeria) earthquake of May 21, 2003 (<Emphasis Type="Italic">M</Emphasis><Subscript>w</Subscript> = 6.8): Ground deformation and intensity

A destructive earthquake of magnitude M_w = 6.8 hit the region of Boumerdes and Algiers (Algeria) on May 21, 2003. This is among the strongest seismic events of the mediterranean region and the most important event in the capital Algiers since 1716. It caused a widespread damage in the epicentral region, claimed 2271 human lives, injured 10000, about 20000 housing units affected and left about 160000 homeless. The main shock was felt about 250 km far from the epicenter and triggered sea waves of 1–3 m in amplitude in Balearic islands (Spain). Based on field observations and press report an intensity IX (MSK scale) is attributed to the epicentral area. The main shock was followed by many aftershocks among them several are of magnitude greater than 5.0, which added panic to inhabitants. The main shock triggered ground deformation, particularly liquefaction whose features are in different forms and sizes and caused damage and collapse of roads. The focal mechanism determined by worldwide institutions yield a pure reverse faulting with a compressional axis striking NE-SW. The epicenter is located offshore about 7 km from the Boumerdes-Dellys coast. Field observations show 0.7 m of coseismic uplift of shoreline between Boudouaou and Dellys. This uplift is about a half of the extracted coseismic slip from the seismic moment. On the other hand there is no clear surface break onshore, confirming hence, that the causative active fault is offshore. However, the rupture may propagate onshore to the SE near the Boudouaou region where ground cracks showing reverse faulting are observed a long a corridor of about 1 km wide. These fissures may correspond to a diffuse coseismic deformation.     

华北回流天气多普勒雷达径向速度分布特征

使用多普勒雷达资料对四次华北回流天气过程进行了分析,结果表明:(1)回波具有较大水平范围的、连绵成片的均匀幕状特征.回波顶较平整,回流降雨过程中还存在零度层亮带.属层状云降水回波.(2)速度图上,在零速度线两侧常分布范围较大数值不等的正负径向速度中心,低空零速度线呈"S"型,风随高度顺时针旋转,有暖平流存在.在强降水时段出现前常伴有区域性的冷平流层.(3)风廓线图上,从低层到高层由东北风转为西南风,风向发生了近180度的顺时针旋转,存在强垂直切变.降水开始与结束时分别表现为低层偏东风与中高层西南气流叠加、低层偏东风与中高层西南气流任何一者消失.边界层顶部出现浅薄的冷平流层是降水强度加强的信号.     

多普勒雷达资料在中尺度模式短时预报中的应用

将国内新一代多普勒雷达基数据Lev-Ⅱ的9个仰角的原始反射率和径向风资料应用于中尺度模式ARPS(the Advanced Regional Prediction System),通过对2007年7月18日济南短时特大暴雨过程的个例研究,分析了雷达资料对初始场的改进效果及其对模拟结果的影响。结果表明,同时利用雷达反射率和径向风资料改进过的初始场能明显改善中尺度数值模式短时定量降水预报。对比风场发现,雷达径向风调整后在初始场中出现明显的中小尺度特征,能减少模式的spin-up时间。随着积分的进行,对水汽场的调节也有一定作用,但相对于风场调节不够显著。雷达反射率主要是改进初始场中的湿度参数,增加初始场中云水等含量。积分开始后,对风场调整也很显著。此次模拟,控制试验较好地预报出雷达回波的分布和水汽中心,对应的降水落区与实况也较为接近,但对雷达回波中心强度的预报略大,相应地降水量的预报也偏大。     

High resolution spectroscopy of two young active late type stars within 20 parsecs of the Sun

We present high-resolution optical echell spectroscopy of HIP 544 and HIP 46843, two nearby solar like stars. The discovery of these young stars at such a close distance to the Sun is really a surprising phenomenon. It will help us to have a better understanding of the structure and evolutionary history of the Milky Way. The radial ve-locities (RV) of HIP 544 and HIP 46843 are measured to be -6.88±0.13km s-1 and 8.30±0.16km s-1, respectively, which are more accurate than before. The equivalent widths (EW) of the Li I 6707.8 A absorption line of HIP 544 and HIP 46843 are mea-sured to be 110±5mA and 195±5mA respectively. Based on these properties, HIP 544 is estimated to be 100-800Myr old and HIP 46843 30-100Myr old using three relatively creditable methods.     

A planetary companion orbiting the intermediate-mass G Giant HD 173416

The discovery of a planetary companion to the intermediate-mass late-type giant star HD173416 from precise Doppler surveys of G and K giants at Xingiong station and Okayama Astrophysical Observatory (OAO) is presented in this letter. The planet has a minimum mass of 2.7 MJ an eccentricity of 0.21, a semimajor axis of 1.16 AU and an orbital period of 324 days.     

Analysis of the three-dimensional stellar velocity field using vector spherical functions

We apply vector spherical functions to problems of stellar kinematics. Using these functions allows all of the systematic components in the stellar velocity field to be revealed without being attached to a specific physical model. Comparison of the theoretical decomposition coefficients of the equations for a particular kinematical model with observational data can provide precise information about whether the model is compatible with the observations and can reveal systematic components that are not described by this model. The formalism of vector spherical functions is particularly well suited for analyzing the present and future (e.g., GAIA) catalogs containing all three velocity vector components: the propermotions in both coordinates and the radial velocity. We show that there are systematic components in the proper motions of Hipparcos stars that cannot be interpreted in terms of the linear Ogorodnikov-Milne model. The same result is also confirmed by an analysis of the radial velocities for these stars.     

WASP-3b: a strongly irradiated transiting gas-giant planet

We report the discovery of WASP-3b, the third transiting exoplanet to be discovered by the WASP and SOPHIE collaboration. WASP-3b transits its host star USNO-B1.0 1256−0285133 every  1.846 834 ± 0.000 002  d. Our high-precision radial velocity measurements present a variation with amplitude characteristic of a planetary-mass companion and in phase with the light curve. Adaptive optics imaging shows no evidence for nearby stellar companions, and line-bisector analysis excludes faint, unresolved binarity and stellar activity as the cause of the radial velocity variations. We make a preliminary spectroscopic analysis of the host star and find it to have   T _eff= 6400 ± 100 K  and  log   g = 4.25 ± 0.05  which suggests it is most likely an unevolved main-sequence star of spectral type F7-8V. Our simultaneous modelling of the transit photometry and reflex motion of the host leads us to derive a mass of  1.76^+0.08_−0.14 M _J  and radius  1.31^+0.07_−0.14 R _J  for WASP-3b. The proximity and relative temperature of the host star suggests that WASP-3b is one of the hottest exoplanets known, and thus has the potential to place stringent constraints on exoplanet atmospheric models.