The motion of a test particle in the Kaluza-Klein-type of gravitational theory with variable rest mass

The geodesic equation in a viable 5D space-time-mass theory of gravity is calculated for the purpose of presenting quantities accessible to experiments and observations. Determining the values of the constants in the theory is left for future tests concerning the principle of equivalence. But qualitatively we can show that the five-velocity is a function of not only of time but also mass. And in general case a possible change of mass depends onm as well ast.     

5D space-time-mass gravity theory with off-diagonal components in the metric tensor

The bi-variational technique is used to calculated Chandrasekhar'sX- andY-functions and their first two moments for an isotropic homogeneous finite slab. Numerical results obtained are compared with published results.     

Hα Emission Stars in the Cepheus OB3 Region

H emission objects were searched for, using the objective-prismSchmidt plates in a 36 deg² sky area covering the Cepheus OB3 association.Hundred and eight emission stars have been found, 68 of which are newfindings to our knowledge. The properties of the IRAS point sourcesidentified with H emission stars indicate that most of theH emission stars are T Tauri stars or related objects. Hemission stars associated with IRAS sources and those unassociated havedifferent distributions, suggesting an age sequence among them.Altogether, they show a ring- or shell-like surface distribution, whichalmost coincides with that of heated dusts, and these distributionsappear to be encompassed by an HI shell.     

马站盆地成因与晚白垩世郯庐断裂带的活动性

通过对郯庐断裂带内马站盆地中沉积岩相和同沉积构造分布特征的详细研究及盆地内凝灰岩夹层中的锆石裂变径迹年龄测定和盆内化石的研究,认为该盆地是一个形成于晚白垩世并与郯庐断裂带活动有关的走滑盆地。该盆地的形成表明郯庐断裂带,至少是其一部分,在晚白垩世时期仍存在明显的走滑活动。      

用非线性近似方法反演单多普勒雷达风场(英)

回顾了近年来由单多普勒雷达观测反演风场的各种方法。这些方法大部分基于线性假设,因此风场的非线性变化经常影响反演结果,使得反演的风场误差增大。我们提出一种以非线性近似理论为基础的反演方法,该方法主要考虑了风场分片光滑的特点并充分利用了雷达的径向风场数据。我们把该方法应用到1998年淮河能量与水循环实验的两个个例中。通过同双多普勒雷达观测的结果比较,发现该方法能反演较高分辨率和准确性的水平风场,反演的垂直风场也比较合理。     

Coupled process-based cyclone surge simulation for the Bay of Bengal

We have developed a wind-wave-surge coupled process-based numerical model for simulating storm surge, consisting of a meso-scale atmospheric model (MM5), a third-generation spectral wave model (WW3) and a coastal ocean model (POM). We introduced an additional sea surface shear stress by wave dissipation into the model to consider the process of energy transfer from winds to currents through whitecap breaking. We demonstrate the importance of this energy transfer path through a hindcast simulation of a cyclone surge in April, 1991 in the Bay of Bengal: it helps generate mean current and has wave effects on wind-induced current fields in extremely shallow water areas.     

应用Terra/MODIS卫星数据估算洞庭湖蓄水量的变化

以洞庭湖为例,利用2002年的美国Terra/MODIS卫星数据,以16天为周期将全年划分为23个时段,分别对湖区水位和蓄水量分布特征和变化规律进行动态监测和综合分析。具体测算方法包括以下4个步骤: (1) 根据湖区特性,将整个洞庭湖分为3个部分：自西向东依此是西洞庭湖 (WDL), 南洞庭湖 (SDL) 和东洞庭湖 (EDL)。这3个部分的蓄水量之和就是整个洞庭湖的总蓄水量。(2) 以水体和陆地的光谱差异为基础,使用Terra/MODIS卫星的NDVI 数据识别并量测湖区水面积。(3) 将湖区水面影像同湖区数字高程模型DEM相叠加,以被监测的湖区水面的平均高度值作为水面高度。水面高度与湖底高度的差即为相应点的水深。(4) 按50 m×50 m网格大小和相应位置的水深的乘积来计算每个水柱体积。最后,将整个湖内的所有水柱的体积值累加便得到洞庭湖的总蓄水量。用上述方法测算的水位和蓄水量与实测资料进行了比较表明,两者具有很好的一致性。     

The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

The Space Infrared telescope for Cosmology and Astrophysics (SPICA) is planned to be the next space astronomy mission observing in the infrared. The mission is planned to be launched in 2017 and will feature a 3.5 m telescope cooled to <5 K through the use of mechanical coolers. These coolers will also cool the focal plane instruments thus avoiding the use of consumables and giving the mission a long lifetime. SPICA’s large, cold aperture will provide a two order of magnitude sensitivity advantage over current far infrared facilities (>30 microns wavelength). We describe the scientific advances that will be made possible by this large increase in sensitivity and give details of the mission, spacecraft and focal plane conceptual design.

Evolution of a precipitating cloud and cloud droplets

The evolution of a precipitating convective cloud was studied by a time-dependent numerical model in which for the simplification of dynamical framework the domain under consideration was expressed by three regions: inner region of cloud, outer region of cloud and environmental region. Clouds are assumed to have no ice-phase. The size distribution of water drops is described using five size-groups. Two types of cloud droplets (case A and case B) were given at cloud base. There are more small cloud droplets in case B than in case A. The slower production of raindrops in case B results in the later formation of a downdraft and rainfall than in case A. In consequence rainfall efficiency is lower in case B. These differences of both cases had a tendency to be larger in a less unstable atmosphere.     

Magnetic pulsation Pi2 and substorm onset

Coincidence between the onset of sudden brightening of the auroral arc in the auroral oval and the onset of Pi2 magnetic pulsation in low latitudes is examined based on the auroral data obtained at a chain of stations in Alaska and the Pi2 data obtained at the low-latitude station Onagawa. The result shows that the low-latitude Pi2 occurs almost simultaneously with the sudden brightening of the auroral arc, i.e. the onset of an auroral substorm (T = 0). It is concluded that the onset of substorms can be identified quite well with the onset of the low-latitude Pi2.