2007年12月南京六次雨雾过程宏、微观结构演变特征

利用2007年冬季南京信息工程大学对雾的综合观测资料,包括能见度仪、雨滴谱仪、雾滴谱仪、宽范围颗粒粒径谱仪(WPS)观测资料,并结合地面常规气象观测资料和NCEP(National Centers for Environmental Prediction)再分析资料,分析2007年12月南京六次雨雾过程的宏、微观结构演变特征。结果显示:(1)南京2007年12月的六次雨雾过程主要是受天气系统的影响,以雨中雾为主,最低能见度均大于250 m。雨雾多出现在偏东气流的作用下,南京地区先发生弱降水,空气近饱和,随后受到来自北方的弱冷空气影响,水汽凝结,雾形成。(2)雨雾发生前贴地层多有逆温,雨雾过程中2 m高度与地表温度差由正转为负,逆温消失。但900 hPa以下,雨雾发生前和过程中,都少有逆温层,雨雾结束后均无逆温结构。雨雾前中低层有云,云状为高积云Ac或高层云As及层积云Sc或碎雨云Fn,低云高0.3～2.5 km,雨雾过程中,600 hPa以下都是饱和层,多伴有Fn,低云高度明显下降,雨雾过后,近饱和层仍然有可能存在。雨雾前900 hPa附近有明显的风切变。(3)雨雾形成初期,大粒子(粒子直径D≥10 μm)和小粒子(1 μm相似文献   

Symplectic adaptive algorithm for solving nonlinear two-point boundary value problems in Astrodynamics

In this paper, from a Hamiltonian point of view, the nonlinear optimal control problems are transformed into nonlinear two-point boundary value problems, and a symplectic adaptive algorithm based on the dual variational principle is proposed for solving the nonlinear two-point boundary value problem. The state and the costate variables within a time interval are approximated by using the Lagrange polynomial and the costate variables at two ends of the time interval are taken as independent variables. Then, based on the dual variational principle, the nonlinear two-point boundary value problems are replaced by a system of nonlinear equations which can preserve the symplectic structure of the nonlinear optimal control problem. Furthermore, the computational efficiency of the proposed symplectic algorithm is improved by using the adaptive multi-level iteration idea. The performance of the proposed algorithm is tested by the problems of Astrodynamics, such as the optimal orbital rendezvous problem and the optimal orbit transfer between halo orbits.     

Strange star candidates revised within a quark model with chiral mass scaling

We calculate the properties of static strange stars using a quark model with chiral mass scaling.The results are characterized by a large maximum mass (～ 1.6 M) and radius (～10 km).Together with a broad collection of modern neutron star models,we discuss some recent astrophysical observational data that could shed new light on the possible presence of strange quark matter in compact stars.We conclude that none of the present astrophysical observations can prove or confute the existence of strange stars.     

The Landau level-superfluid modified factor and the overal soft X/<Emphasis Type="Italic">γ</Emphasis>-ray efficiency coefficient of a magnetar

As soon as the energies of electrons near the Fermi surface exceed Q, the threshold energy of inverse β-decay, electron capture (EC) dominates inside a neutron star. The high-energy neutrons released by EC will destroy anisotropic ³ P ₂ neutron Cooper pairs in the degenerate superfluid. By colliding with the neutrons produced in the process n+(n↑n↓)→n+n+n, the kinetic energies of the neutrons released by EC will be transformed into thermal energy. A portion of this thermal energy will be transported from the star interior to the star surface by conduction, then converted to a thermal spectrum of soft X-rays and γ-rays. By introducing two important parameters: the Landau level-superfluid modified factor and the overal soft X/γ-ray efficiency coefficient, we compute the theoretical luminosity L _X of a magnetar under our model and plot a diagram of L _X as a function of magnetic field strength B. Numerical calculations based on our model agree well with the observed properties of magnetar candidates.     

低高度角大气静力学延迟修正的改进

进行低高度角观测是GPS(Global Positioning System)气象学的发展趋势,其中发展高精度的低高度角的大气静力学延迟修正是主要的关键技术.比较了3种计算无线电波从空间到地面接收机的大气静力学延迟修正方法:(1)在大气球对称假设下用探空气球资料路径积分得到大气静力学延迟;(2)在大气球对称假设下用NCEP(National Centers for Environmental Prediction)再分析资料得到大气静力学延迟;(3)用Niell的大气静力学映射函数得到大气静力学延迟.与2001年中国地区89个探空气球站资料计算得到的大气静力学映射函数比较结果显示:NCEP再分析资料路径积分的方法在低高度角(5°以下)的精度好于Niell映射函数模型约5倍.     

The evolution of the z distribution of normal neutron stars in the Galaxy

Under the two initial 1‐D one parameter velocity distribution forms (one is normal, the other is exponential), the z direction scale height evolution of normal neutron stars in the Galaxy is studied by numerical simulation. We do statistics for the cases at different time segments, also do statistics for the cumulative cases made of each time segment. The results show in the cumulative cases the evolution curves of the scale heights are smoother than in the each time segment, i.e., the cumulation improve the signal‐to‐noise ratio. Certainly the evolution cases are different at different Galactic disk locations, which also have very large difference from the average cases in the whole disk. In the initial stages of z evolution of normal neutron stars, after the beginning transient states, the cumulative scale heights increase linearly with time, and the cumulative scale height increasing rates have linear relationship with the initial velocity distribution parameters, which have larger fluctuation in the vicinity of the Sun than in the whole disk. We utilize the linear relationship of the cumulative scale height increasing rates vs. the initial velocity distribution parameters in the vicinity of the Sun to make comparison with the observation near the Sun. The results show if there is no magnetic decay, then the deserved initial velocity parameters are obvious lower than the present well known results from some authors; whereas if introducing magnetic decay, for the 1‐D normal case we can make consistence among concerning results using magnetic decay time values which are supported by some authors, while for the 1‐D exponential case the results show the lackness of young pulsar samples in the larger z in the vicinity of the Sun (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Dependence of the holmberg effect on separations between paired galaxies

To investigate the dependence of the Holmberg effect of paired galaxies on three-dimensional separations, we have constructed four subsamples characterized by three-dimensional separations s ≤ 50 kpc, 50 kpc < s ≤ 100 kpc , 100kpc < s ≤150kpc , and 150 kpc < s ≤ 200 kpc , respectively. In this study, linear correlation coefficients and surplus standard deviations of color indices, luminosity, and size between two components of paired galaxies are calculated. It is found that there is a weak tendency for correlation coefficients of color indices to increase with decreasing three-dimensional separations, but such a tendency does not exist for ones of luminosity and size. We also note that there is no tendency for surplus standard deviations to decrease with decreasing three-dimensional separations. This suggests that it is still very difficult to clearly affirm the dependence of the Holmberg Effect of paired galaxies on three-dimensional separations.     

Zn2+对日本沼虾(Macrobrachium nipponensis)的急性致毒效应

在水温(27.4±1.3)℃条件下,以体长(33.23±1.66)mm、体质量(0.7893±0.1518)g的日本沼虾为实验动物,采用静水停食法开展了Zn2+对日本沼虾的急性毒性实验,并以此为基础,测定了Zn2+不同质量浓度水平下日本沼虾的耗氧率与窒息点.结果表明:(1)Zn2+对日本沼虾的急性致死效应与其呼吸生理代谢受阻密切相关;(2) Zn2+对日本沼虾24h、48h、72h、96h的半致死质量浓度依次为1.493、0.844、0.643和0.464mg/L; (3) Zn2+对日本沼虾昼均、夜均和日均耗氧率均无显著影响的阈值为0.046mg/L,该值为Zn2+对日本沼虾急性毒性的安全质量浓度;(4) Zn2+对日本沼虾产生轻度胁迫和中度胁迫的质量浓度范围分别为0.046-0.064mg/L和0.064-0.082mg/L.     

拟穴青蟹(Scylla paramamosain)蛋白二硫键异构酶基因的分子克隆与表达分析

蛋白二硫键异构酶(PDI)是内质网中的关键酶, 参与蛋白合成过程中二硫键的形成、还原和异构。本文首次从拟穴青蟹(Scylla paramamosain)克隆获得了PDI基因cDNA全长, 该序列长度为2015bp, 开放阅读框为1452bp, 编码483个氨基酸。荧光定量PCR检测发现PDI存在于拟穴青蟹的多个组织中; 在拟穴青蟹卵巢发育过程中, PDI基因的表达量在前4个时期逐渐上升, 到了第5期(成熟期)表达量则下降, 表明PDI参与了卵巢发育的蛋白合成过程。免疫组化表明, 拟穴青蟹卵母细胞存在PDI阳性反应, 进一步为该分子参与卵巢发育提供了形态学证据。     

青海天峻新关角隧道涌排水水源识别与量化分析

涌排水严重影响隧道施工与运行安全,查明隧道涌排水的来源,是隧道防水止水重要科学依据.青海天峻新关角隧道南北洞口处的地下水排水量分别为10021,60877 m3/d,两者存在近50000 m3/d的差异,涌排水量大,且来源不明.基于水文地质条件分析,分别采集了新关角隧道隧址区内大气降水、不同类型地下水和隧道出口涌排水水...