风暴尺度天气下利用集合卡尔曼滤波模拟多普勒雷达资料同化试验I.不考虑模式误差的情形

本文在假定模式无偏差的情况下, 利用一次风暴过程的模拟多普勒雷达资料进行一系列风暴天气尺度的集合卡尔曼滤波资料同化试验, 检验集合卡尔曼滤波在风暴天气尺度资料同化方面的效果, 并验证各集合卡尔曼滤波参数对同化效果的影响。试验结果表明, 集合卡尔曼滤波能有效地应用于风暴尺度的资料同化; 40个集合成员以及6 km的局地化尺度能较好地滤除采样误差造成的虚假相关, 同时可以将观测信息传递到无观测的模式格点; 利用背景场加上空间平滑的高斯型随机扰动生成初始成员的方式较未经过平滑的方式有更好的分析效果; 背景场扰动方法能够提高样本的离散度; 只同化反射率的同化试验表明, 反射率的同化效果较明显, 也证明了集合卡尔曼滤波在非常规资料同化中的作用; 增加径向风资料同化的效果优于只进行反射率同化的结果。     

雨雪冰冻天气多普勒雷达产品特征

2008年1月下旬至2月上旬福建省西部北部出现了历史罕见的雨雪冰冻灾害。利用多普勒雷达反射率、回波顶高、径向速度、垂直风廓线等产品对此次雨雪冰冻天气进行特征分析,通过分析发现:①冰晶和雪的回波强度通常比连续性降水回波弱,在反射率图上,回波表现为边缘毛松,丝缕状纹理结构明显,边缘模糊不清,没有确定的边界;②回波顶高和零度层较低,因为垂直方向大气相对较稳定,不利于对流发展,降水粒子没有发展到高空;③在径向速度图上存在牛眼,说明在低空有急流存在。在低层有环形的零速度线,中高层的零速度线为倒"S"形,表明低层有风切变存在,中高层有冷平流;④风廓线图上高层为西南风,中层为西北风,低层为西南风,近地层为东北风。说明从近地层到高层为"冷-暖-冷-暖"的层结结构,有利于冻雨天气形成。     

天津地区雷暴大风天气雷达产品特征分析

应用2002-2007年天津共46次雷暴大风天气过程的新一代天气雷达资料,并结合灾情报告和地面自动气象站资料,根据雷达基本反射率回波特征,影响渤海西部雷暴大风的雷达回波形态有以下四种类型:弓状回波、阵风锋、带状回波和零散椭圆状回波,其中弓状回波对应的雷暴大风天气最为强烈,特别是弓状回波的前部和顶端突起部分;同时弓状回波主体维持时间与雷暴大风维持时间基本一致.另外,应用垂直积分液态水含量产品(VIL)进行了统计分析.结果表明:当VIL值达到或超过40 kg·m~(-2)时,随后VIL值的快速减小对于预警雷暴大风天气有指示意义,这种信息一般能够提前10分钟出现.此外,分析了雷暴大风的路径来源有四类:分别是北方路径有9次,西北路径占19次,西方路径14次和其他路径4次,其中北方路径带来的灾害相对严重.这些特征对预警渤海西部雷暴大风天气提供使用价值,同时也可提供其他地区参考使用.     

低纬高原罕见“雷打雪”中尺度特征分析

应用常规高空资料、FY-2C卫星红外和水汽图像、加密自动站地面观测资料,结合新一代多普勒雷达探测资料,综合分析了2008年2月28日夜间至29日凌晨发生在云南的"雷打雪"罕见天气现象.结果表明:南支槽和冷空气、西南低空急流的共同影响,是其发生的有利天气背景,其中强对流天气就发生在急流与锋面相互作用的湿度锋湿区内斜压不稳定的环境中.中-γ尺度对流云团生成并逐渐增强为中-β尺度对流云团是形成此次复杂对流天气的直接中尺度系统.多普勒雷达回波中,PPI上有回波强度达25～33dBz的"人字形"回波、钩状回波以及阵风锋的出现,相应VPPI上出现逆风区、低层零线"S"形暖平流及"牛眼"结构是"雷打雪"天气中降雨转为冰雹、阵雪过程中,中尺度对流系统由弱变强的典型特征.地面逐时温、压、湿、风的迅速演变特征表现为雷暴发生前增温增湿和增压,温度、气压出现峰值,且气压曲线显示为圆顶状的中尺度雷暴高压特征;风的变化则表现为风向呈逆时针旋转,偏北风增大并出现风速峰值.雷暴过境时,要素显示为降温增湿,出现露点锋.     

基于5分钟雷达资料降水估测模型的比较

For the Z-R relationship in radar-based rainfall estimation, the distribution of corresponding R values for a given Z value （or the corresponding Z value for a given R value） may be highly skewed. However, the traditional power-law model is physically deduced and fitted under the normal-distribution presumption of radar wave echoes associated with a rain rate value, and it may not be very appropriate. Considering this problem, the authors devised several generalized linear models with different forms and distribution presumptions to represent the Z-R relationship. Radar-reflectivity scans observed by a CINRAD/SC Doppler radar and 5-minute rainfall accumulation recorded by 10 ground gauges were used to fit these models. All data used in this study were collected during some large rainfalls of the period from 2005 to 2007. The radar and all gauges were installed in the catchment of the Yishu River, a branch of the Huaihe River in China. Three models based on normal distribution and a dBZ presumption of gamma distribution were fitted using maximum-likelihood techniques, which were resolved by genetic algorithms. Comparisons of estimated maximized likelihoods based on assumptions of gamma and normal distribution showed that all generalized linear models （GLMs） of presumed gamma distribution were better fitted than GLMs based on normal distribution. In a comparison of maximum-likelihood, the differences between these three models were small. Three error statistics were used to assess the agreement between radar estimated rainfall and gauge rainfall： relative bias （B）, root mean square error （RMSE）, and correlation coefficient （r）. The results showed that no one model was excellent in all criteria. On the whole, the GLM-based models gave smaller relative bias than the traditional power-law model. It is suggested that validations conducted in many previous works should have been made against a specific criterion but overlooked others.     

北京地区一次罕见的雷暴大风过程特征分析

分析了2006年6月24日北京地区一次罕见的瞬时极大风速超过32 m.s-1的雷暴大风事件。多普勒天气雷达观测表明,此次强雷暴大风与镶嵌在飑线回波带中的弓形回波相关。后侧入流急流促使飑线回波带南段快速移动并与其前面的新生单体合并加强形成弓形回波。深厚的中气旋、低层径向速度辐合和高层辐散等在构成弓形回波的强对流单体形成过程中起了重要的作用。根据雷达回波特征演变推断,这次雷暴大风直接由构成弓形回波的一个强对流单体内的下击暴流导致。使用微波辐射计和风廓线仪的观测资料揭示了上述强风暴发生的环境条件,即高的对流有效位能值、中等强度的风垂直切变,以及风切变的分布特征为飑线等的产生提供了有利条件。下沉对流有效位能和对流层低层环境大气温度直减率明显增加并接近干绝热,这对即将到来的下击暴流具有指示意义。     

NLTE models of line-driven stellar winds – III. Influence of X-ray radiation on wind structure of O stars

We study the influence of X-rays on the wind structure of selected O stars. For this purpose we use our non-local thermodynamic equilibrium (NLTE) wind code with inclusion of additional artificial source of X-rays, assumed to originate in the wind shocks.
We show that the influence of shock X-ray emission on wind mass-loss rate is relatively small. Wind terminal velocity may be slightly influenced by the presence of strong X-ray sources, especially for stars cooler than   T _eff≲ 35 000 K  .
We discuss the origin of the   L _X/ L ∼ 10⁻⁷  relation. For stars with thick wind this relation can be explained assuming that the cooling time depends on wind density. Stars with optically thin winds exhibiting the 'weak wind problem' display enhanced X-ray emission which may be connected with large shock cooling length. We propose that this effect can explain the 'weak wind problem'.
Inclusion of X-rays leads to a better agreement of the model ionization structure with observations. However, we do not find any significant influence of X-rays on P  v ionization fraction implying that the presence of X-rays cannot explain the P  v problem.
We study the implications of modified ionization equilibrium due to shock emission on the line transfer in the X-ray region. We conclude that the X-ray line profiles of helium-like ions may be affected by the line absorption within the cool wind.     

On the X-ray emission from massive star clusters and their evolving superbubbles – II. Detailed analytics and observational effects

In this work, we present a comprehensive X-ray picture of the interaction between a super star cluster and the interstellar medium. In order to do that, we compare and combine the X-ray emission from the superwind driven by the cluster with the emission from the wind-blown bubble. Detailed analytical models for the hydrodynamics and X-ray luminosity of fast polytropic superwinds are presented. The superwind X-ray luminosity models are an extension of the results obtained in Paper I. Here, the superwind polytropic character allows us to parametrize a wide variety of effects, for instance, radiative cooling. Additionally, X-ray properties that are valid for all bubble models taking thermal evaporation into account are derived. The final X-ray picture is obtained by calculating analytically the expected surface brightness and weighted temperature of each component. All of our X-ray models have an explicit dependence on metallicity and admit general emissivities as functions of the hydrodynamical variables. We consider a realistic X-ray emissivity that separates the contributions from hydrogen and metals. The paper ends with a comparison of the models with observational data.     

Constraining jet/disc geometry and radiative processes in stellar black holes XTE J1118+480 and GX 339−4

We present results from modelling of quasi-simultaneous broad-band (radio through X-ray) observations of the Galactic stellar black hole (BH) transient X-ray binary (XRB) systems XTE J1118+480 and GX 339−4 using an irradiated disc + compact jet model. In addition to quantifying the physical properties of the jet, we have developed a new irradiated disc model which also constrains the geometry and temperature of the outer accretion disc by assuming a disc heated by viscous energy release and X-ray irradiation from the inner regions. For the source XTE J1118+480, which has better spectral coverage of the two in optical and near-infrared (OIR) wavelengths, we show that the entire broad-band continuum can be well described by an outflow-dominated model + an irradiated disc. The best-fitting radius of the outer edge of the disc is consistent with the Roche lobe geometry of the system, and the temperature of the outer edge of the accretion disc is similar to those found for other XRBs. Irradiation of the disc by the jet is found to be negligible for this source. For GX 339−4, the entire continuum is well described by the jet-dominated model only, with no disc component required. For the two XRBs, which have very different physical and orbital parameters and were in different accretion states during the observations, the sizes of the jet base are similar and both seem to prefer a high fraction of non-thermal electrons in the acceleration/shock region and a magnetically dominated plasma in the jet. These results, along with recent similar results from modelling other galactic XRBs and AGNs, may suggest an inherent unity in diversity in the geometric and radiative properties of compact jets from accreting black holes.