Multi-scale Analysis of a Hailstorm and Short-time Heavy Rainfall Process in Hohhot City

Based on the conventional observation data,satellite,radar,automatic observation and other refined monitoring data,the severe hail weather in Hohhot City on July 29,2015 was analyzed at multiple scales.The results showed that from the perspective of synoptic-scale system,high-altitude cold air invaded Mongol shortwave trough,and the North China small high pressure and the subtropical high formed a warm shear line;the surface convergence line triggered severe convection weather.Unstable vertical structure,continuous increase of low-level humidity,more drier of high altitudes and the wind direction shear at 180° triggered hailstorm and lightning weather in Hohhot.α-scale convective cloud clusters were maintained in Hohhot,and the ground "herringbone" shear line oscillated violently between the north and the south.Strong lightning and big hails appeared on the ground.The "herringbone" shear line lifted slowly to the north,and there was short-time heavy precipitation on the ground.Radar products showed "bow echo",and the echo had a hanging structure;a mesoscale cyclone was formed 3 km away from the ground.On the radar wind profile,it can be seen that low-layer warm advection and strong wind shear triggered strong hailstorm in Hohhot.The disappearance of low- level warm advection and the maintenance of strong vertical shear of wind produced short-time heavy precipitation.There was a small difference between short-time heavy precipitation and hail in echo top height,but the coverage was significantly reduced.In Hohhot City,vertically integrated liquid water content quickly increased during the hail,and decreased during the short-time heavy precipitation.

CO Clouds around SNR G21.8-0.6 and G32.8-0.1

We made the first CO（1-0） mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720MHz maser. Based on the morphological correspondence and velocity and position agreement between the radio remnant and the CO clouds, we tentatively identify the clouds that are respectively interacting with the two SNRs.

THE 2－D NUMERICAL STUDY ON THE PRINCIPLES OF RAIN－ENHANCEMENT AND HAIL－SUPPRESSIONIN CONVECTIVE CLOUDS

ＴＨＥ２－ＤＮＵＭＥＲＩＣＡＬＳＴＵＤＹＯＮＴＨＥＰＲＩＮＣＩＰＬＥＳＯＦＲＡＩＮ－ＥＮＨＡＮＣＥＭＥＮＴＡＮＤＨＡＩＬ－ＳＵＰＰＲＥＳＳＩＯＮＩＮＣＯＮＶＥＣＴＩＶＥＣＬＯＵＤＳＭａｏＹｕｈｕａ（毛玉华）ａｎｄＨｕＺｈｉｊｉｎ（胡志晋）ＴＨＥ２－Ｄ...

Non-similar collapse of singular isothermal spherical molecular cloud cores with nonzero initial velocities

Theoretically, stars formed from the collapse of cores in molecular clouds. Historically, the core had been assumed to be a singular isothermal sphere （SIS）, and the collapse had been investigated in a self-similar manner. When the rotation and magnetic fields lead to non-symmetric collapse, a spheroidal shape may occur. Here, the result of the centrifugal force and magnetic field gradient is assumed to be in the normal direction to the rotational axis, and its components are supposed to be a fraction β of the local gravitational force. In this research, a collapsing SIS core is considered to find the importance that the parameter β plays in the oblateness of the mass shells, which are the crests of the expansion waves. We apply the Adomian decomposition method to solve the system of nonlinear partial differential equations because the collapse does not occur in a spherically symmetric and self-similar man- ner. In this way, we obtain a semi-analytical relation for the mass infall rate M of the shells in the envelope. Near the rotational axis, M˙ decreases with the increase of the non-dimensional radius ξ, while a direct relation is observed between M˙ and ξ in the equatorial regions. Also, the values of M˙ in the polar regions are greater than their equatorial values, and this difference occurs more often at smaller values of ξ. Overall, the results show that before reaching the crest of the expansion wave, the visible shape of the molecular cloud cores can evolve into oblate spheroids. The ratio of major to minor axes of oblate cores increases when increasing the parameter β, and its value can approach the observed elongated shapes of cores in the maps of molecular clouds, such as those in Taurus and Perseus.

基于神经网络 B-P 算法的雹云识别模型及其效果检验

本文根据成都、内江和泸州等地的雷达回波和部分探空资料，应用神经网络Ｂ－Ｐ算法建立了不同地区的３参数和４参数雹云识别模型，并对模型进行了分析和效果检验。结果表明：该模型不仅能得到较高的拟合率和预报准确率，而且由于Ｂ－Ｐ网络具有自组织、自学习和自适应的能力，与其它方法相比具有一定的优越性。

冰雹云探测技术研究进展--基于巴彦淖尔人工防雹技术研究试验

“西北人工影响天气能力建设项目巴彦淖尔人工防雹技术研究试验”于2018—2021年在内蒙古巴彦淖尔地区开展,本试验在该地区已有探测设备基础上增加X波段双偏振雷达、二维雨滴谱仪、测雹板等特种观测设备,以科学合理的设备布局及观测方式为基础开展外场研究试验,研究建立适宜于内蒙古自治区巴彦淖尔人工防雹作业特点的技术体系。利用C波段多普勒雷达、地面降雹资料研究分析了巴彦淖尔地区降雹时空分布特征、冰雹云移动路径,得出巴彦淖尔地区降雹天气主要发生在每年6—8月、12—20时的河套地区,主要冰雹云移动路径是自西北向东南(46.7%),其次是自西南向东北(26.2%);研究分析了2019年测雹板观测地面降雹特征,根据测雹板反演出的冰雹粒子最大直径为19.9 mm,最小为3 mm,总体能较好反映降雹区域的降雹实况,降雹粒子数分布近似于指数分布,拟合的指数分布系数为N_(0)=6349、θ=0.4153,且在粒子直径为5 mm时存在“左截断”现象(3~5 mm直径区间粒子数少),误差产生的主要原因有凹坑重叠、人工数据读取等因素。

Diagnosis of An Infrequent Regional Hail Weather Course in Gansu

Based on routine weather charts, numerical predication products and satellite cloud images, the causes of an infrequent regional hail weather process occurred in east of Gansu on Aug. 2, 2006 were diagnosed and analyzed. The results showed that the hail weather process occurred at the abnormal large-scale circulation leading the system to west. When the cold trough, which was separated by the north cold vortex, moved southward through Hetao and then intersected with 300 hPa jet stream and the surface cold front, that led to the strong convection. There were strong upward motion and unstable stratification in hail area, three MCS in satellite cloud, and a character of formed arch shape echo on radar echo charts.

Satellite Retrieval of a Strong Hailstorm Process

A case of hailstorm process occurring on 24 June 2006 in northwestern China was studied using satellite retrieval methodology. The particle effective radius (re) in the cloud tops was calculated by the reflectance in the 3.7 μm channel, and cloud-top microphysical properties were vividly represented using the RGB visual multispectral classification scheme. The microphysical zones of clouds and the processes of hail formation and develop-ment are inferred using the relations of cloud-top temperature (T) versus re for the tops of convective clouds. The results show that particle effective radius was smaller near the cloud base of hailstorm. There was a deep zone of diffusional droplet growth at the low level where the particles grew slowly with height, and there existed an evident area of small ice particles in the cloud top, suggesting the existence of a strong updraft in the clouds. The low glaciated temperature indicated a great depth from the cloud base to the glaciation height, which provided a deep layer of supercooled water for hail growth.

A New Thioamide Derivative for Separation and Preconcentration of Multi Elements in Aquatic Environment by Cloud Point Extraction

2-(pyridine-2-yl)-N-p-chlorohydrazinecarbothioamide (HCPTS) was synthesized, characterized and successfully applied for the preconcentration of Cu(II), Ni(II), Zn(II), Cd(II), Co(II), Pb(II), Fe(II), and Hg(II) in water, blood, and urine samples prior to graphite furnace atomic absorption determination (GFAAS);Hg was determined by cold vapor technique. Under the optimum experimental conditions (i.e. pH = 8, 10–4 M of HCPTS, 0.05% w/v of Triton X-114), calibration graphs were linear in the range of 0.02 to 200 ng?mL–1 for Co(II), Cd(II), Pb(II) and Ni(II);0.03 to 200 ng?mL–1 for Cu(II);0.07 to 200 ng?mL–1 for Fe(II) and Zn(II) and 0.02 to 150 ng?mL–1 for Hg(II). The enrichment factors were 43, 51, 41, 46, 54, 40, 45 and 52 for Cu(II), Ni(II),Zn (II), Cd(II), Co(II), Pb(II), Fe(II), and Hg(II), respectively. The limit of detection were found to be 0.019, 0.094, 0.0514, 0.052, 0.0165, 0.047, 0.068 and 0.041 ng?mL–1 for Cu(II), Ni(II), Zn(II), Cd(II), Co(II), Pb(II), Fe(II), and Hg(II), respectively. The developed method was applied to the determination of these metal ions in water, blood and urine samples with satisfactory results.

First Mapping Observations of Two Possible Cloud Collision Candidates IRAS 02459+6029 and 05363+3127

The first mapping observations of the cold infrared sources IRAS 02459＋6029 and 05363＋3127 in the molecular lines ^12CO（1-0））, ^13CO（1-0） and C^18O（1-0） were made using the 13.7 m millimeter wave telescope in Qinghai. Both the integrated intensity maps and position-velocity diagrams show that each has two components adjacent in both space and velocity which means possible cloud-cloud collisions in the two regions. The near-infrared color-color diagram from the 2MASS database reveals that the density of YSOs in the colliding site is much higher than in the surrounding regions. The results appear to indicate that star forming activities have taken place in the two regions due to the cloud-cloud collision. We conclude that both sources are cloud collision candidates.

Determination of the magnetic fields of Magellanic X-ray pulsars

The 80 high-mass X-ray binary （HMXB） pulsars that are known to reside in the Magellanic Clouds （MCs） have been observed by the XMM-Newton and Chandra X-ray telescopes on a regular basis for 15 years, and the XMM-Newton and Chandra archives contain nearly complete information about the duty cycles of the sources with spin periods Ps 〈 100 s. We have reprocessed the archival data from both observatories and we combined the output products with all the published observations of 31 MC pulsars with Ps 〈 100 s in an attempt to investigate the faintest X-ray emission states of these objects that occur when accretion to the polar caps proceeds at the smallest possible rates. These states determine the so-called propeller lines of the accreting pulsars and yield information about the magnitudes of their surface magnetic fields. We have found that the faintest states of the pulsars segregate into five discrete groups which obey to a high degree of accuracy the theoretical relation between spin period and X-ray luminosity. So the entire population of these pulsars can be described by just five propeller lines and the five corresponding magnetic moments （0.29, 0.53, 1.2, 2.9 and 7.3, in units of 1030 G cma）.

Study of the filamentary infrared dark cloud G192.76+00.10 in the S254–S258 OB complex

We present results of a high resolution study of the filamentary infrared dark cloud G192.76＋00.10 in the S254-S258 OB complex in several molecular species tracing different physical conditions. These include three isotopologues of carbon monoxide （CO）, ammonia （NH3） and carbon monosulfide （CS）. The aim of this work is to study the general structure and kinematics of the filamen- tary cloud, and its fragmentation and physical parameters. The gas temperature is derived from the NH3 （J, K） = （1, 1）, （2, 2） and 12CO（2-1） lines, and the 13CO（1-0）, 13CO（2-1） emission is used to inves- tigate the overall gas distribution and kinematics. Several dense clumps are identified from the CS（2-1） data. Values of the gas temperature lie in the range 10 - 35 K, and column density N（H2） reaches the value 5.1 ×1022 cm-2. The width of the filament is of order 1 pc. The masses of the dense clumps range from ×30 M⊙ to - 160 M⊙. They appear to be gravitationally unstable. The molecular emission shows a gas dynamical coherence along the filament, The velocity pattern may indicate longitudinal collapse.

A search for evidence of small-scale inhomogeneities in dense cores from line profile analysis

In order to search for intensity fluctuations on the HCN（1-0） and HCO＋（1-0） line pro- files, which could arise due to possible small-scale inhomogeneous structure, long-term observations of high-mass star-forming cores S140 and S199 were carried out. The data were processed by the Fourier filtering method. Line temperature fluctuations that exceed the noise level were detected. Assuming the cores consist of a large number of randomly moving small thermal fragments, the total number of frag- ments is - 4 × 106 for the region with linear size - 0.1 pc in S140 and - 106 for the region with linear size - 0.3 pc in S 199. Physical parameters of fragments in S 140 were obtained from detailed modeling of the HCN emission in the framework of the clumpy cloud model.

Experimental study on detonation parameters and cellular structures of fuel cloud

In this paper, detonation parameters of fuel cloud, such as propylene oxide （PO）, isopropyl nitrate （IPN）, hex- ane, 90# oil and decane were measured in a self-designed and constructed vertical shock tube. Results show that the deto- nation pressure and velocity of PO increase to a peak value and then decrease smoothly with increasing equivalence ra- tio. Several nitrate sensitizers were added into PO to make fuel mixtures, and test results indicated that the additives can efficiently enhance detonation velocity and pressure of fuel cloud and one type of additive n-propyl nitrate （NPN） played the best in the improvement. The critical initiation energy that directly initiated detonation of all the test liquid fuel clouds showed a U-shape curve relationship with equiva- lence ratios. The optimum concentration lies on the rich-fuel side （;b 〉 1）. The critical initiation energy is closely related to molecular structure and volatility of fuels. IPN and PO have similar critical values while that of alkanes are larger. Detonation cell sizes of PO were respectively investigated at 25;C, 35;C and 50;C with smoked foil technique. The cell width shows a U-shape curve relationship with equivalence ratios at all temperatures. The minimal cell width also lies on the rich-fuel side （;b 〉 1）. The cell width of PO vapor is slightly larger than that of PO cloud. Therefore, the deto- nation reaction of PO at normal temperature is controlled by gas phase reaction.

The Long-term Survival Chances of Young Massive Star Clusters

We review the long-term survival chances of young massive star clusters （YMCs）, hallmarks of intense starburst episodes often associated with Violent galaxy interactions. We address the key question as to whether at least some of these YMCs can be considered protoglobular clusters （GCs）, in which case these would be expected to evolve into counterparts of the ubiquitous old GCs believed to be among the oldest galactic building blocks. In the absence of significant external perturbations, the key factor determining a cluster＇s long-term survival chances is the shape of its stellar initial mass function （IMF）. It is, however, not straightforward to assess the IMF shape in unresolved extragalactic YMCs. We discuss in detail the promise of using high-resolution spectroscopy to make progress towards this goal, as well as the numerous pitfalls associated with this approach. We also discuss the latest progress in worldwide efforts to better understand the evolution of entire cluster systems, the disruption processes they are affected by, and whether we can use recently gained insights to determine the nature of at least some of the YMCs observed in extragalactic starbursts as proto-GCs. We conclude that there is an increasing body of evidence that GC formation appears to be continuing until today; their long-term evolution crucially depends on their environmental conditions, however.

A New Interpretation of the Bipolar HII Region S106 from HCN J = 3 - 2 Mapping Observations

The first mapping observations of the bipolar HII region S106 in HCN J = 3 - 2 line were made by KOSMA submillimeter telescope in April, 2004. The results show that there is a bipolar outflow centered on the high-mass star S106 IRS4 and that the flat structure of molecular cloud core is perpendicular to the axis of the outflow. This image roughly corresponds to the optical image where a dark lane bisects the bipolar HII region. Together with the optical, infrared and radio data, we conclude that the central UC HII region and molecular outflow formed before the two lobes of the bipolar HII region, and that a neutral disk is responsible for the bipolar HII region and the outflow.

一次冰雹云发展的雷达回波特征分析及其防雹作业效果物理检验

利用云南昭通CC雷达和威宁探空等资料,对贵州省威宁县2017年7月23日的一次冰雹云发展过程的雷达基本反射率因子和径向速度的变化特征进行分析,同时通过插值得到剖面变化特征,研究雹云垂直结构演变,并根据雷达回波顶高、强回波中心(45 dBZ)高度、组合反射率和垂直累积液态水含量(VIL)这4个雷达探测特征物理量,进行时间序列分析,得到防雹作业效果。结果表明:(1)降雹前对流单体的合并使回波强度和VIL分别跃增至60 dBZ和50 kg·m^(-2)以上,冰雹云的雷达回波出现旁瓣回波和“V”形缺口。(2)中低层气流的径向辐合及高层强辐散带来的强烈抽吸作用所产生的上升气流,使雹云能够稳定维持和发展。(3)防雹作业后,雹云开始由上至下分裂直至完全分裂成两个孤立弱单体,回波顶高明显降低,组合反射率较峰值下降近30 dBZ。(4)在作业单元和对比单元的生命史时间内,作业单元的4个雷达探测特征物理量下降速率均大于对比单元的,表明防雹作业有效抑制了雹云的发展。通过对比分析发现,防雹作业24 min后,4个雷达探测特征物理量的双比值均小于1,进一步证明防雹作业取得了明显的正效果,加速了对流单体的消亡。

Molecular Gas Distribution around the Supernova Remnant G40.5-0.5

The distribution of dense molecular gas around the supernova rem- nant G40.5-0.5 has been investigated by radio spectroscopic observations in the CO （J=1 - 0） transition. The molecular gas is found to extend over the entire region of G40.5-0.5. A molecular shell, with a diameter of ～ 26′, coincides with the ionized gas as revealed by the cm-radio observations. This coincidence, along with the velocity discontinuity following the shell, provides direct evidence for interaction between the ionized gas and the dense molecular gas. No clear evidence for cosmic-ray accelera- tion can be identified from this SNR as previously suggested, due to positional uncertainty in relating the SNR shell defined by CO to the EGRET gamma-ray sources, GRO J1904＋06, from the gamma-ray observations.

A multiwavelength study of the star forming HⅡ region Sh2-82

Based on a multiwavelength study, the interstellar medium and young stel- lar objects （YSOs） around the H II region Sh2-82 have been analyzed. Two molecular clumps were found from the archival data of the Galactic Ring Survey, and using the Two Micron All-Sky Survey catalog, we found two corresponding young clusters embedded in the molecular clumps. The very good relations between CO emission, infrared shells and YSOs suggest that it is probably a triggered star formation region from the expansion of Sh2-82. We further used the data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire from Spitzer to study the YSOs within the two clumps, confirming star formation in this region. By spectral energy distribution fits to each YSO candidate with infrared excess, we derived the slope of the initial mass function. Finally, comparing the H II region＇s dynamical age and the fragmenta- tion time of the molecular shell, we discard the ＂collect and collapse＂ process as being the triggering mechanism for YSO formation. Sh2-82 can be a mixture of other pro- cesses such as radiative-driven implosion and/or collisions with pre-existing clumps.