农田近地表风沙流风程效应变化特征研究

风沙流的风程效应研究是定量获取风沙流沿程变化的核心和难点,风程效应是指输沙率随沙床表面或地块长度的增加而不断增大,而后趋于稳定的变化特征,饱和输沙率（f_max）和饱和路径长度（L_sat）是风程效应的重要参数。采用自动连续称重式集沙仪,以河北坝上地区康保县境内典型旱作农田为研究对象,观测了2017、2018年和2021年内4次典型风蚀事件,分析近地表5 cm高度风沙流的风程效应在5 min时间尺度下的变化特征。结果表明：（1） 近地表输沙通量随风程距离的增大而增大。（2） 4次风蚀事件中L_sat的变化范围在11~280 m之间,并存在明显差异,其变化与风速无关。（3） 近地表风沙流的f_max与风速（U）呈幂函数关系。（4） 风程效应的变化特征与地表可蚀性因子、地表微地貌变化有着紧密联系,未来应对不同的土壤类型和质地农田的风程效应进行深入研究。     

沙丘形态及表沙粒度特征对风况和地表植被变化的响应

以毛乌素沙地3种沙丘（新月形沙丘、抛物线形沙丘和反向沙丘）为研究对象,对其形态、表沙粒度特征和区域风况进行了量化分析,探讨了沙丘表沙物理运动过程及其形态对外界条件（风况和地表植被）变化的反馈,揭示了沙丘表沙粒度特征对不同沙丘形态的响应机制。结果表明：新月形沙丘表沙平均粒径由迎风坡底部向顶部逐渐变小,分选呈现逐渐变好趋势, 但粒径较小和分选较差的表沙样出现在沙丘迎风坡中部。随着地表植被覆盖度的增加,新月形沙丘逐渐向抛物线形沙丘转变,近地表输沙能力和沙丘上风向沙源的供应同样受到限制,致使抛物线形沙丘由迎风坡底部向顶部呈现表沙平均粒径变大,而分选逐渐变好的趋势。毛乌素沙地内季节性风况（春季盛行强劲西北风,夏季盛行较弱东南风）的变化不仅促进了反向沙丘的发育,并且重组了西北盛行风影响下的表沙粒度特征。在夏季反向风风蚀的作用下,沙丘落沙坡顶部出现反向堆积和脊线反向移动的现象,同时其顶部呈现平均粒径由小变大、分选逐渐变好的趋势。     

一次华北气旋造成北京特大暴雪天气过程分析

利用北京延庆站和海淀站风廓线产品、微波辐射计产品、北京市雷达产品(南郊和车道沟)、北京市58个称重雨量站观测资料、FY-2E卫星云图、常规气象资料综合分析2012年11月3到4日北京暴雪天气过程。分析表明：降水相态(雨、雪)由华北气旋的锋面性质和锋面位置决定;过程雨雪量由气旋的强度、持续时间和水汽通道维持时间决定;风廓线和微波辐射计产品资料在雨雪开始时间、雨雪相态转换方面有明显的指示性作用。     

Measurement of the radial density gradient of cosmic ray in the heliosphere by the GRAPES-3 experiment

A radial anisotropy in the flux of cosmic rays in heliosphere was theoretically predicted by Parker and others within the framework of the diffusion–convection mechanism. The solar wind is responsible for sweeping out the galactic cosmic rays, creating a radial density gradient within the heliosphere. This gradient coupled with the interplanetary magnetic field induces a flow of charged particles perpendicular to the ecliptic plane which was measured and correctly explained by Swinson, and is hereafter referred as ‘Swinson flow’. The large area GRAPES-3 tracking muon telescope offers a powerful probe to measure the Swinson flow and the underlying radial density gradient of the galactic cosmic rays at a relatively high rigidity of ∼100 GV. The GRAPES-3 data collected over a period of six years (2000–2005) were analyzed and the amplitude of the Swinson flow was estimated to be (0.0644 ± 0.0008)% of cosmic ray flux which was an ∼80σ effect. The phase of the maximum flow was at a sidereal time of (17.70 ± 0.05) h which was 18 min earlier than the expected value of 18 h. This small 18 min phase difference had a significance of ∼6σ indicating the inherent precision of the GRAPES-3 measurement. The radial density gradient of the galactic cosmic rays at a median rigidity of 77 GV was found to be 0.65% AU⁻¹.     

青藏高原500hpa暖性高压生成的热成风适应机制

本文利用热成风适应原理,采取分解分析法对青藏高原500hpa暖性高压的生成机制作了一些定性和定量的讨论。结果表明:在扰动的水平尺度大于热成风适应的特征尺度的条件下,当源地有明显的负值非热成风涡度出现时,流场将向温度场适应,而温度场由于高原的加热作用存在暖中心或暖脊,则适应的结果在高原大气500hpa形成暖性高压,并伴随高层辐合,低层辐散及下沉运动。     

Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign

We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ∼295 ks between 30th June and 24th July 2005, and continuously for ∼64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329-1347] was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in X-ray flux due to the Deep Impact event was small, ∼20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×¹⁰⁶ kg (∼10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, much stronger than the man-made increase due to Deep Impact, were found in the observed X-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma, with intermittent impulsive events due to solar flares and coronal mass ejections.     

Analysis of plasma and field conditions during some intensely geo-effective transient solar/interplanetary disturbances of solar cycle 23

The problem of solar wind-magnetosphere coupling is investigated for intense geomagnetic storms (Dst < -100nT) that occurred during solar cycle 23. For this purpose interplanetary plasma and field data during some intensely geo-effective transient solar/interplanetary disturbances have been analysed. A geomagnetic index that represents the intensity of planetary magnetic activity at subauroral latitude and the other that measures the ring current magnetic field, together with solar plasma and field parameters (V, B, Bz, σB, N, and T) and their various derivatives (BV,-BVz, BV², -BzV², B²V, Bz²V, NV²) have been analysed in an attempt to study mechanism and the cause of geo-effectiveness of interplanetary manifestations of transient solar events. Several functions of solar wind plasma and field parameters are tested for their ability to predict the magnitude of geomagnetic storm.     

Analysis on monthly-averaged distribution of sea surface wind and wave over the seas southeast of Asia using ERS-2 scatterometer data

The wind system over the seas southeast of Asia (SSEA) plays an important role in China's climate variation. In this paper, ERS scatterometer winds covering the period from January 2000 to December 2000 and the area of 2-41 °N, 105- 130°E were analyzed with a distance-weighting interpolation method and the monthly mean distribution of the sea surface wind speed were given. The seasonal characteristics of winds in the SSEA were analyzed. Based on WAVEWATCH Ⅲ model, distribution of significant wave height was calculated.     

A Statistical Analysis on the E ect of Vertical Wind Shear on Tropical Cyclone Development

Using tropical cyclone (TC) best track and intensity of the western North Pacific data from the Joint TyphoonWarning Center (JTWC) of the United States and the NCEP/NCAR reanalysis data for the period of 1992-2002, the effects of vertical wind shear on TC intensity are examined. The samples were limited to the westward or northwestward moving TCs between 5°N and 20°N in order to minimize thermodynamic effects. It is found that the effect of vertical wind shear between 200 and 500 hPa on TC intensity change is larger than that of the shear between 500 and 850 hPa, while similar to that of the shear between 200 and 850 hPa. Vertical wind shear may have a threshold value, which tends to decrease as TC intensifies. As the intensifying rate of TC weakens, the average shear increases. The large shear has the obvious trend of inhibiting TC development. The average shear of TC which can develop into typhoon (tropical depression or tropical storm) is below 7 m s-1 (above 8 m s-1).     

Influence of coronal mass ejection on geomagnetic activity during 1988–1993

The most rapid and dramatic evolution in the solar corona occurs in events now known as Coronal Mass Ejections (CMEs). There have considerable importance for our understanding of the evolution of the mass and energy injected into the interplanetary medium. In this work, we have studied the relation of CMEs with geomagnetic activity for the period of 1988 to 1993. Not all CMEs are capable of producing geomagnetic disturbances. Our study indicates that the maximum chance of a geomagnetic disturbance occurs two to three days after a CME in association with B-type solar flares.