2007-2019年太湖藻型和草型湖区叶绿素a变化特征及影响因子

基于太湖31个站点的逐月监测数据,分析了2007-2019年太湖藻型湖区和草型湖区的叶绿素a变化特征,并分析研究不同环境因子对不同类型湖区叶绿素a的影响.结果表明,近年来太湖不同类型湖区的总磷浓度和叶绿素a浓度变化基本一致,均呈波动上升趋势.不同类型湖区的总磷浓度拐点均为2015年,叶绿素a浓度拐点均为2016年.最低月平均水温、前冬积温、年平均水温、年均风速与藻型湖区和草型湖区叶绿素a浓度均呈显著相关.沉水植物分布面积与草型湖区叶绿素a浓度之间呈显著相关.湖西区年内和年度降雨剧烈变化,湖西区年降雨量与不同类型湖区当年叶绿素a浓度的关系不明显,5日极端降雨量与不同类型湖区下年度叶绿素a浓度均呈显著正相关.太湖蓝藻水华强度在短期内可能仍会处于较高水平,迫切需要高度重视高温时段太湖蓝藻打捞处置工作,保障饮用水安全;同时,要进一步加强湖西区强降雨期间的非点源污染防控措施研究,推动入湖污染通量稳步降低,并探索东西山之间及东茭咀附近水域沉水植物生态修复技术,降低风浪扰动作用,尽快恢复相关重要水域的沉水植物.     

京津冀一次飑线过程的精细时空演变特征分析

利用常规探空资料、多普勒天气雷达资料和风廓线雷达资料对2013年3月19日夜里到20日凌晨发生在湖南中南部和广东北部的一次区域性雷暴大风天气进行了分析,发现本次强对流天气过程的天气尺度背景是北支高压脊的崩溃和南支槽的建立,槽前出现较强的低空急流和切变线并在湖南中南部和广东北部形成了上干冷下暖湿的温湿配置结构下发生并强烈发展的;地面自动站观测显示北风侵入到前期露点温度较高的贵州黄平地区并形成风向辐合触发了对流,之后对流单体东移进入前期地面辐合线和露点锋相配合,同时500 hPa极为干冷的湖南中部偏南地区不断发展加强成对流带;雷达观测显示19日夜里在湖南西部不断出现对流单体并在其东移南下过程中最终形成飑线结构,该飑线中存在多个超级单体;通过多普勒天气雷达的中气旋产品与雷暴大风出现时间对应比较发现：大多数由中气旋引发的雷暴大风,在雷暴大风出现前2~3个体扫,其中气旋底高不断下降至2 km左右或以下,且在雷暴大风出现前1~2个体扫,中气旋的最强切变高度显著下降至中气旋底高位置附近;通过风廓线雷达数据与雷暴大风出现时间对应比较发现：底层大气折射率结构常数(C2n)大幅度的跃升通常在雷暴大风出现前10~15 min左右出现,其对雷暴大风的出现可能具有一定的指示意义。基于雷达资料快速更新四维变分同化（RR4DVar）分析系统,利用京津冀6部新一代多普勒天气雷达资料和区域（约700个）自动站资料对2013年7月30—31日京津冀地区一次飑线系统在移动过程中系统不同部位的热动力结构及其环境场时空演变特征进行了分析。结果表明,这次飑线过程是在有利的天气尺度背景形势下发生发展的。飑线形成初期,其中段和南段前部有强的暖湿空气辐合上升运动,并受到强的中层垂直风切变的影响,且在飑线中南段两侧水平正负涡度近似平衡,这种环境下,十分有利于飑线中南段的组织发展。而北段前部受弱的中层垂直风切变及辐散下沉运动影响,不利于北段系统有组织的发展;随着飑线移动下山,中段和南段前部在较强的中层垂直风切变控制下,出现强的暖湿空气辐合上升运动,且存在偏南暖湿气流稳定输送到系统上升运动区中,这对飑线系统中段和南段自身对流单体新生及高度组织化极为有利。随着飑线演变为弓形回波,中段环境场仍维持强的中层垂直风切变且位于冷池出流边界的控制之下,由于地形强迫效应,有利于弓形回波前沿低空偏南暖湿气流的辐合上升,是飑线下山迅速增强并发展成弓形回波,且稳定维持的主要原因。     

青藏高原东北侧7月少雨流型的研究

根据青藏高原东北侧9个代表站1951—2000年历年7月的降水量资料,确定了5个多、少雨年。再用NCEP／NCAR再分析格点资料,分别求出850,700,600,500,200,100,70,50和30hPa共计9个层次上多、少雨年份7月月平均合成位势高度场。计算了500hPa合成高度场与其余各个层次合成高度场流型的相似性度量以及各个层次的东亚北风指数。结果表明：20世纪80年代提出的1300hPa层次上高原东北侧“西正东负”少雨流型的特征在850～70hPa整层大气中仍然存在。同时．7月少雨流型与平流层低层70,50hPa前期环流特征之间也存在联系,这些结果可供西北干旱形成研究和干旱预测业务参考。     

The Venusian induced magnetosphere: A case study of plasma and magnetic field measurements on the Venus Express mission

Plasma and magnetic field measurements made onboard the Venus Express on June 1, 2006, are analyzed and compared with predictions of a global model. It is shown that in the orbit studied, the plasma and magnetic field observations obtained near the North Pole under solar minimum conditions were qualitatively and, in many cases also, quantitatively in agreement with the general picture obtained using a global numerical quasi-neutral hybrid model of the solar wind interaction (HYB-Venus). In instances where the orbit of Venus Express crossed a boundary referred to as the magnetic pileup boundary (MPB), field line tracing supports the suggestion that the MPB separates the region that is magnetically connected to the fluctuating magnetosheath field from a region that is magnetically connected to the induced magnetotail lobes.     

The magnetic field near Mars: A comparison between a hybrid model, Mars Global Surveyor and Mars Express observations

Mars Express (MEX) does not carry its own magnetometer which complicates interpretation of ASPERA-3/MEX ion measurements. The direction of the interplanetary magnetic field (IMF) is especially important because it, among other things, determines the direction of the convective electric field and orientation of the cross tail current sheet and tail lobes. In this paper we present a case study to show the properties of the magnetic field near Mars in a quasi-neutral hybrid (QNH) model at the orbits where the Mars Global Surveyor (MGS) has made measurements, present a method to derive the IMF clock angle by comparing fields in a hybrid model and the direction of the magnetic field measured by MGS by deriving the IMF clock angle. We also use H⁺ ring velocity distribution observations upstream of the bow shock measured by the IMA/ASPERA-3 instrument on board MEX spacecraft. These observations are used to indirectly provide the orientation of the IMF. We use a QNH model (HYB-Mars) where ions are modeled as particles while electrons form a mass-less charge neutralizing fluid. We found that the direct MGS and non-direct IMA observations of the orientation magnetic field vectors in non-crustal magnetic field regions are consistent with the global magnetic field draping pattern predicted by the global model.     

Variations of the magnetic field near Mars caused by magnetic crustal anomalies

The possible avenues for photoelectron transport were determined during southern hemisphere winter at Mars by using a mapping analysis of the theoretical magnetic field. Magnetic field line tracing was performed by superposing two magnetic field models: (1) magnetic field derived from a three-dimensional (3D) self-consistent quasi-neutral hybrid model which does not contain the Martian crustal magnetic anomalies and (2) a 3D map of the magnetic field associated with the magnetic anomalies based on Mars Global Surveyor magnetic field measurements. It was found that magnetic field lines connected to the nightside of the planet are mainly channeled within the optical shadow of the magnetotail whereas magnetic field lines connected to the dayside of the planet are observed to form the remainder of the magnetosphere. The simulation suggests that the crustal anomalies create “a magnetic shield” by decreasing the region near Mars which is magnetically connected to the Martian magnetosphere. The rotation of Mars causes periodic changes in magnetic connectivity, but not to qualitative changes in the overall magnetic field draping around Mars.     

WASP-3b: a strongly irradiated transiting gas-giant planet

We report the discovery of WASP-3b, the third transiting exoplanet to be discovered by the WASP and SOPHIE collaboration. WASP-3b transits its host star USNO-B1.0 1256−0285133 every  1.846 834 ± 0.000 002  d. Our high-precision radial velocity measurements present a variation with amplitude characteristic of a planetary-mass companion and in phase with the light curve. Adaptive optics imaging shows no evidence for nearby stellar companions, and line-bisector analysis excludes faint, unresolved binarity and stellar activity as the cause of the radial velocity variations. We make a preliminary spectroscopic analysis of the host star and find it to have   T _eff= 6400 ± 100 K  and  log   g = 4.25 ± 0.05  which suggests it is most likely an unevolved main-sequence star of spectral type F7-8V. Our simultaneous modelling of the transit photometry and reflex motion of the host leads us to derive a mass of  1.76^+0.08_−0.14 M _J  and radius  1.31^+0.07_−0.14 R _J  for WASP-3b. The proximity and relative temperature of the host star suggests that WASP-3b is one of the hottest exoplanets known, and thus has the potential to place stringent constraints on exoplanet atmospheric models.     

Dependence of the Characteristics of Solar Wind Discontinuities and Shocks with Heliolatitude and Radial Distance

The distribution of the shocks in the heliosphere and their characteristic variations are investigated using Ulysses observations. The jumps in solar wind velocity, IMF magnitude, and proton density across the shocks and discontinuities are evaluated and used to characterize them. The distribution of these discontinuities with respect to heliolatitude ± 80° and with radial distance 1 to 5 AU are analyzed during solar minimum and solar maximum to understand their global behavior. It is noticed that the jumps in solar wind parameters associated with shocks and discontinuities are more prominent during the second orbit of Ulysses, which coincided with the maximum phase of solar activity.     

Radar Backscatter from Underdense Meteors and Diffusion Rates

Many meteoroids burn up between about 120 km and 70 km, deposit metals and dust and form ionized trails which are detected by radars. Model studies about the influence of neutral or positively charged background dust on the ambipolar diffusion indicate that significant smaller decay times should be observed for weak meteor echoes compared to strong meteor echoes which can affect the estimation of temperatures. The variation of meteor decay times in dependence on echo strength, height, and season was studied using radar observations at 69° N, 22° S, and 67° S. Significantly reduced decay times were found for weak echoes below about 88 km at low latitudes throughout the year, and at high latitudes with the exception of summer. In summer at high latitudes, decreasing decay times of weak and strong meteors are observed at altitudes below about 85 km during the appearance of noctilucent clouds. The impact of reduced decay times on the estimation of neutral temperatures from decay times is discussed.     

全新世时期北京-张家口地区与黄土高原地区风成系统的差异

近年来,中国北方的沙尘暴对北京地区的影响越来越受到人们的重视,从地质记录上分析研究北京—张家口地区沙尘暴的粉尘来源对确定重点治理区、改善北京地区的大气环境质量具有积极意义。黄土是地质时期沙尘暴形成的风成沉积物,其粒径分布蕴含了粉尘搬运过程中的大气环境信息,本文利用黄土-古土壤沉积的粒径分布特征,分析了北京—张家口地区和黄土高原地区风成系统的差异,并根据粉尘动力学原理,结合遥感信息揭示的地面风蚀痕迹,探讨了北京—张家口地区黄土粉尘的主要来源,指出北京—张家口地区和黄土高原地区分属不同的风成系统,有不同的粉尘源区和不同的大气动力条件。北京—张家口地区大气动力强度大,粉尘源区近,粉尘主要来自阴山以北的内蒙古苏尼特右旗—二连浩特方向,与浑善达克沙地关系不大,也与黄土高原地区主要粉尘物源区不同